baker

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Author name code: baker
ADS astronomy entries on 2022-09-14
=author:"Baker, D." OR =author:"Baker, Deborah" -title:"Mars" -title:VizieR"

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Title: Stellar FIP effect from the empirical side
Authors: Seli, Bálint; Van Driel-Gesztelyi, Lidia; Baker, Deborah;
Laming, J. Martin; Kovari, Zsolt; Oláh, Katalin; Kriskovics, Levente;
Vida, Krisztián; Balázs, Lajos
2022cosp...44.2585S Altcode:
The difference between the elemental abundances of the corona and the
photosphere is an apparently common feature of stellar atmospheres. The
abundance difference depends on the first ionization potential of the
given element, so the phenomenon is known as the FIP effect. Here we
explore the variation of the strength of the FIP effect for different
types of stars, through the FIP bias parameter. Using a sample of 59
main sequence and evolved stars with known coronal abundances from the
literature, we look for macroscopic, measurable parameters that affect
the stellar FIP bias, and also re-evaluate the simple dependence on
the effective temperature.

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Title: Investigating of the nature of magnetic oscillations associated
with FIP effect
Authors: Murabito, Mariarita; Jafarzadeh, Shahin; Van Driel-Gesztelyi,
Lidia; Ermolli, Ilaria; Baker, Deborah; Brooks, David; Long, David;
Jess, David; Valori, Gherardo; Stangalini, Marco
2022cosp...44.2591M Altcode:
Observations of the photosphere, chromosphere, and corona combined with
magnetic field modeling of one of the biggest sunspots of the 24 solar
cycle, revealed that regions of high FIP bias plasma in the corona
were magnetically linked to the locations of the intrinsic magnetic
oscillations in the solar chromosphere. In order to characterize
the driver of the oscillations, we analyzed the relation between
the spatial distribution of the magnetic wave power and the overall
field geometry and plasma parameters obtained from the multi-height
spectropolarimetric non-local thermodynamic equilibrium (NLTE)
inversions. In correspondence with the locations where the magnetic
wave energy is observed at chromospheric heights, we found evidence
in support of locally excited acoustic waves that, after crossing the
equipartition layer located close to the umbra-penumbra boundary at
photospheric heights, are converted into magnetic-like waves. These
results indicate a direct connection between sunspot chromospheric
activity and observable changes in coronal plasma composition,
demonstrating the power of high resolution, multi-height studies of the
solar atmosphere that will become the gold standard in the era of DKIST.

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Title: Understanding the Correlation between Solar Coronal Abundances
and F10.7 Radio Emission
Authors: To, Andy S. H.; Baker, Deborah; Long, David; James, Alexander;
Brooks, David; van Driel-Gesztelyi, Lidia; Valori, Gherardo; Bastian,
Tim; Lomuscio, Samantha; Stansby, David
2022cosp...44.2592T Altcode:
Solar corona plasma composition, derived from full-Sun spectra, and
the F10.7 radio flux (2.8 GHz) have been shown to be highly correlated
(r = 0.88) during the recent weak solar cycle. However, this correlation
becomes nonlinear at times of increased solar magnetic activity. We used
co-temporal, high spatial resolution, radio (JVLA), and EUV (Hinode/EIS)
images of the Sun taken on the 3 and 7 April 2020 to understand the
underlying causes of the non-linearity of the FIP bias-F10.7 solar
index correlation. We then calculated differential emission measures
from AIA images, and paired them with the observed FIP bias to predict
the bremsstrahlung component of F10.7 radio emission. Results of this
study provide constraints on the amplitude of composition variability
related to solar cycle amplitude, and provide an alternative method
to calculate coronal composition.

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Title: What determines active region coronal plasma composition?
Authors: Mihailescu, Teodora; Baker, Deborah; Long, David; Green,
Lucie; Brooks, David; van Driel-Gesztelyi, Lidia; To, Andy S. H.
2022cosp...44.2580M Altcode:
The chemical composition of the solar corona is different from that
of the solar photosphere, with the strongest variation being observed
in active regions. Using spectral data from the Extreme Ultraviolet
(EUV) Imaging Spectrometer (EIS) on Hinode, we present a survey of
coronal elemental composition as expressed in the FIP bias in 28 active
regions with a wide range of ages and magnetic flux contents, and at
different stages in their evolution. We find no correlation between the
FIP bias of an active region and its magnetic flux or age. However,
there is a dependence of the FIP bias on the evolutionary stage of
the active region. FIP bias shows an increasing trend with average
magnetic flux density up to 200 G but this trend does not continue
at higher values. In contrast to the single values typically used
to characterize the FIP bias in a region, we find that the FIP bias
distribution within active regions has a significant spread. The highest
spread is observed in very dispersed active regions and active regions
that have formed a filament channel along their main polarity inversion
lines, which is an indicator of the wide range of physical processes
that take place in these active regions. These findings indicate that,
while some general trends can be observed, the processes influencing
the composition of an active region are complex and specific to its
evolution, history and magnetic configuration or environment. The
spread of FIP bias values in active regions shows a broad match with
that previously observed in situ in the slow solar wind.

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Title: What have we learned about I-FIP Effect on the Sun from
Hinode/EIS?
Authors: Baker, Deborah; van Driel-Gesztelyi, Lidia
2022cosp...44.2572B Altcode:
Plasma composition in stellar coronae can differ from that of their
photospheres, the cause of which is one of the open questions in
astrophysics. Elements with a low first ionization potential (FIP)
are observed to have either enhanced or depleted abundances relative
to that of high FIP elements. The abundance pattern is known as the FIP
effect or inverse FIP (I-FIP) effect, depending on whether the low FIP
elements are over-/under- (FIP/I-FIP) abundant in coronae. Some stellar
coronae are dominated by FIP effect plasma but cooler, more active stars
are dominated by I-FIP effect plasma. Our local laboratory, the Sun,
has a FIP effect dominated corona, however, short-lived I-FIP patches
have occasionally been observed. Analysis of multiple cases of I-FIP
effect revealed certain conditions in the magnetic field and flare
heating to be necessary for the occurrence of I-FIP effect plasma on
the Sun. An overview of what we have learned from sixteen years of
spatially resolved spectroscopic observations from Hinode/EIS will be
presented. We will demonstrate the power of combining spectroscopic,
imaging, and magnetic field observations of our Sun to understand
the physical processes on cooler stars which we only observe as point
sources.

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Title: Evolution of Plasma Composition in an Eruptive Flux Rope
Authors: Baker, Deborah; Demoulin, Pascal; Long, David; Janvier, Miho;
Green, Lucie; Brooks, David; van Driel-Gesztelyi, Lidia; Mihailescu,
Teodora; To, Andy S. H.; Yardley, Stephanie; Valori, Gherardo
2022cosp...44.1361B Altcode:
Magnetic flux ropes are bundles of twisted magnetic field enveloping a
central axis. They harbor free magnetic energy and can be progenitors
of coronal mass ejections (CMEs). However, identifying flux ropes on
the Sun can be challenging. One of the key coronal observables that
has been shown to indicate the presence of a flux rope is a peculiar
bright coronal structure called a sigmoid. In this work, we show Hinode
EUV Imaging Spectrometer observations of sigmoidal active region (AR)
10977. We analyze the coronal plasma composition in the AR and its
evolution as a sigmoid (flux rope) forms and erupts as a CME. Plasma
with photospheric composition was observed in coronal loops close to
the main polarity inversion line during episodes of significant flux
cancellation, suggestive of the injection of photospheric plasma into
these loops driven by photospheric flux cancellation. Concurrently,
the increasingly sheared core field contained plasma with coronal
composition. As flux cancellation decreased and a sigmoid/flux
rope formed, the plasma evolved to an intermediate composition in
between photospheric and typical AR coronal compositions. Finally,
the flux rope contained predominantly photospheric plasma during and
after a failed eruption preceding the CME. Hence, plasma composition
observations of AR 10977 strongly support models of flux rope formation
by photospheric flux cancellation forcing magnetic reconnection first
at the photospheric level then at the coronal level.

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Title: What Determines Active Region Coronal Plasma Composition?
Authors: Mihailescu, Teodora; Baker, Deborah; Green, Lucie M.;
van Driel-Gesztelyi, Lidia; Long, David M.; Brooks, David H.; To,
Andy S. H.
2022ApJ...933..245M Altcode: 2022arXiv220505027M
The chemical composition of the solar corona is different from that
of the solar photosphere, with the strongest variation being observed
in active regions (ARs). Using data from the Extreme Ultraviolet
(EUV) Imaging Spectrometer (EIS) on Hinode, we present a survey of
coronal elemental composition as expressed in the first ionization
potential (FIP) bias in 28 ARs of different ages and magnetic flux
content, which are at different stages in their evolution. We find
no correlation between the FIP bias of an AR and its total unsigned
magnetic flux or age. However, there is a weak dependence of FIP
bias on the evolutionary stage, decreasing from 1.9 to 2.2 in ARs
with spots to 1.5-1.6 in ARs that are at more advanced stages of
the decay phase. FIP bias shows an increasing trend with average
magnetic flux density up to 200 G, but this trend does not continue
at higher values. The FIP bias distribution within ARs has a spread
between 0.4 and 1. The largest spread is observed in very dispersed
ARs. We attribute this to a range of physical processes taking place
in these ARs, including processes associated with filament channel
formation. These findings indicate that, while some general trends
can be observed, the processes influencing the composition of an AR
are complex and specific to its evolution, magnetic configuration,
or environment. The spread of FIP bias values in ARs shows a broad
match with that previously observed in situ in the slow solar wind.

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Title: The identification of magnetic perturbations in the solar
atmosphere
Authors: Stangalini, Marco; Jafarzadeh, Shahin; Baker, Deborah; Jess,
David; Murabito, Mariarita; Valori, Gherardo
2022cosp...44.2590S Altcode:
Magneto-hydrodynamic (MHD) waves and, in particular, magnetic
perturbations associated with specific wave modes are thought to be
important mechanisms not only for the heating of the outer layers of
the Sun's atmosphere, but also for the elemental abundance anomaly
observed in the corona. High resolution spectropolarimetry is nowadays
progressively extending to the upper layers of the solar atmosphere,
and this provides invaluable insight into MHD wave processes up to
chromospheric heights. However, the identification of real magnetic
perturbations remains a difficult task due to a number of spurious
effects that can mimic the signals associated with them. In this
contribution we will show a novel approach to the identification
of real magnetic oscillations potentially linked to FIP and discuss
proxies to be used in statistical analyses.

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Title: Detection of Stellar-like Abundance Anomalies in the Slow
Solar Wind
Authors: Brooks, David H.; Baker, Deborah; van Driel-Gesztelyi, Lidia;
Warren, Harry P.; Yardley, Stephanie L.
2022ApJ...930L..10B Altcode: 2022arXiv220409332B
The elemental composition of the Sun's hot atmosphere, the corona,
shows a distinctive pattern that is different from the underlying
surface or photosphere. Elements that are easy to ionize in the
chromosphere are enhanced in abundance in the corona compared to
their photospheric values. A similar pattern of behavior is often
observed in the slow-speed (&lt;500 km s-1) solar wind
and in solar-like stellar coronae, while a reversed effect is seen
in M dwarfs. Studies of the inverse effect have been hampered in the
past because only unresolved (point-source) spectroscopic data were
available for these stellar targets. Here we report the discovery of
several inverse events observed in situ in the slow solar wind using
particle-counting techniques. These very rare events all occur during
periods of high solar activity that mimic conditions more widespread
on M dwarfs. The detections allow a new way of connecting the slow
wind to its solar source and are broadly consistent with theoretical
models of abundance variations due to chromospheric fast-mode waves
with amplitudes of 8-10 km s-1, sufficient to accelerate
the solar wind. The results imply that M-dwarf winds are dominated
by plasma depleted in easily ionized elements and lend credence to
previous spectroscopic measurements.

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Title: Extending the FIP bias sample to magnetically active
stars. Challenging the FIP bias paradigm
Authors: Seli, B.; Oláh, K.; Kriskovics, L.; Kővári, Zs.; Vida,
K.; Balázs, L. G.; Laming, J. M.; van Driel-Gesztelyi, L.; Baker, D.
2022A&A...659A...3S Altcode: 2021arXiv211114735S
Context. The different elemental abundances of the photosphere and the
corona are striking features of not only the Sun, but of other stars
as well. This phenomenon is known as the first ionisation potential
(FIP) effect, and its strength can be characterized by the FIP bias,
the logarithmic abundance difference between low- and high-FIP elements
in the corona, compared to the photosphere. The FIP bias was shown to
depend on the surface temperature of the star. Aims: We aim to
extend the Teff−FIP bias relationship to a larger stellar
sample and analyse the effect of other astrophysical parameters on
the relation (e.g. surface gravity, age, activity indicators). Methods: We compiled FIP bias and other parameters for 59 stars
for which coronal composition is available, now including evolved
stars. Using principal component analysis and linear discriminant
analysis, we searched for correlations with other astrophysical
parameters within the sample that may influence the stellar FIP
bias. Results: Adding stars to the Teff−FIP bias
diagram unveiled new features in its structure. In addition to the
previously known relationship, there appears to be a second branch:
a parallel sequence about 0.5 dex above it. While the Teff
remains the main determinant of the FIP bias, other parameters such as
stellar activity indicators also have influence. We find three clusters
in the FIP bias determinant parameter space. One distinct group is
formed by the evolved stars. Two groups contain main sequence stars
in continuation separated roughly by the sign change of the FIP-bias
value. Conclusions: The new branch of the Teff−FIP
bias diagram contains stars with higher activity level, in terms of
X-ray flux and rotational velocity. The Rossby number also seems
to be important, indicating possible dependence on the type of
dynamo operating in these stars influencing their FIP bias. The two
main-sequence clusters run from the earliest spectral types of A-F with
shallow convection zones through G-K-early-M stars with gradually deeper
convection zones, and they end with the fully convective M dwarf stars,
depicting the change of the dynamo type with the internal differences
of the main sequence stars in connection with the FIP-bias values.

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Title: Localizing FRBs through VLBI with the Algonquin Radio
Observatory 10 m Telescope
Authors: Cassanelli, T.; Leung, Calvin; Rahman, M.; Vanderlinde, K.;
Mena-Parra, J.; Cary, S.; Masui, Kiyoshi W.; Luo, Jing; Lin, H. -H.;
Bij, A.; Gill, A.; Baker, D.; Bandura, Kevin; Berger, S.; Boyle, P. J.;
Brar, Charanjot; Chatterjee, S.; Cubranic, D.; Dobbs, Matt; Fonseca,
E.; Good, D. C.; Kaczmarek, J. F.; Kaspi, V. M.; Landecker, T. L.;
Lanman, A. E.; Li, Dongzi; McKee, J. W.; Meyers, B. W.; Michilli,
D.; Naidu, Arun; Ng, Cherry; Patel, Chitrang; Pearlman, Aaron B.;
Pen, U. L.; Pleunis, Ziggy; Quine, Brendan; Renard, A.; Sanghavi,
Pranav; Smith, K. M.; Stairs, Ingrid; Tendulkar, Shriharsh P.
2022AJ....163...65C Altcode: 2021arXiv210705659C
The Canadian Hydrogen Intensity Mapping Experiment (CHIME)/FRB
experiment has detected thousands of fast radio bursts (FRBs) due to its
sensitivity and wide field of view; however, its low angular resolution
prevents it from localizing events to their host galaxies. Very long
baseline interferometry (VLBI), triggered by FRB detections from
CHIME/FRB will solve the challenge of localization for non-repeating
events. Using a refurbished 10 m radio dish at the Algonquin Radio
Observatory located in Ontario Canada, we developed a testbed for a VLBI
experiment with a theoretical λ/D ≲ 30 mas. We provide an overview of
the 10 m system and describe its refurbishment, the data acquisition,
and a procedure for fringe fitting that simultaneously estimates the
geometric delay used for localization and the dispersive delay from
the ionosphere. Using single pulses from the Crab pulsar, we validate
the system and localization procedure, and analyze the clock stability
between sites, which is critical for coherently delay referencing an
FRB event. We find a localization of ~200 mas is possible with the
performance of the current system (single-baseline). Furthermore,
for sources with insufficient signal or restricted wideband to
simultaneously measure both geometric and ionospheric delays,
we show that the differential ionospheric contribution between the
two sites must be measured to a precision of 1 × 10-8 pc
cm-3 to provide a reasonable localization from a detection
in the 400-800 MHz band. Finally we show detection of an FRB observed
simultaneously in the CHIME and the Algonquin 10 m telescope, the
first non-repeating FRB in this long baseline. This project serves as
a testbed for the forthcoming CHIME/FRB Outriggers project.

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Title: A multi-planetary system orbiting the early-M dwarf TOI-1238
Authors: González-Álvarez, E.; Zapatero Osorio, M. R.; Sanz-Forcada,
J.; Caballero, J. A.; Reffert, S.; Béjar, V. J. S.; Hatzes, A. P.;
Herrero, E.; Jeffers, S. V.; Kemmer, J.; López-González, M. J.;
Luque, R.; Molaverdikhani, K.; Morello, G.; Nagel, E.; Quirrenbach,
A.; Rodríguez, E.; Rodríguez-López, C.; Schlecker, M.; Schweitzer,
A.; Stock, S.; Passegger, V. M.; Trifonov, T.; Amado, P. J.; Baker,
D.; Boyd, P. T.; Cadieux, C.; Charbonneau, D.; Collins, K. A.; Doyon,
R.; Dreizler, S.; Espinoza, N.; Fűrész, G.; Furlan, E.; Hesse, K.;
Howell, S. B.; Jenkins, J. M.; Kidwell, R. C.; Latham, D. W.; McLeod,
K. K.; Montes, D.; Morales, J. C.; O'Dwyer, T.; Pallé, E.; Pedraz,
S.; Reiners, A.; Ribas, I.; Quinn, S. N.; Schnaible, C.; Seager, S.;
Skinner, B.; Smith, J. C.; Schwarz, R. P.; Shporer, A.; Vanderspek,
R.; Winn, J. N.
2022A&A...658A.138G Altcode: 2021arXiv211114602G
Context. The number of super-Earth and Earth-mass planet discoveries has
increased significantly in the last two decades thanks to the Doppler
radial velocity and planetary transit observing techniques. Either
technique can detect planet candidates on its own, but the power
of a combined photometric and spectroscopic analysis is unique for
an insightful characterization of the planets, which in turn has
repercussions for our understanding of the architecture of planetary
systems and, therefore, their formation and evolution. Aims: Two
transiting planet candidates with super-Earth radii around the nearby
(d = 70.64 ± 0.06 pc) K7-M0 dwarf star TOI-1238 were announced by
NASA's Transiting Exoplanet Survey Satellite (TESS), which observed
the field of TOI-1238 in four different sectors. We aim to validate
their planetary nature using precise radial velocities taken with
the CARMENES spectrograph. Methods: We obtained 55 CARMENES
radial velocity measurements that span the 11 months between 9 May
2020 and 5 April 2021. For a better characterization of the parent
star's activity, we also collected contemporaneous optical photometric
observations at the Joan Oró and Sierra Nevada observatories and
retrieved archival photometry from the literature. We performed a
combined TESS+CARMENES photometric and spectroscopic analysis by
including Gaussian processes and Keplerian orbits to account for the
stellar activity and planetary signals simultaneously. Results:
We estimate that TOI-1238 has a rotation period of 40 ± 5 d based on
photometric and spectroscopic data. The combined analysis confirms the
discovery of two transiting planets, TOI-1238 b and c, with orbital
periods of 0.764597−0.000011+0.000013
d and 3.294736−0.000036+0.000034 d,
masses of 3.76−1.07+1.15 M⊕
and 8.32−1.88+1.90 M⊕, and
radii of 1.21−0.10+0.11 R⊕ and
2.11−0.14+0.14 R⊕. They orbit
their parent star at semimajor axes of 0.0137 ± 0.0004 au and 0.036 ±
0.001 au, respectively.The two planets are placed on opposite sides of
the radius valley for M dwarfs and lie between the star and the inner
border of TOI-1238's habitable zone. The inner super-Earth TOI-1238
b is one of the densest ultra-short-period planets ever discovered
(ρ = 11.7−3.4+4.2 g cm−3). The
CARMENES data also reveal the presence of an outer, non-transiting,
more massive companion with an orbital period and radial velocity
amplitude of ≥600 d and ≥70 m s−1, which implies a
likely mass of M ≥ 2 √(1− e2) MJup and a
separation ≥1.1 au from its parent star.

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Title: Evolution of Plasma Composition in an Eruptive Flux Rope
Authors: Baker, D.; Green, L. M.; Brooks, D. H.; Démoulin, P.;
van Driel-Gesztelyi, L.; Mihailescu, T.; To, A. S. H.; Long, D. M.;
Yardley, S. L.; Janvier, M.; Valori, G.
2022ApJ...924...17B Altcode: 2021arXiv211011714B
Magnetic flux ropes are bundles of twisted magnetic field enveloping a
central axis. They harbor free magnetic energy and can be progenitors
of coronal mass ejections (CMEs). However, identifying flux ropes on
the Sun can be challenging. One of the key coronal observables that
has been shown to indicate the presence of a flux rope is a peculiar
bright coronal structure called a sigmoid. In this work, we show Hinode
EUV Imaging Spectrometer observations of sigmoidal active region (AR)
10977. We analyze the coronal plasma composition in the AR and its
evolution as a sigmoid (flux rope) forms and erupts as a CME. Plasma
with photospheric composition was observed in coronal loops close to
the main polarity inversion line during episodes of significant flux
cancellation, suggestive of the injection of photospheric plasma into
these loops driven by photospheric flux cancellation. Concurrently,
the increasingly sheared core field contained plasma with coronal
composition. As flux cancellation decreased and a sigmoid/flux
rope formed, the plasma evolved to an intermediate composition in
between photospheric and typical AR coronal compositions. Finally,
the flux rope contained predominantly photospheric plasma during and
after a failed eruption preceding the CME. Hence, plasma composition
observations of AR 10977 strongly support models of flux rope formation
by photospheric flux cancellation forcing magnetic reconnection first
at the photospheric level then at the coronal level.

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Title: Investigating the origin of magnetic perturbations associated
with the FIP Effect
Authors: Murabito, M.; Stangalini, M.; Baker, D.; Valori, G.; Jess,
D. B.; Jafarzadeh, S.; Brooks, D. H.; Ermolli, I.; Giorgi, F.; Grant,
S. D. T.; Long, D. M.; van Driel-Gesztelyi, L.
2021A&A...656A..87M Altcode: 2021arXiv210811164M
Recently, magnetic oscillations were detected in the chromosphere
of a large sunspot and found to be linked to the coronal locations
where a first ionization potential (FIP) effect was observed. In
an attempt to shed light on the possible excitation mechanisms
of these localized waves, we further investigate the same data
by focusing on the relation between the spatial distribution of
the magnetic wave power and the overall field geometry and plasma
parameters obtained from multi-height spectropolarimetric non-local
thermodynamic equilibrium (NLTE) inversions of IBIS data. We find,
in correspondence with the locations where the magnetic wave energy
is observed at chromospheric heights, that the magnetic fields have
smaller scale heights, meaning faster expansions of the field lines,
which ultimately results in stronger vertical density stratification
and wave steepening. In addition, the acoustic spectrum of the
oscillations at the locations where magnetic perturbations are
observed is broader than that observed at other locations, which
suggests an additional forcing driver to the p-modes. Analysis of the
photospheric oscillations in the sunspot surroundings also reveals
a broader spectrum between the two opposite polarities of the active
region (the leading spot and the trailing opposite polarity plage),
and on the same side where magnetic perturbations are observed in
the umbra. We suggest that strong photospheric perturbations between
the two polarities are responsible for this broader spectrum of
oscillations, with respect to the p-mode spectrum, resulting in locally
excited acoustic waves that, after crossing the equipartition layer,
located close to the umbra-penumbra boundary at photopheric heights,
are converted into magnetic waves and steepen due to the strong
density gradient. Movie associated to Fig. 1 is available at <A
href="https://www.aanda.org/10.1051/0004-6361/202141504/olm">https://www.aanda.org</A>

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Title: The high-energy Sun - probing the origins of particle
acceleration on our nearest star
Authors: Matthews, S. A.; Reid, H. A. S.; Baker, D.; Bloomfield, D. S.;
Browning, P. K.; Calcines, A.; Del Zanna, G.; Erdelyi, R.; Fletcher,
L.; Hannah, I. G.; Jeffrey, N.; Klein, L.; Krucker, S.; Kontar, E.;
Long, D. M.; MacKinnon, A.; Mann, G.; Mathioudakis, M.; Milligan,
R.; Nakariakov, V. M.; Pesce-Rollins, M.; Shih, A. Y.; Smith, D.;
Veronig, A.; Vilmer, N.
2021ExA...tmp..135M Altcode:
As a frequent and energetic particle accelerator, our Sun provides
us with an excellent astrophysical laboratory for understanding
the fundamental process of particle acceleration. The exploitation
of radiative diagnostics from electrons has shown that acceleration
operates on sub-second time scales in a complex magnetic environment,
where direct electric fields, wave turbulence, and shock waves all
must contribute, although precise details are severely lacking. Ions
were assumed to be accelerated in a similar manner to electrons, but
γ-ray imaging confirmed that emission sources are spatially separated
from X-ray sources, suggesting distinctly different acceleration
mechanisms. Current X-ray and γ-ray spectroscopy provides only a basic
understanding of accelerated particle spectra and the total energy
budgets are therefore poorly constrained. Additionally, the recent
detection of relativistic ion signatures lasting many hours, without
an electron counterpart, is an enigma. We propose a single platform
to directly measure the physical conditions present in the energy
release sites and the environment in which the particles propagate and
deposit their energy. To address this fundamental issue, we set out
a suite of dedicated instruments that will probe both electrons and
ions simultaneously to observe; high (seconds) temporal resolution
photon spectra (4 keV - 150 MeV) with simultaneous imaging (1 keV -
30 MeV), polarization measurements (5-1000 keV) and high spatial and
temporal resolution imaging spectroscopy in the UV/EUV/SXR (soft X-ray)
regimes. These instruments will observe the broad range of radiative
signatures produced in the solar atmosphere by accelerated particles.

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Title: TOI-1296b and TOI-1298b observed with TESS and SOPHIE:
two hot Saturn-mass exoplanets with different densities around
metal-rich stars
Authors: Moutou, C.; Almenara, J. M.; Hébrard, G.; Santos, N. C.;
Stassun, K. G.; Deheuvels, S.; Barros, S.; Benni, P.; Bieryla, A.;
Boisse, I.; Bonfils, X.; Boyd, P. T.; Collins, K. A.; Baker, D.;
Cortés-Zuleta, P.; Dalal, S.; Debras, F.; Deleuil, M.; Delfosse, X.;
Demangeon, O.; Essack, Z.; Forveille, T.; Girardin, E.; Guerra, P.;
Heidari, N.; Hesse, K.; Hoyer, S.; Jenkins, J. M.; Kiefer, F.; König,
P. C.; Laloum, D.; Latham, D.; Lopez, T.; Martioli, E.; Osborn, H. P.;
Ricker, G.; Seager, S.; Vanderspek, R.; Vezie, M.; Villaseñor, J.;
Winn, J.; Wohler, B.; Ziegler, C.
2021A&A...653A.147M Altcode: 2021arXiv210909252M
We present the discovery of two new transiting extrasolar planet
candidates identified as TOI-1296.01 and TOI-1298.01 by the Transiting
Exoplanet Survey Satellite (TESS). The planetary nature of these
candidates has been secured with the SOPHIE high-precision spectrograph
through the measurement of the companion's mass with the radial velocity
method. Both planets are similar to Saturn in mass and have similar
orbital periods of a few days. They, however, show discrepant radii and
therefore different densities. The radius discrepancy might be explained
by the different levels of irradiation by the host stars. The subgiant
star TOI-1296 hosts a low-density planet with 1.2 RJup
while the less luminous, lower-size star TOI-1298 hosts a much denser
planet with a 0.84 RJup radius, resulting in bulk densities
of 0.198 and 0.743 g cm−3, respectively.In addition, both
stars are strongly enriched in heavy elements, having metallicities
of +0.44 and +0.49 dex, respectively. The planet masses and orbital
periods are 0.298 ± 0.039 MJup and 3.9443715 ± 5.8 ±
10−6 days for TOI-1296b, and 0.356 ± 0.032 MJup
and 4.537164 ± 1.2 ± 10−5 days for TOI-1298b. The mass
measurements have a relative precision of better than 13%. Based
on observations collected with the SOPHIE spectrograph on the 1.93 m
telescope at the Observatoire de Haute-Provence (CNRS), France.

---------------------------------------------------------
Title: Sensitivity of solar wind mass flux to coronal temperature
Authors: Stansby, D.; Berčič, L.; Matteini, L.; Owen, C. J.; French,
R. J.; Baker, D.; Badman, S. T.
2021A&A...650L...2S Altcode: 2020arXiv200913918S
Solar wind models predict that the mass flux carried away from
the Sun in the solar wind should be extremely sensitive to the
temperature in the corona, where the solar wind is accelerated. We
perform a direct test of this prediction in coronal holes and
active regions using a combination of in situ and remote sensing
observations. For coronal holes, a 50% increase in temperature
from 0.8 to 1.2 MK is associated with a tripling of the coronal
mass flux. This trend is maintained within active regions at
temperatures over 2 MK, with a four-fold increase in temperature
corresponding to a 200-fold increase in coronal mass flux. Code
to reproduce the figures presented in this Letter is available at <A
href="https://github.com/dstansby/publication-code">https://github.com/dstansby/publication-code</A>.
PSP and WIND data are available from <A
href="https://spdf.gsfc.nasa.gov/pub/data">https://spdf.gsfc.nasa.gov/pub/data</A>,
GONG data from <A
href="https://gong2.nso.edu/oQR/zqs/">https://gong2.nso.edu/oQR/zqs/</A>,
SDO and SOHO data from <A
href="http://jsoc.stanford.edu/">http://jsoc.stanford.edu/</A>,
and EIS data from <A
href="http://solarb.mssl.ucl.ac.uk/SolarB/">http://solarb.mssl.ucl.ac.uk/SolarB/</A>.

---------------------------------------------------------
Title: Widespread occurrence of high-velocity upflows in solar
active regions
Authors: Yardley, S. L.; Brooks, D. H.; Baker, D.
2021A&A...650L..10Y Altcode: 2021arXiv210601396Y
 Aims: We performed a systematic study of 12 active regions
(ARs) with a broad range of areas, magnetic fluxes, and associated
solar activity in order to determine whether there are upflows present
at the AR boundaries and, if these upflows exist, whether there is
a high-speed asymmetric blue wing component present in them. 
Methods: To identify the presence and locations of the AR upflows, we
derive relative Doppler velocity maps by fitting a Gaussian function
to Hinode/EIS Fe XII 192.394 Å line profiles. To determine whether
there is a high-speed asymmetric component present in the AR upflows,
we fit a double Gaussian function to the Fe XII 192.394 Å mean
spectrum that is computed in a region of interest situated in the
AR upflows. Results: Upflows are observed at both the eastern
and western boundaries of all ARs in our sample, with average upflow
velocities ranging between −5 and −26 km s−1. A blue
wing asymmetry is present in every line profile. The intensity ratio
between the minor high-speed asymmetric Gaussian component compared
to the main component is relatively small for the majority of regions;
however, in a minority of cases (8/30) the ratios are large and range
between 20 and 56 %. Conclusions: These results suggest that
upflows and the high-speed asymmetric blue wing component are a common
feature of all ARs.

---------------------------------------------------------
Title: Plasma Upflows Induced by Magnetic Reconnection Above an
Eruptive Flux Rope
Authors: Baker, Deborah; Mihailescu, Teodora; Démoulin, Pascal;
Green, Lucie M.; van Driel-Gesztelyi, Lidia; Valori, Gherardo; Brooks,
David H.; Long, David M.; Janvier, Miho
2021SoPh..296..103B Altcode: 2021arXiv210616137B
One of the major discoveries of Hinode's Extreme-ultraviolet
Imaging Spectrometer (EIS) is the presence of upflows at the edges
of active regions. As active regions are magnetically connected
to the large-scale field of the corona, these upflows are a likely
contributor to the global mass cycle in the corona. Here we examine
the driving mechanism(s) of the very strong upflows with velocities
in excess of 70 km s−1, known as blue-wing asymmetries,
observed during the eruption of a flux rope in AR 10977 (eruptive flare
SOL2007-12-07T04:50). We use Hinode/EIS spectroscopic observations
combined with magnetic-field modeling to investigate the possible
link between the magnetic topology of the active region and the strong
upflows. A Potential Field Source Surface (PFSS) extrapolation of the
large-scale field shows a quadrupolar configuration with a separator
lying above the flux rope. Field lines formed by induced reconnection
along the separator before and during the flux-rope eruption are
spatially linked to the strongest blue-wing asymmetries in the upflow
regions. The flows are driven by the pressure gradient created when
the dense and hot arcade loops of the active region reconnect with
the extended and tenuous loops overlying it. In view of the fact
that separator reconnection is a specific form of the more general
quasi-separatrix (QSL) reconnection, we conclude that the mechanism
driving the strongest upflows is, in fact, the same as the one driving
the persistent upflows of ≈10 - 20 km s−1 observed in
all active regions.

---------------------------------------------------------
Title: The Evolution of Plasma Composition during a Solar Flare
Authors: To, Andy S. H.; Long, David M.; Baker, Deborah; Brooks, David
H.; van Driel-Gesztelyi, Lidia; Laming, J. Martin; Valori, Gherardo
2021ApJ...911...86T Altcode: 2021arXiv210209985T
We analyze the coronal elemental abundances during a small flare using
Hinode/EIS observations. Compared to the preflare elemental abundances,
we observed a strong increase in coronal abundance of Ca XIV 193.84
Å, an emission line with low first ionization potential (FIP &lt;
10 eV), as quantified by the ratio Ca/Ar during the flare. This is in
contrast to the unchanged abundance ratio observed using Si X 258.38
Å/S X 264.23 Å. We propose two different mechanisms to explain
the different composition results. First, the small flare-induced
heating could have ionized S, but not the noble gas Ar, so that the
flare-driven Alfvén waves brought up Si, S, and Ca in tandem via
the ponderomotive force which acts on ions. Second, the location of
the flare in strong magnetic fields between two sunspots may suggest
fractionation occurred in the low chromosphere, where the background
gas is neutral H. In this region, high-FIP S could behave more like a
low-FIP than a high-FIP element. The physical interpretations proposed
generate new insights into the evolution of plasma abundances in the
solar atmosphere during flaring, and suggests that current models must
be updated to reflect dynamic rather than just static scenarios.

---------------------------------------------------------
Title: Upflows in the Upper Solar Atmosphere
Authors: Tian, Hui; Harra, Louise; Baker, Deborah; Brooks, David H.;
Xia, Lidong
2021SoPh..296...47T Altcode: 2021arXiv210202429T
Spectroscopic observations at extreme- and far-ultraviolet wavelengths
have revealed systematic upflows in the solar transition region and
corona. These upflows are best seen in the network structures of
the quiet Sun and coronal holes, boundaries of active regions, and
dimming regions associated with coronal mass ejections. They have been
intensively studied in the past two decades because they are likely to
be closely related to the formation of the solar wind and heating of the
upper solar atmosphere. We present an overview of the characteristics
of these upflows, introduce their possible formation mechanisms, and
discuss their potential roles in the mass and energy transport in the
solar atmosphere. Although past investigations have greatly improved
our understanding of these upflows, they have left us with several
outstanding questions and unresolved issues that should be addressed
in the future. New observations from the Solar Orbiter mission, the
Daniel K. Inouye Solar Telescope, and the Parker Solar Probe will
likely provide critical information to advance our understanding of
the generation, propagation, and energization of these upflows.

---------------------------------------------------------
Title: Detection of Transiting Exoplanet Candidates at Austin
College's Adams Observatory: Ground-Based Support for NASA's TESS
Mission
Authors: Baker, D.; O'Dwyer, T.; Schnaible, C.; Skinner, B.
2021BAAS...53c1230B Altcode:
NASA's Transiting Exoplanet Survey Satellite (TESS) monitors more than
200,000 stars in the search for transiting exoplanets. One of the
primary goals of the TESS mission is to identify 50 planets smaller
than four Earth radii with measured masses [1]. Because of the wide
field of view and corresponding large pixel size of the TESS telescope,
high precision ground-based observations are needed to confirm planetary
transits and eliminate false positives [2]. The TESS Follow-up Observing
Program Sub Group 1 (TFOP SG1) was developed to coordinate ground-based
photometric follow-up observations [3]. The Adams Observatory at
Austin College provides ground-based photometric support for the TESS
project through TFOP SG1. Located on the roof of the IDEA Center science
building, this facility houses the largest research telescope in north
Texas and offers outstanding opportunities for research, education, and
public outreach. In addition to TFOP, the Adams Observatory contributed
to exoplanet transit observations as a member of the KELT Follow-Up
Network [2]. The main telescope at the Adams Observatory is a 0.61-m f/8
DFM telescope of Ritchey-Chrétien design. When coupled with a Finger
Lakes Instruments (FLI) Proline 16803 imager, this system produces a 26'
× 26' field of view and a 0.38" pixel scale. Under optimal conditions,
we can detect a minimum transit depth of ~3.0 ppt, which for an M-dwarf
star would correspond to an exoplanet with radius ~3 Earth radii. In summer 2020, we observed 11 stars identified by the TESS Science
Team as potentially having exoplanets. Our high-precision follow-up
observations offer three possible scenarios for these TESS targets: 1)
a light curve from the target star indicating a possible transiting
exoplanet, 2) a light curve from a nearby star indicating a nearby
eclipsing binary (NEB) star system, and 3) flat light curves for both
the target star and nearby stars. Of the 11 stars, four stars exhibit
Case 1 behavior and have been verified as planetary candidates. An NEB
has been detected near one target star (Case 2), and the star has been
"retired" from TESS exoplanet studies. Six observations exhibit flat
light curves (Case 3), which could indicate that either the planet
is too small (and the corresponding dip in light too shallow) for
detection at the Adams Observatory, or that the TESS observation is
a false positive. These results may be useful for eliminating other
possible causes of light curve variations in the search for small
Earth-sized exoplanets. [1] Ricker G. R. et al. (2015), JATIS 1(1),
014003. [2] Collins K. A. et al. (2018), AJ 156:234. [3]
Collins K. (2019), AAS Meeting, 2019AAS...23314005C.

---------------------------------------------------------
Title: Spectropolarimetric fluctuations in a sunspot chromosphere
Authors: Stangalini, M.; Baker, D.; Valori, G.; Jess, D. B.;
Jafarzadeh, S.; Murabito, M.; To, A. S. H.; Brooks, D. H.; Ermolli,
I.; Giorgi, F.; MacBride, C. D.
2021RSPTA.37900216S Altcode: 2020arXiv200905302S
The instrumental advances made in this new era of 4 m class solar
telescopes with unmatched spectropolarimetric accuracy and sensitivity
will enable the study of chromospheric magnetic fields and their
dynamics with unprecedented detail. In this regard, spectropolarimetric
diagnostics can provide invaluable insight into magneto-hydrodynamic
(MHD) wave processes. MHD waves and, in particular, Alfvénic
fluctuations associated with particular wave modes were recently
recognized as important mechanisms not only for the heating of the outer
layers of the Sun's atmosphere and the acceleration of the solar wind,
but also for the elemental abundance anomaly observed in the corona
of the Sun and other Sun-like stars (also known as first ionization
potential) effect. Here, we take advantage of state-of-the-art and
unique spectropolarimetric Interferometric BIdimensional Spectrometer
observations to investigate the relation between intensity and circular
polarization (CP) fluctuations in a sunspot chromosphere. Our results
show a clear link between the intensity and CP fluctuations in a patch
which corresponds to a narrow range of magnetic field inclinations. This
suggests the presence of Alfvénic perturbations in the sunspot. This article is part of the Theo Murphy meeting issue `High-resolution
wave dynamics in the lower solar atmosphere'.

---------------------------------------------------------
Title: Alfvénic Perturbations in a Sunspot Chromosphere Linked to
Fractionated Plasma in the Corona
Authors: Baker, Deborah; Stangalini, Marco; Valori, Gherardo; Brooks,
David H.; To, Andy S. H.; van Driel-Gesztelyi, Lidia; Démoulin,
Pascal; Stansby, David; Jess, David B.; Jafarzadeh, Shahin
2021ApJ...907...16B Altcode: 2020arXiv201204308B
In this study, we investigate the spatial distribution of highly
varying plasma composition around one of the largest sunspots of solar
cycle 24. Observations of the photosphere, chromosphere, and corona
are brought together with magnetic field modeling of the sunspot
in order to probe the conditions that regulate the degree of plasma
fractionation within loop populations of differing connectivities. We
find that, in the coronal magnetic field above the sunspot umbra,
the plasma has photospheric composition. Coronal loops rooted in the
penumbra contain fractionated plasma, with the highest levels observed
in the loops that connect within the active region. Tracing field
lines from regions of fractionated plasma in the corona to locations
of Alfvénic fluctuations detected in the chromosphere shows that they
are magnetically linked. These results indicate a connection between
sunspot chromospheric activity and observable changes in coronal
plasma composition.

---------------------------------------------------------
Title: Opening pupils' eyes to the Sun
Authors: French, Ryan; James, Alexander; Baker, Deborah; Dunn, William;
Matthews, Sarah; da Silva Pestana, Brian; Graham, Grace; Shackell,
Benjamin; Carretero, Adam Smith; Trindade, Granger
2020A&G....61.6.22F Altcode:
Ryan French and colleagues discuss their Hinode/EIS outreach work and
the resulting resources available for A-level classes

---------------------------------------------------------
Title: Sensitivity of Solar Wind Mass Flux to Coronal Electron
Temperature
Authors: Stansby, D.; Bercic, L.; Matteini, L.; Owen, C. J.; French,
R.; Baker, D.; Badman, S. T.
2020AGUFMSH0290012S Altcode:
Solar wind models predict that the mass flux carried away from the Sun
in the solar wind should be extremely sensitive to the temperature in
the corona. Using a range of in-situ and remote sensing measurements
from Parker Solar Probe, the Solar Dynamics Observatory, and Hinode/EIS,
we have tested this hypothesis by measuring the coronal electron
temperature and coronal mass flux in both coronal holes and active
region outflows. We find that a three-fold increase in coronal
temperature from 0.7 MK to 2.2 MK results in a large increase in coronal
mass flux by over a factor of 100. This is in qualitative agreement with
current solar wind acceleration models, and provides a new empirical
constraint for future models to be tested against. Our work highlights
how a wide range of remote and in-situ data sources can be combined
to perform new tests of solar wind heating and acceleration theories.

---------------------------------------------------------
Title: Constraint of terrestrial model parameters from ensemble
forward simulations
Authors: Feng, S.; Lauvaux, T.; Williams, C. A.; Zhou, Y.; Baker,
I. T.; Davis, K. J.; Barkley, Z.; Keller, K.; Baker, D.; Schuh, A. E.;
Jacobson, A. R.; Liu, J.; Basu, S.
2020AGUFMA128...03F Altcode:
Recent estimates of the North American carbon budget have
shown a moderate convergence at annual and longer time scales
between terrestrial biogeochemical models (BGCMs) and atmospheric
inversions. However, multi-BGCM comparisons revealed large discrepancies
both spatially and temporally among net ecosystem exchange estimates,
illustrating our limited understanding of the underlying mechanisms. To
bridge the gap between processes and atmospheric inversions, we
propagated process-based errors in a BGCM, here an ensemble of CASA
model simulations, into a mesoscale atmospheric system to identify and
possibly optimize parameters instead of surface fluxes. Our offline
atmospheric-ecosystem coupled model also represent uncertainties from
the atmospheric transport in an ensemble-based framework. The unique
collection of continental Planetary Boundary Layer measurements
of CO2 mixing ratios and meteorological variables from the NASA
Atmospheric Carbon and Transport-America (ACT-America) mission provides
new perspectives on our understanding of transport and fluxes of
greenhouse gases across three regions of the U.S., four seasons, and a
variety of synoptic weather conditions. We have assembled a calibrated,
continental-scale, 27-km resolution atmospheric model ensemble including
biospheric and fossil fuel contributions, prescribing the large-scale
inflow of CO2 from several global models. The ensemble system
can separate and quantify the uncertainties in modeled CO2
mixing ratios from atmospheric transport, biospheric fluxes, fossil
fuel emissions, and boundary inflows. Key parameters of CASA, driving
ecosystem respiration and photosynthetic uptake, are constrained using
both atmospheric mixing ratio measurements. We identified discrepancies
between bottom-up and top-down approaches spatially using aircraft
footprints from a backward Lagrangian particle model, to define optimal
parameter values for dominant ecosystems across the US.

---------------------------------------------------------
Title: The Solar Orbiter Science Activity Plan. Translating solar
and heliospheric physics questions into action
Authors: Zouganelis, I.; De Groof, A.; Walsh, A. P.; Williams, D. R.;
Müller, D.; St Cyr, O. C.; Auchère, F.; Berghmans, D.; Fludra,
A.; Horbury, T. S.; Howard, R. A.; Krucker, S.; Maksimovic, M.;
Owen, C. J.; Rodríguez-Pacheco, J.; Romoli, M.; Solanki, S. K.;
Watson, C.; Sanchez, L.; Lefort, J.; Osuna, P.; Gilbert, H. R.;
Nieves-Chinchilla, T.; Abbo, L.; Alexandrova, O.; Anastasiadis, A.;
Andretta, V.; Antonucci, E.; Appourchaux, T.; Aran, A.; Arge, C. N.;
Aulanier, G.; Baker, D.; Bale, S. D.; Battaglia, M.; Bellot Rubio,
L.; Bemporad, A.; Berthomier, M.; Bocchialini, K.; Bonnin, X.; Brun,
A. S.; Bruno, R.; Buchlin, E.; Büchner, J.; Bucik, R.; Carcaboso,
F.; Carr, R.; Carrasco-Blázquez, I.; Cecconi, B.; Cernuda Cangas, I.;
Chen, C. H. K.; Chitta, L. P.; Chust, T.; Dalmasse, K.; D'Amicis, R.;
Da Deppo, V.; De Marco, R.; Dolei, S.; Dolla, L.; Dudok de Wit, T.;
van Driel-Gesztelyi, L.; Eastwood, J. P.; Espinosa Lara, F.; Etesi,
L.; Fedorov, A.; Félix-Redondo, F.; Fineschi, S.; Fleck, B.; Fontaine,
D.; Fox, N. J.; Gandorfer, A.; Génot, V.; Georgoulis, M. K.; Gissot,
S.; Giunta, A.; Gizon, L.; Gómez-Herrero, R.; Gontikakis, C.; Graham,
G.; Green, L.; Grundy, T.; Haberreiter, M.; Harra, L. K.; Hassler,
D. M.; Hirzberger, J.; Ho, G. C.; Hurford, G.; Innes, D.; Issautier,
K.; James, A. W.; Janitzek, N.; Janvier, M.; Jeffrey, N.; Jenkins,
J.; Khotyaintsev, Y.; Klein, K. -L.; Kontar, E. P.; Kontogiannis,
I.; Krafft, C.; Krasnoselskikh, V.; Kretzschmar, M.; Labrosse, N.;
Lagg, A.; Landini, F.; Lavraud, B.; Leon, I.; Lepri, S. T.; Lewis,
G. R.; Liewer, P.; Linker, J.; Livi, S.; Long, D. M.; Louarn, P.;
Malandraki, O.; Maloney, S.; Martinez-Pillet, V.; Martinovic, M.;
Masson, A.; Matthews, S.; Matteini, L.; Meyer-Vernet, N.; Moraitis,
K.; Morton, R. J.; Musset, S.; Nicolaou, G.; Nindos, A.; O'Brien,
H.; Orozco Suarez, D.; Owens, M.; Pancrazzi, M.; Papaioannou, A.;
Parenti, S.; Pariat, E.; Patsourakos, S.; Perrone, D.; Peter, H.;
Pinto, R. F.; Plainaki, C.; Plettemeier, D.; Plunkett, S. P.; Raines,
J. M.; Raouafi, N.; Reid, H.; Retino, A.; Rezeau, L.; Rochus, P.;
Rodriguez, L.; Rodriguez-Garcia, L.; Roth, M.; Rouillard, A. P.;
Sahraoui, F.; Sasso, C.; Schou, J.; Schühle, U.; Sorriso-Valvo, L.;
Soucek, J.; Spadaro, D.; Stangalini, M.; Stansby, D.; Steller, M.;
Strugarek, A.; Štverák, Š.; Susino, R.; Telloni, D.; Terasa, C.;
Teriaca, L.; Toledo-Redondo, S.; del Toro Iniesta, J. C.; Tsiropoula,
G.; Tsounis, A.; Tziotziou, K.; Valentini, F.; Vaivads, A.; Vecchio,
A.; Velli, M.; Verbeeck, C.; Verdini, A.; Verscharen, D.; Vilmer, N.;
Vourlidas, A.; Wicks, R.; Wimmer-Schweingruber, R. F.; Wiegelmann,
T.; Young, P. R.; Zhukov, A. N.
2020A&A...642A...3Z Altcode: 2020arXiv200910772Z
Solar Orbiter is the first space mission observing the solar plasma
both in situ and remotely, from a close distance, in and out of the
ecliptic. The ultimate goal is to understand how the Sun produces
and controls the heliosphere, filling the Solar System and driving
the planetary environments. With six remote-sensing and four in-situ
instrument suites, the coordination and planning of the operations are
essential to address the following four top-level science questions:
(1) What drives the solar wind and where does the coronal magnetic field
originate?; (2) How do solar transients drive heliospheric variability?;
(3) How do solar eruptions produce energetic particle radiation that
fills the heliosphere?; (4) How does the solar dynamo work and drive
connections between the Sun and the heliosphere? Maximising the
mission's science return requires considering the characteristics
of each orbit, including the relative position of the spacecraft
to Earth (affecting downlink rates), trajectory events (such
as gravitational assist manoeuvres), and the phase of the solar
activity cycle. Furthermore, since each orbit's science telemetry
will be downloaded over the course of the following orbit, science
operations must be planned at mission level, rather than at the level
of individual orbits. It is important to explore the way in which those
science questions are translated into an actual plan of observations
that fits into the mission, thus ensuring that no opportunities are
missed. First, the overarching goals are broken down into specific,
answerable questions along with the required observations and the
so-called Science Activity Plan (SAP) is developed to achieve this. The
SAP groups objectives that require similar observations into Solar
Orbiter Observing Plans, resulting in a strategic, top-level view of
the optimal opportunities for science observations during the mission
lifetime. This allows for all four mission goals to be addressed. In
this paper, we introduce Solar Orbiter's SAP through a series of
examples and the strategy being followed.

---------------------------------------------------------
Title: The Solar Orbiter EUI instrument: The Extreme Ultraviolet
Imager
Authors: Rochus, P.; Auchère, F.; Berghmans, D.; Harra, L.; Schmutz,
W.; Schühle, U.; Addison, P.; Appourchaux, T.; Aznar Cuadrado,
R.; Baker, D.; Barbay, J.; Bates, D.; BenMoussa, A.; Bergmann, M.;
Beurthe, C.; Borgo, B.; Bonte, K.; Bouzit, M.; Bradley, L.; Büchel,
V.; Buchlin, E.; Büchner, J.; Cabé, F.; Cadiergues, L.; Chaigneau,
M.; Chares, B.; Choque Cortez, C.; Coker, P.; Condamin, M.; Coumar,
S.; Curdt, W.; Cutler, J.; Davies, D.; Davison, G.; Defise, J. -M.;
Del Zanna, G.; Delmotte, F.; Delouille, V.; Dolla, L.; Dumesnil, C.;
Dürig, F.; Enge, R.; François, S.; Fourmond, J. -J.; Gillis, J. -M.;
Giordanengo, B.; Gissot, S.; Green, L. M.; Guerreiro, N.; Guilbaud,
A.; Gyo, M.; Haberreiter, M.; Hafiz, A.; Hailey, M.; Halain, J. -P.;
Hansotte, J.; Hecquet, C.; Heerlein, K.; Hellin, M. -L.; Hemsley, S.;
Hermans, A.; Hervier, V.; Hochedez, J. -F.; Houbrechts, Y.; Ihsan,
K.; Jacques, L.; Jérôme, A.; Jones, J.; Kahle, M.; Kennedy, T.;
Klaproth, M.; Kolleck, M.; Koller, S.; Kotsialos, E.; Kraaikamp, E.;
Langer, P.; Lawrenson, A.; Le Clech', J. -C.; Lenaerts, C.; Liebecq,
S.; Linder, D.; Long, D. M.; Mampaey, B.; Markiewicz-Innes, D.;
Marquet, B.; Marsch, E.; Matthews, S.; Mazy, E.; Mazzoli, A.; Meining,
S.; Meltchakov, E.; Mercier, R.; Meyer, S.; Monecke, M.; Monfort,
F.; Morinaud, G.; Moron, F.; Mountney, L.; Müller, R.; Nicula, B.;
Parenti, S.; Peter, H.; Pfiffner, D.; Philippon, A.; Phillips, I.;
Plesseria, J. -Y.; Pylyser, E.; Rabecki, F.; Ravet-Krill, M. -F.;
Rebellato, J.; Renotte, E.; Rodriguez, L.; Roose, S.; Rosin, J.;
Rossi, L.; Roth, P.; Rouesnel, F.; Roulliay, M.; Rousseau, A.; Ruane,
K.; Scanlan, J.; Schlatter, P.; Seaton, D. B.; Silliman, K.; Smit,
S.; Smith, P. J.; Solanki, S. K.; Spescha, M.; Spencer, A.; Stegen,
K.; Stockman, Y.; Szwec, N.; Tamiatto, C.; Tandy, J.; Teriaca, L.;
Theobald, C.; Tychon, I.; van Driel-Gesztelyi, L.; Verbeeck, C.;
Vial, J. -C.; Werner, S.; West, M. J.; Westwood, D.; Wiegelmann, T.;
Willis, G.; Winter, B.; Zerr, A.; Zhang, X.; Zhukov, A. N.
2020A&A...642A...8R Altcode:
Context. The Extreme Ultraviolet Imager (EUI) is part of the remote
sensing instrument package of the ESA/NASA Solar Orbiter mission
that will explore the inner heliosphere and observe the Sun from
vantage points close to the Sun and out of the ecliptic. Solar Orbiter
will advance the "connection science" between solar activity and the
heliosphere. Aims: With EUI we aim to improve our understanding
of the structure and dynamics of the solar atmosphere, globally as well
as at high resolution, and from high solar latitude perspectives. 
Methods: The EUI consists of three telescopes, the Full Sun Imager and
two High Resolution Imagers, which are optimised to image in Lyman-α
and EUV (17.4 nm, 30.4 nm) to provide a coverage from chromosphere
up to corona. The EUI is designed to cope with the strong constraints
imposed by the Solar Orbiter mission characteristics. Limited telemetry
availability is compensated by state-of-the-art image compression,
onboard image processing, and event selection. The imposed power
limitations and potentially harsh radiation environment necessitate
the use of novel CMOS sensors. As the unobstructed field of view of
the telescopes needs to protrude through the spacecraft's heat shield,
the apertures have been kept as small as possible, without compromising
optical performance. This led to a systematic effort to optimise the
throughput of every optical element and the reduction of noise levels
in the sensor. Results: In this paper we review the design
of the two elements of the EUI instrument: the Optical Bench System
and the Common Electronic Box. Particular attention is also given to
the onboard software, the intended operations, the ground software,
and the foreseen data products. Conclusions: The EUI will
bring unique science opportunities thanks to its specific design,
its viewpoint, and to the planned synergies with the other Solar
Orbiter instruments. In particular, we highlight science opportunities
brought by the out-of-ecliptic vantage point of the solar poles,
the high-resolution imaging of the high chromosphere and corona,
and the connection to the outer corona as observed by coronagraphs.

---------------------------------------------------------
Title: Directly comparing coronal and solar wind elemental
fractionation
Authors: Stansby, D.; Baker, D.; Brooks, D. H.; Owen, C. J.
2020A&A...640A..28S Altcode: 2020arXiv200500371S
Context. As the solar wind propagates through the heliosphere, dynamical
processes irreversibly erase the signatures of the near-Sun heating
and acceleration processes. The elemental fractionation of the solar
wind should not change during transit, however, making it an ideal
tracer of these processes. Aims: We aim to verify directly if
the solar wind elemental fractionation is reflective of the coronal
source region fractionation, both within and across different solar wind
source regions. Methods: A backmapping scheme was used to predict
where solar wind measured by the Advanced Composition Explorer (ACE)
originated in the corona. The coronal composition measured by the Hinode
Extreme ultraviolet Imaging Spectrometer (EIS) at the source regions
was then compared with the in situ solar wind composition. 
Results: On hourly timescales, there is no apparent correlation between
coronal and solar wind composition. In contrast, the distribution of
fractionation values within individual source regions is similar in
both the corona and solar wind, but distributions between different
sources have a significant overlap. Conclusions: The matching
distributions directly verify that elemental composition is conserved
as the plasma travels from the corona to the solar wind, further
validating it as a tracer of heating and acceleration processes. The
overlap of fractionation values between sources means it is not possible
to identify solar wind source regions solely by comparing solar wind
and coronal composition measurements, but a comparison can be used to
verify consistency with predicted spacecraft-corona connections.

---------------------------------------------------------
Title: Directly Comparing Coronal and Solar Wind Elemental
Fractionation
Authors: Stansby, D.; Baker, D.; Owen, C.; Brooks, D.
2020SPD....5120801S Altcode:
The elemental fractionation of the quasi-collisionless solar wind
should not change during transit, making it an ideal tracer of coronal
heating and acceleration processes. We aimed to verify directly if the
solar wind elemental fractionation is reflective of the coronal source
region fractionation, both within and across different solar wind
source regions. A backmapping scheme was used to predict where solar
wind measured by the Advanced Composition Explorer (ACE) across 15 days
originated in the corona. The coronal composition measured by Hinode
Extreme ultraviolet Imaging Spectrometer (EIS) at the source regions
was then compared with the in-situ solar wind composition. On hourly
timescales there was no apparent correlation between coronal and solar
wind composition. In contrast, the distribution of fractionation values
within individual source regions was similar in both the corona and
solar wind, but distributions between different sources had significant
overlap. The overlap of fractionation values between sources means it is
not possible to identify solar wind source regions solely by comparing
solar wind and coronal composition measurements, but a comparison can be
used to verify consistency with predicted spacecraft-corona connections.

---------------------------------------------------------
Title: Jupiter's X-ray Emission During the 2007 Solar Minimum
Authors: Dunn, W. R.; Branduardi-Raymont, G.; Carter-Cortez, V.;
Campbell, A.; Elsner, R.; Ness, J. -U.; Gladstone, G. R.; Ford, P.;
Yao, Z.; Rodriguez, P.; Clark, G.; Paranicas, C.; Foster, A.; Baker,
D.; Gray, R.; Badman, S. V.; Ray, L. C.; Bunce, E. Â. J.; Snios,
B.; Jackman, C. M.; Rae, I. J.; Kraft, R.; Rymer, A.; Lathia, S.;
Achilleos, N.
2020JGRA..12527219D Altcode:
The 2007-2009 solar minimum was the longest of the space age. We
present the first of two companion papers on Chandra and XMM-Newton
X-ray campaigns of Jupiter through February-March 2007. We find that
low solar X-ray flux during solar minimum causes Jupiter's equatorial
regions to be exceptionally X-ray dim (0.21 GW at minimum; 0.76 GW at
maximum). While the Jovian equatorial emission varies with solar cycle,
the aurorae have comparably bright intervals at solar minimum and
maximum. We apply atomic charge exchange models to auroral spectra
and find that iogenic plasma of sulphur and oxygen ions provides
excellent fits for XMM-Newton observations. The fitted spectral S:O
ratios of 0.4-1.3 are in good agreement with in situ magnetospheric S:O
measurements of 0.3-1.5, suggesting that the ions that produce Jupiter's
X-ray aurora predominantly originate inside the magnetosphere. The
aurorae were particularly bright on 24-25 February and 8-9 March,
but these two observations exhibit very different spatial, spectral,
and temporal behavior; 24-25 February was the only observation
in this campaign with significant hard X-ray bremsstrahlung from
precipitating electrons, suggesting this may be rare. For 8-9 March,
a bremsstrahlung component was absent, but bright oxygen O6+
lines and best-fit models containing carbon, point to contributions
from solar wind ions. This contribution is absent in the other
observations. Comparing simultaneous Chandra ACIS and XMM-Newton
EPIC spectra showed that ACIS systematically underreported 0.45- to
0.6-keV Jovian emission, suggesting quenching may be less important for
Jupiter's atmosphere than previously thought. We therefore recommend
XMM-Newton for spectral analyses and quantifying opacity/quenching
effects.

---------------------------------------------------------
Title: Can Subphotospheric Magnetic Reconnection Change the Elemental
Composition in the Solar Corona?
Authors: Baker, Deborah; van Driel-Gesztelyi, Lidia; Brooks, David H.;
Démoulin, Pascal; Valori, Gherardo; Long, David M.; Laming, J. Martin;
To, Andy S. H.; James, Alexander W.
2020ApJ...894...35B Altcode: 2020arXiv200303325B
Within the coronae of stars, abundances of those elements with low
first ionization potential (FIP) often differ from their photospheric
values. The coronae of the Sun and solar-type stars mostly show
enhancements of low-FIP elements (the FIP effect) while more active
stars such as M dwarfs have coronae generally characterized by the
inverse-FIP effect (I-FIP). Here we observe patches of I-FIP effect
solar plasma in AR 12673, a highly complex βγδ active region. We
argue that the umbrae of coalescing sunspots, and more specifically
strong light bridges within the umbrae, are preferential locations for
observing I-FIP effect plasma. Furthermore, the magnetic complexity
of the active region and major episodes of fast flux emergence also
lead to repetitive and intense flares. The induced evaporation of
the chromospheric plasma in flare ribbons crossing umbrae enables
the observation of four localized patches of I-FIP effect plasma in
the corona of AR 12673. These observations can be interpreted in the
context of the ponderomotive force fractionation model which predicts
that plasma with I-FIP effect composition is created by the refraction
of waves coming from below the chromosphere. We propose that the waves
generating the I-FIP effect plasma in solar active regions are generated
by subphotospheric reconnection of coalescing flux systems. Although
we only glimpse signatures of I-FIP effect fractionation produced by
this interaction in patches on the Sun, on highly active M stars it
may be the dominant process.

---------------------------------------------------------
Title: Preparing for Geophysical Science Enabled by Crewed and
Robotic Missions on the Surface of the Moon
Authors: Schmerr, N.; Richardson, J.; Ghent, R.; Siegler, M.; Young,
K.; Wasser, M.; Whelley, P.; Buczkowski, D.; Carter, L.; Connor,
C.; Connor, L.; Bleacher, J.; Fouch, M.; Baker, D.; Hurford, T.;
Jozwiak, L.; Kruse, S.; Lekic, V.; Naids, A.; Porter, R.; Montesi, L.;
Richardson, D. C.; Rumpf, E.; Schorghofer, N.; Sunshine, J.; Goossens,
S.; Whelley, N.; Wyrick, D.; Zhu, W.; Bell, E.; DeMartini, J.; Coan,
D.; Akin, D.; Cohen, B.; Mazarico, E.; Neal, C.; Panning, M.; Petro,
N.; Strauss, B.; Weber, R.; Glotch, T.; Hendrix, A.; Parker, A.;
Wright, S.
2020LPICo2241.5048S Altcode:
Geophysics on the Moon will be an important tool for identifying
key targets for geological prospecting, scientific sampling, ISRU,
assessing hazards and risks to crews and infrastructure, and determining
the deep workings of the lunar interior.

---------------------------------------------------------
Title: Geophysical Exploration of the Dynamics and Evolution of the
Solar System (GEODES)
Authors: Schmerr, N.; Richardson, J.; Ghent, R.; Siegler, M.; Young,
K.; Wasser, M.; Whelley, P.; Buczkowski, D.; Carter, L.; Connor,
C.; Connor, L.; Bleacher, J.; Fouch, M.; Baker, D.; Hurford, T.;
Jozwiak, L.; Kruse, S.; Lekic, V.; Naids, A.; Porter, R.; Montesi,
L.; Richardson, D. C.; Rumpf, E.; Schorghofer, N.; Sunshine, J.;
Goossens, S.; Whelley, N.; Wyrick, D.; Zhu, W.; Bell, E.; Coan, D.;
Akin, D.; Cohen, B.; Mazarico, E.; Neal, C. R.; Panning, M.; Petro,
N.; Strauss, B.; Weber, R.; Glotch, T.; Hendrix, A.; Parker, A.;
Wright, S.; DeMartini, J.
2020LPI....51.1621S Altcode:
GEODES is a SSERVI project that is exploring a suite of natural
resources on the Moon, Mars, and asteroids through multidisciplinary
geophysical investigations.

---------------------------------------------------------
Title: Photometric Observations of Possible Exoplanet Transits at
Austin College's Adams Observatory: Ground-Based Support for NASA's
TESS Mission
Authors: Baker, D.; Hannon, N.; Martin, A.; Winterrowd, M.
2020LPICo2195.3059B Altcode:
The Adams Observatory at Austin College provides ground-based
photometric support for the Transiting Exoplanet Survey Satellite
(TESS) Follow-up Observing Program (TFOP). Here we present a summary
of our follow-up observations through November 2019.

---------------------------------------------------------
Title: Active Region Modulation of Coronal Hole Solar Wind
Authors: Macneil, Allan R.; Owen, Christopher J.; Baker, Deborah;
Brooks, David H.; Harra, Louise K.; Long, David M.; Wicks, Robert T.
2019ApJ...887..146M Altcode:
Active regions (ARs) are a candidate source of the slow solar wind
(SW), the origins of which are a topic of ongoing research. We present
a case study that examines the processes by which SW is modulated in
the presence of an AR in the vicinity of the SW source. We compare
properties of SW associated with a coronal hole (CH)-quiet Sun boundary
to SW associated with the same CH but one Carrington rotation later,
when this region bordered the newly emerged NOAA AR 12532. Differences
found in a range of in situ parameters are compared between these
rotations in the context of source region mapping and remote sensing
observations. Marked changes exist in the structure and composition of
the SW, which we attribute to the influence of the AR on SW production
from the CH boundary. These unique observations suggest that the
features that emerge in the AR-associated wind are consistent with an
increased occurrence of interchange reconnection during SW production,
compared with the initial quiet Sun case.

---------------------------------------------------------
Title: Achievements of Hinode in the first eleven years
Authors: Hinode Review Team; Al-Janabi, Khalid; Antolin, Patrick;
Baker, Deborah; Bellot Rubio, Luis R.; Bradley, Louisa; Brooks,
David H.; Centeno, Rebecca; Culhane, J. Leonard; Del Zanna, Giulio;
Doschek, George A.; Fletcher, Lyndsay; Hara, Hirohisa; Harra,
Louise K.; Hillier, Andrew S.; Imada, Shinsuke; Klimchuk, James A.;
Mariska, John T.; Pereira, Tiago M. D.; Reeves, Katharine K.; Sakao,
Taro; Sakurai, Takashi; Shimizu, Toshifumi; Shimojo, Masumi; Shiota,
Daikou; Solanki, Sami K.; Sterling, Alphonse C.; Su, Yingna; Suematsu,
Yoshinori; Tarbell, Theodore D.; Tiwari, Sanjiv K.; Toriumi, Shin;
Ugarte-Urra, Ignacio; Warren, Harry P.; Watanabe, Tetsuya; Young,
Peter R.
2019PASJ...71R...1H Altcode:
Hinode is Japan's third solar mission following Hinotori (1981-1982)
and Yohkoh (1991-2001): it was launched on 2006 September 22 and is in
operation currently. Hinode carries three instruments: the Solar Optical
Telescope, the X-Ray Telescope, and the EUV Imaging Spectrometer. These
instruments were built under international collaboration with the
National Aeronautics and Space Administration and the UK Science and
Technology Facilities Council, and its operation has been contributed
to by the European Space Agency and the Norwegian Space Center. After
describing the satellite operations and giving a performance evaluation
of the three instruments, reviews are presented on major scientific
discoveries by Hinode in the first eleven years (one solar cycle long)
of its operation. This review article concludes with future prospects
for solar physics research based on the achievements of Hinode.

---------------------------------------------------------
Title: Comprehensive Determination of the Hinode/EIS Roll Angle
Authors: Pelouze, Gabriel; Auchère, Frédéric; Bocchialini, Karine;
Harra, Louise; Baker, Deborah; Warren, Harry P.; Brooks, David H.;
Mariska, John T.
2019SoPh..294...59P Altcode: 2019arXiv190311923P
We present a new coalignment method for the EUV Imaging Spectrometer
(EIS) on board the Hinode spacecraft. In addition to the pointing
offset and spacecraft jitter, this method determines the roll angle
of the instrument, which has never been systematically measured, and
which is therefore usually not corrected. The optimal pointing for EIS
is computed by maximizing the cross-correlations of the Fe XII 195.119
Å line with images from the 193 Å band of the Atmospheric Imaging
Assembly (AIA) on board the Solar Dynamics Observatory (SDO). By
coaligning 3336 rasters with high signal-to-noise ratio, we estimate
the rotation angle between EIS and AIA and explore the distribution
of its values. We report an average value of (−0.387±0.007 )
∘. We also provide a software implementation of this method
that can be used to coalign any EIS raster.

---------------------------------------------------------
Title: Transient Inverse-FIP Plasma Composition Evolution within a
Solar Flare
Authors: Baker, Deborah; van Driel-Gesztelyi, Lidia; Brooks, David
H.; Valori, Gherardo; James, Alexander W.; Laming, J. Martin; Long,
David M.; Démoulin, Pascal; Green, Lucie M.; Matthews, Sarah A.;
Oláh, Katalin; Kővári, Zsolt
2019ApJ...875...35B Altcode: 2019arXiv190206948B
Understanding elemental abundance variations in the solar corona
provides an insight into how matter and energy flow from the
chromosphere into the heliosphere. Observed variations depend on the
first ionization potential (FIP) of the main elements of the Sun’s
atmosphere. High-FIP elements (&gt;10 eV) maintain photospheric
abundances in the corona, whereas low-FIP elements have enhanced
abundances. Conversely, inverse FIP (IFIP) refers to the enhancement of
high-FIP or depletion of low-FIP elements. We use spatially resolved
spectroscopic observations, specifically the Ar XIV/Ca XIV intensity
ratio, from Hinode’s Extreme-ultraviolet Imaging Spectrometer to
investigate the distribution and evolution of plasma composition
within two confined flares in a newly emerging, highly sheared
active region. During the decay phase of the first flare, patches
above the flare ribbons evolve from the FIP to the IFIP effect, while
the flaring loop tops show a stronger FIP effect. The patch and loop
compositions then evolve toward the preflare basal state. We propose
an explanation of how flaring in strands of highly sheared emerging
magnetic fields can lead to flare-modulated IFIP plasma composition
over coalescing umbrae which are crossed by flare ribbons. Subsurface
reconnection between the coalescing umbrae leads to the depletion of
low-FIP elements as a result of an increased wave flux from below. This
material is evaporated when the flare ribbons cross the umbrae. Our
results are consistent with the ponderomotive fractionation model for
the creation of IFIP-biased plasma.

---------------------------------------------------------
Title: Origins and Properties of Active Region Solar Wind
Authors: Macneil, Allan; Owen, Christopher; Baker, Deborah; Harra,
Louise; Long, David; Wicks, Robert
2019EGUGA..21.9712M Altcode:
A primary goal of both the recently-launched Parker Solar Probe (PSP)
and upcoming Solar Orbiter (SolO) missions is to identify and explain
the origins of the solar wind. Recent studies have suggested that
active regions (ARs) are the source of a significant fraction of the
solar wind. Of particular interest is the AR contribution to the slow
solar wind; the origins of which are still largely unknown. We present
a case study of a rare opportunity to explain how the solar wind may
emerge from, or be otherwise altered by, an AR, and also to identify the
properties resulting from such a process. A simple backmapping procedure
is applied to combine EUV remote sensing (SDO-AIA and Hinode-EIS) and
in situ (ACE and WIND) observations of the corona and solar wind for
two consecutive Carrington rotations. Contrasting observations during
the latter rotation, when an AR is present at a trailing coronal hole
(CH) boundary, to those during the former, when the AR is yet to emerge,
allows us to isolate the influence of the AR on the solar wind from the
CH boundary in a unique way. This observational strategy is particularly
timely, as the combination of in situ and remote sensing observations,
often from multiple spacecraft, will be critical to the identification
of solar wind origins with PSP and SolO. With this methodology we find
that, as a result of the presence of the AR, there is significant
alteration of solar wind features such as velocity, composition,
structure, and magnetic field orientation. The changes observed when
the AR is present are consistent with the occurrence of interchange
reconnection between AR and CH magnetic fields, which we argue is the
likely mechanism by which the AR solar wind is produced.

---------------------------------------------------------
Title: Contribution of ULF Wave Activity to the Global Recovery of
the Outer Radiation Belt During the Passage of a High-Speed Solar
Wind Stream Observed in September 2014
Authors: Da Silva, L. A.; Sibeck, D.; Alves, L. R.; Souza, V. M.;
Jauer, P. R.; Claudepierre, S. G.; Marchezi, J. P.; Agapitov, O.;
Medeiros, C.; Vieira, L. E. A.; Wang, C.; Jiankui, S.; Liu, Z.;
Gonzalez, W.; Dal Lago, A.; Rockenbach, M.; Padua, M. B.; Alves,
M. V.; Barbosa, M. V. G.; Fok, M. -C.; Baker, D.; Kletzing, C.;
Kanekal, S. G.; Georgiou, M.
2019JGRA..124.1660D Altcode:
Energy coupling between the solar wind and the Earth's magnetosphere can
affect the electron population in the outer radiation belt. However,
the precise role of different internal and external mechanisms that
leads to changes of the relativistic electron population is not entirely
known. This paper describes how ultralow frequency (ULF) wave activity
during the passage of Alfvénic solar wind streams contributes to the
global recovery of the relativistic electron population in the outer
radiation belt. To investigate the contribution of the ULF waves, we
searched the Van Allen Probes data for a period in which we can clearly
distinguish the enhancement of electron fluxes from the background. We
found that the global recovery that started on 22 September 2014, which
coincides with the corotating interaction region preceding a high-speed
stream and the occurrence of persistent substorm activity, provides an
excellent scenario to explore the contribution of ULF waves. To support
our analyses, we employed ground- and space-based observational data
and global magnetohydrodynamic simulations and calculated the ULF wave
radial diffusion coefficients employing an empirical model. Observations
show a gradual increase of electron fluxes in the outer radiation belt
and a concomitant enhancement of ULF activity that spreads from higher
to lower L-shells. Magnetohydrodynamic simulation results agree with
observed ULF wave activity in the magnetotail, which leads to both
fast and Alfvén modes in the magnetospheric nightside sector. The
observations agree with the empirical model and are confirmed by phase
space density calculations for this global recovery period.

---------------------------------------------------------
Title: Outer Van Allen Radiation Belt Response to Interacting
Interplanetary Coronal Mass Ejections
Authors: Kilpua, E. K. J.; Turner, D. L.; Jaynes, A. N.; Hietala,
H.; Koskinen, H. E. J.; Osmane, A.; Palmroth, M.; Pulkkinen, T. I.;
Vainio, R.; Baker, D.; Claudepierre, S. G.
2019JGRA..124.1927K Altcode:
We study the response of the outer Van Allen radiation belt during an
intense magnetic storm on 15-22 February 2014. Four interplanetary
coronal mass ejections (ICMEs) arrived at Earth, of which the three
last ones were interacting. Using data from the Van Allen Probes, we
report the first detailed investigation of electron fluxes from source
(tens of kiloelectron volts) to core (megaelectron volts) energies and
possible loss and acceleration mechanisms as a response to substructures
(shock, sheath and ejecta, and regions of shock-compressed ejecta) in
multiple interacting ICMEs. After an initial enhancement induced by a
shock compression of the magnetosphere, core fluxes strongly depleted
and stayed low for 4 days. This sustained depletion can be related to
a sequence of ICME substructures and their conditions that influenced
the Earth's magnetosphere. In particular, the main depletions occurred
during a high-dynamic pressure sheath and shock-compressed southward
ejecta fields. These structures compressed/eroded the magnetopause close
to geostationary orbit and induced intense and diverse wave activity
in the inner magnetosphere (ULF Pc5, electromagnetic ion cyclotron,
and hiss) facilitating both effective magnetopause shadowing and
precipitation losses. Seed and source electrons in turn experienced
stronger variations throughout the studied interval. The core fluxes
recovered during the last ICME that made a glancing blow to Earth. This
period was characterized by a concurrent lack of losses and sustained
acceleration by chorus and Pc5 waves. Our study highlights that
the seemingly complex behavior of the outer belt during interacting
ICMEs can be understood by the knowledge of electron dynamics during
different substructures.

---------------------------------------------------------
Title: Solar Cycle Observations of the Neon Abundance in the
Sun-as-a-star
Authors: Brooks, David H.; Baker, Deborah; van Driel-Gesztelyi, Lidia;
Warren, Harry P.
2018ApJ...861...42B Altcode: 2018arXiv180507032B
Properties of the Sun’s interior can be determined accurately
from helioseismological measurements of solar oscillations. These
measurements, however, are in conflict with photospheric elemental
abundances derived using 3D hydrodynamic models of the solar
atmosphere. This divergence of theory and helioseismology is known as
the “solar modeling problem.” One possible solution is that the
photospheric neon abundance, which is deduced indirectly by combining
the coronal Ne/O ratio with the photospheric O abundance, is larger
than generally accepted. There is some support for this idea from
observations of cool stars. The Ne/O abundance ratio has also been
found to vary with the solar cycle in the slowest solar wind streams
and coronal streamers, and the variation from solar maximum to minimum
in streamers (∼0.1-0.25) is large enough to potentially bring some
of the solar models into agreement with the seismic data. Here we use
daily sampled observations from the EUV Variability Experiment on the
Solar Dynamics Observatory taken in 2010-2014, to investigate whether
the coronal Ne/O abundance ratio shows a variation with the solar cycle
when the Sun is viewed as a star. We find only a weak dependence on,
and moderate anti-correlation with, the solar cycle with the ratio
measured around 0.2-0.3 MK falling from 0.17 at solar minimum to
0.11 at solar maximum. The effect is amplified at higher temperatures
(0.3-0.6 MK) with a stronger anti-correlation and the ratio falling
from 0.16 at solar minimum to 0.08 at solar maximum. The values we
find at solar minimum are too low to solve the solar modeling problem.

---------------------------------------------------------
Title: Coronal Elemental Abundances in Solar Emerging Flux Regions
Authors: Baker, Deborah; Brooks, David H.; van Driel-Gesztelyi,
Lidia; James, Alexander W.; Démoulin, Pascal; Long, David M.; Warren,
Harry P.; Williams, David R.
2018ApJ...856...71B Altcode: 2018arXiv180108424B
The chemical composition of solar and stellar atmospheres differs from
the composition of their photospheres. Abundances of elements with low
first ionization potential (FIP) are enhanced in the corona relative
to high-FIP elements with respect to the photosphere. This is known as
the FIP effect and it is important for understanding the flow of mass
and energy through solar and stellar atmospheres. We used spectroscopic
observations from the Extreme-ultraviolet Imaging Spectrometer on board
the Hinode observatory to investigate the spatial distribution and
temporal evolution of coronal plasma composition within solar emerging
flux regions inside a coronal hole. Plasma evolved to values exceeding
those of the quiet-Sun corona during the emergence/early-decay phase
at a similar rate for two orders of magnitude in magnetic flux, a rate
comparable to that observed in large active regions (ARs) containing
an order of magnitude more flux. During the late-decay phase, the rate
of change was significantly faster than what is observed in large,
decaying ARs. Our results suggest that the rate of increase during the
emergence/early-decay phase is linked to the fractionation mechanism
that leads to the FIP effect, whereas the rate of decrease during
the later decay phase depends on the rate of reconnection with the
surrounding magnetic field and its plasma composition.

---------------------------------------------------------
Title: A Solar cycle correlation of coronal element abundances in
Sun-as-a-star observations
Authors: Brooks, David H.; Baker, Deborah; van Driel-Gesztelyi, Lidia;
Warren, Harry P.
2017NatCo...8..183B Altcode: 2018arXiv180200563B
The elemental composition in the coronae of low-activity solar-like
stars appears to be related to fundamental stellar properties such as
rotation, surface gravity, and spectral type. Here we use full-Sun
observations from the Solar Dynamics Observatory, to show that when
the Sun is observed as a star, the variation of coronal composition
is highly correlated with a proxy for solar activity, the F10.7 cm
radio flux, and therefore with the solar cycle phase. Similar cyclic
variations should therefore be detectable spectroscopically in X-ray
observations of solar analogs. The plasma composition in full-disk
observations of the Sun is related to the evolution of coronal magnetic
field activity. Our observations therefore introduce an uncertainty
into the nature of any relationship between coronal composition and
fixed stellar properties. The results highlight the importance of
systematic full-cycle observations for understanding the elemental
composition of solar-like stellar coronae.

---------------------------------------------------------
Title: A study of the long term evolution in active region upflows
Authors: Harra, Louise K.; Ugarte-Urra, Ignacio; De Rosa, Marc;
Mandrini, Cristina; van Driel-Gesztelyi, Lidia; Baker, Deborah;
Culhane, J. Leonard; Démoulin, Pascal
2017PASJ...69...47H Altcode:
Since their discovery, upflows at the edges of active regions have
attracted a lot of interest, primarily as they could potentially
contribute to the slow solar wind. One aspect that has not been studied
yet is how the long term evolution of active regions impacts the
upflows. In this work, we analyze one active region that survives three
solar rotations. We track how the flows change with time. We use local
and global modeling of the decaying active region to determine how the
age of the active region will impact the extent of the open magnetic
fields, and then how some of the upflows could become outflows. We
finish with a discussion of how these results, set in a broader context,
can be further developed with the Solar Orbiter mission.

---------------------------------------------------------
Title: On-Disc Observations of Flux Rope Formation Prior to Its
Eruption
Authors: James, A. W.; Green, L. M.; Palmerio, E.; Valori, G.; Reid,
H. A. S.; Baker, D.; Brooks, D. H.; van Driel-Gesztelyi, L.; Kilpua,
E. K. J.
2017SoPh..292...71J Altcode: 2017arXiv170310837J
Coronal mass ejections (CMEs) are one of the primary manifestations of
solar activity and can drive severe space weather effects. Therefore,
it is vital to work towards being able to predict their
occurrence. However, many aspects of CME formation and eruption
remain unclear, including whether magnetic flux ropes are present
before the onset of eruption and the key mechanisms that cause CMEs
to occur. In this work, the pre-eruptive coronal configuration of
an active region that produced an interplanetary CME with a clear
magnetic flux rope structure at 1 AU is studied. A forward-S sigmoid
appears in extreme-ultraviolet (EUV) data two hours before the onset
of the eruption (SOL2012-06-14), which is interpreted as a signature
of a right-handed flux rope that formed prior to the eruption. Flare
ribbons and EUV dimmings are used to infer the locations of the flux
rope footpoints. These locations, together with observations of the
global magnetic flux distribution, indicate that an interaction between
newly emerged magnetic flux and pre-existing sunspot field in the days
prior to the eruption may have enabled the coronal flux rope to form
via tether-cutting-like reconnection. Composition analysis suggests
that the flux rope had a coronal plasma composition, supporting our
interpretation that the flux rope formed via magnetic reconnection in
the corona. Once formed, the flux rope remained stable for two hours
before erupting as a CME.

---------------------------------------------------------
Title: Apparent and Intrinsic Evolution of Active Region Upflows
Authors: Baker, Deborah; Janvier, Miho; Démoulin, Pascal; Mandrini,
Cristina H.
2017SoPh..292...46B Altcode: 2017arXiv170206022B
We analyze the evolution of Fe XII coronal plasma upflows from
the edges of ten active regions (ARs) as they cross the solar disk
using the Hinode Extreme Ultraviolet Imaging Spectrometer (EIS) to do
this. Confirming the results of Démoulin et al. (Sol. Phys.283, 341,
2013), we find that for each AR there is an observed long-term evolution
of the upflows. This evolution is largely due to the solar rotation
that progressively changes the viewpoint of dominantly stationary
upflows. From this projection effect, we estimate the unprojected
upflow velocity and its inclination to the local vertical. AR upflows
typically fan away from the AR core by 40° to nearly vertical
for the following polarity. The span of inclination angles is more
spread out for the leading polarity, with flows angled from −29°
(inclined toward the AR center) to 28° (directed away from the
AR). In addition to the limb-to-limb apparent evolution, we identify
an intrinsic evolution of the upflows that is due to coronal activity,
which is AR dependent. Furthermore, line widths are correlated with
Doppler velocities only for the few ARs with the highest velocities. We
conclude that for the line widths to be affected by the solar rotation,
the spatial gradient of the upflow velocities must be large enough
such that the line broadening exceeds the thermal line width of Fe
XII. Finally, we find that upflows occurring in pairs or multiple
pairs are a common feature of ARs observed by Hinode/EIS, with up to
four pairs present in AR 11575. This is important for constraining the
upflow-driving mechanism as it implies that the mechanism is not local
and does not occur over a single polarity. AR upflows originating from
reconnection along quasi-separatrix layers between overpressure AR
loops and neighboring underpressure loops is consistent with upflows
occurring in pairs, unlike other proposed mechanisms that act locally
in one polarity.

---------------------------------------------------------
Title: MMS Super-Conjunction Studies of Chorus Wave Properties and
Their Effects on Energetic Electrons
Authors: Jaynes, A. N.; Baker, D.; Blake, J. B.; Kletzing, C.; Zhao,
H.; Leonard, T. W.; Turner, D. L.; Fennell, J. F.; Wilder, F. D.;
Kanekal, S. G.; Schiller, Q.; Mauk, B.; Cohen, I.
2016AGUFMSM43E..07J Altcode:
During the first full sweep of NASA's MMS mission through the
Earth's magnetotail, referred to as Phase 1x, the active state of the
geomagnetic environment allowed many opportunities for new insights
into inner magnetospheric dynamics. Of particular interest is the
local generation of whistler-mode chorus waves and their subsequent
effect on energetic electrons. In this study, we take advantage of
conjunctions between MMS and the rest of the Heliospheric System
Observatory satellites, including one super-conjunction event on
01 May 2016, when both Van Allen Probes and MMS were all within 1
Re of each other at the same time. Using multipoint measurements,
we examine the properties and effects of chorus in fine detail. This
concentration of observation points in the chorus generation region
unveils new understanding of the wave-particle interactions that
accelerate electrons and form the Earth's radiation belts.

---------------------------------------------------------
Title: Evolution of the magnetic field distribution of active regions
Authors: Dacie, S.; Démoulin, P.; van Driel-Gesztelyi, L.; Long,
D. M.; Baker, D.; Janvier, M.; Yardley, S. L.; Pérez-Suárez, D.
2016A&A...596A..69D Altcode: 2016arXiv160903723D
 Aims: Although the temporal evolution of active regions (ARs)
is relatively well understood, the processes involved continue to be
the subject of investigation. We study how the magnetic field of a
series of ARs evolves with time to better characterise how ARs emerge
and disperse. Methods: We examined the temporal variation in
the magnetic field distribution of 37 emerging ARs. A kernel density
estimation plot of the field distribution was created on a log-log
scale for each AR at each time step. We found that the central portion
of the distribution is typically linear, and its slope was used to
characterise the evolution of the magnetic field. Results:
The slopes were seen to evolve with time, becoming less steep as the
fragmented emerging flux coalesces. The slopes reached a maximum value
of -1.5 just before the time of maximum flux before becoming steeper
during the decay phase towards the quiet-Sun value of -3. This behaviour
differs significantly from a classical diffusion model, which produces
a slope of -1. These results suggest that simple classical diffusion
is not responsible for the observed changes in field distribution, but
that other processes play a significant role in flux dispersion. 
Conclusions: We propose that the steep negative slope seen during the
late-decay phase is due to magnetic flux reprocessing by (super)granular
convective cells.

---------------------------------------------------------
Title: Current energetic particle sensors
Authors: Fennell, J. F.; Blake, J. B.; Claudepierre, S.; Mazur, J.;
Kanekal, S.; O'Brien, P.; Baker, D.; Crain, W.; Mabry, D.; Clemmons, J.
2016JGRA..121.8840F Altcode:
Several energetic particle sensors designed to make measurements in
the current decade are described and their technology and capabilities
discussed and demonstrated. Most of these instruments are already on
orbit or approaching launch. These include the Magnetic Electron Ion
Spectrometers (MagEIS) and the Relativistic Electron Proton Telescope
(REPT) that are flying on the Van Allen Probes, the Fly's Eye Electron
Proton Spectrometers (FEEPS) flying on the Magnetospheric Multiscale
(MMS) mission, and Dosimeters flying on the AC6 Cubesat mission. We
focus mostly on the electron measurement capability of these sensors
while providing summary comments of their ion measurement capabilities
if they have any.

---------------------------------------------------------
Title: Photospheric Vector Magnetic Field Evolution of NOAA Active
Region 11504 and the Ensuing CME
Authors: James, Alexander; Green, Lucie; Valori, Gherardo; van
Driel-Gesztelyi, Lidia; Baker, Deborah; Brooks, David; Palmerio, Erika
2016SPD....4730305J Altcode:
Coronal mass ejections (CMEs) are eruptions of billions of tonnes of
plasma from the Sun that drive the most severe space weather effects
we observe. In order to be able to produce forecasts of space weather
with lead times of the order of days, accurate predictions of the
occurrence of CMEs must be developed. The eruptive active-region
studied in this work (NOAA 11504) is complex, featuring fragmentation
of penumbral magnetic field in the days prior to eruption, as well as
rotation of the leading sunspot. SDO/HMI vector photospheric magnetic
field measurements are utilised alongside SDO/AIA multi-wavelength
extreme ultra-violet (EUV) observations to study the dynamics of the
photospheric and coronal structures, as well as Hinode/EIS spectroscopic
measurements, including elemental composition data. The EUV data show
flare ribbons as well as coronal dimmings, which are used to infer
the orientation of the erupting flux rope. This flux rope orientation
is then compared to in situ measurements of the flux rope. The vector
magnetic field data is used to determine the possible contributions
the field fragmentation and sunspot rotation may have made to the
formation of the flux rope and the triggering of the CME.

---------------------------------------------------------
Title: Preface: Probing the Sun Inside and Out
Authors: Harra, Louise; Baker, Deborah; Howe, Rachel; Leibacher,
John; van Driel-Gesztelyi, Lidia
2015SoPh..290.3091H Altcode: 2015SoPh..tmp..167H
No abstract at ADS

---------------------------------------------------------
Title: Persistent Near-Surface Flow Structures from Local
Helioseismology
Authors: Howe, Rachel; Komm, R. W.; Baker, D.; Harra, L.; van
Driel-Gesztelyi, L.; Bogart, R. S.
2015SoPh..290.3137H Altcode: 2015arXiv150706525H; 2015SoPh..tmp..115H
Near-surface flows measured by the ring-diagram technique of local
helioseismology show structures that persist over multiple rotations. We
examine these phenomena using data from the Global Oscillation Network
Group (GONG) and the Helioseismic and Magnetic Imager (HMI) and show
that a correlation analysis of the structures can be used to estimate
the rotation rate as a function of latitude, giving a result consistent
with the near-surface rate from global helioseismology and slightly
slower than that obtained from a similar analysis of the surface
magnetic field strength. At latitudes of 60∘ and above,
the HMI flow data reveal a strong signature of a two-sided zonal flow
structure. This signature may be related to recent reports of "giant
cells" in solar convection.

---------------------------------------------------------
Title: A Study of the Coronal Non-thermal Velocity in Polar Regions
During the Rise from Solar Minimum to Solar Maximum in Cycle 24
Authors: Harra, L.; Baker, D.; Edwards, S. J.; Hara, H.; Howe, R.;
van Driel-Gesztelyi, L.
2015SoPh..290.3203H Altcode: 2015SoPh..tmp....8H
We explore the changes in coronal non-thermal velocity (Vnt)
measurements at the poles from solar minimum to solar maximum using
Hinode EUV Imaging Spectrometer data. We find that although the
intensity in the corona at the poles does tend to increase with
the cycle, there are no significant changes in the Vnt
values. The locations of enhanced Vnt values measured do not
always have a counterpart in intensity, and they are sometimes located
in weak emission regions. Unipolar magnetic streams, created through
diffusion of the following polarity of the decaying active regions,
slowly progress towards the poles. These streams are expected to
be related to magnetic nulls as locations that indicate an increased
likelihood for magnetic reconnection to occur. Through global potential
field source-surface modelling, we determine how the number of nulls
varied during the cycle and find that those that lie at &lt; 1.1
solar radii vary significantly. We search for a correlation between
the variation of the magnetic nulls and the Vnt values,
as it may be expected that with an increasing number of nulls, the
Vnt values in the corona increase as well. There is no
correlation with the Vnt values, however. This indicates
that the magnetic structures that create the enhanced Vnt
behaviour are small-scale features and hence not easily measurable at
the poles. Because they do not change during the solar cycle, they are
likely to be created by a local dynamo. The variation of the upper
range of Vnt is reduced, which highlights that strongly
dynamic behaviour is reduced as the solar maximum approaches. This
is likely to be due to the reduced area of the polar coronal hole,
which allows fewer opportunities for reconnection to occur between
open and closed magnetic fields.

---------------------------------------------------------
Title: Source of a Prominent Poleward Surge During Solar Cycle 24
Authors: Yeates, A. R.; Baker, D.; van Driel-Gesztelyi, L.
2015SoPh..290.3189Y Altcode: 2015SoPh..tmp...18Y; 2015arXiv150204854Y
As an observational case study, we consider the origin of a prominent
poleward surge of leading polarity, visible in the magnetic butterfly
diagram during Solar Cycle 24. A new technique is developed for
assimilating individual regions of strong magnetic flux into a
surface-flux transport model. By isolating the contribution of each
of these regions, the model shows the surge to originate primarily in
a single high-latitude activity group consisting of a bipolar active
region present in Carrington Rotations 2104 - 05 (November 2010 -
January 2011) and a multipolar active region in Rotations 2107 - 08
(February - April 2011). This group had a strong axial dipole moment
opposed to Joy's law. On the other hand, the modelling suggests that
the transient influence of this group on the butterfly diagram will
not be matched by a large long-term contribution to the polar field
because it is located at high latitude. This is in accordance with
previous flux-transport models.

---------------------------------------------------------
Title: Parallel Evolution of Quasi-separatrix Layers and Active
Region Upflows
Authors: Mandrini, C. H.; Baker, D.; Démoulin, P.; Cristiani, G. D.;
van Driel-Gesztelyi, L.; Vargas Domínguez, S.; Nuevo, F. A.; Vásquez,
A. M.; Pick, M.
2015ApJ...809...73M Altcode: 2015arXiv150701264M
Persistent plasma upflows were observed with Hinode’s EUV
Imaging Spectrometer (EIS) at the edges of active region (AR)
10978 as it crossed the solar disk. We analyze the evolution of
the photospheric magnetic and velocity fields of the AR, model
its coronal magnetic field, and compute the location of magnetic
null-points and quasi-sepratrix layers (QSLs) searching for the origin
of EIS upflows. Magnetic reconnection at the computed null points
cannot explain all of the observed EIS upflow regions. However, EIS
upflows and QSLs are found to evolve in parallel, both temporarily
and spatially. Sections of two sets of QSLs, called outer and
inner, are found associated to EIS upflow streams having different
characteristics. The reconnection process in the outer QSLs is forced
by a large-scale photospheric flow pattern, which is present in the AR
for several days. We propose a scenario in which upflows are observed,
provided that a large enough asymmetry in plasma pressure exists
between the pre-reconnection loops and lasts as long as a photospheric
forcing is at work. A similar mechanism operates in the inner QSLs; in
this case, it is forced by the emergence and evolution of the bipoles
between the two main AR polarities. Our findings provide strong support
for the results from previous individual case studies investigating the
role of magnetic reconnection at QSLs as the origin of the upflowing
plasma. Furthermore, we propose that persistent reconnection along
QSLs does not only drive the EIS upflows, but is also responsible for
the continuous metric radio noise-storm observed in AR 10978 along
its disk transit by the Nançay Radio Heliograph.

---------------------------------------------------------
Title: 49 new T dwarfs identified using methane imaging
Authors: Cardoso, C. V.; Burningham, B.; Smart, R. L.; van Spaandonk,
L.; Baker, D.; Smith, L. C.; Zhang, Z. H.; Andrei, A. H.; Bucciarelli,
B.; Dhital, S.; Jones, H. R. A.; Lattanzi, M. G.; Magazzú, A.;
Pinfield, D. J.; Tinney, C. G.
2015MNRAS.450.2486C Altcode: 2015arXiv150206503C
We present the discovery of 49 new photometrically classified T
dwarfs from the combination of large infrared and optical surveys
combined with follow-up Telescopio Nazionale Galileo photometry. We
used multiband infrared and optical photometry from the United Kingdom
Infrared Telescope and Sloan Digital Sky Surveys to identify possible
brown dwarf candidates, which were then confirmed using methane filter
photometry. We have defined a new photometric conversion between
CH4s - CH4l colour and spectral type for T4-T8
brown dwarfs based on a part of the sample that has been followed up
using methane photometry and spectroscopy. Using methane differential
photometry as a proxy for spectral type for T dwarfs has proved to
be a very efficient technique. Of a subset of 45 methane selected
brown dwarfs that were observed spectroscopically, 100 per cent were
confirmed as T dwarfs. Future deep imaging surveys will produce large
samples of faint brown dwarf candidates, for which spectroscopy will
not be feasible. When broad wavelength coverage is unavailable, methane
imaging offers a means to efficiently classify candidates from such
surveys using just a pair of near-infrared images.

---------------------------------------------------------
Title: FIP Bias Evolution in a Decaying Active Region
Authors: Baker, D.; Brooks, D. H.; Démoulin, P.; Yardley, S. L.;
van Driel-Gesztelyi, L.; Long, D. M.; Green, L. M.
2015ApJ...802..104B Altcode: 2015arXiv150107397B
Solar coronal plasma composition is typically characterized by
first ionization potential (FIP) bias. Using spectra obtained by
Hinode’s EUV Imaging Spectrometer instrument, we present a series
of large-scale, spatially resolved composition maps of active region
(AR)11389. The composition maps show how FIP bias evolves within the
decaying AR during the period 2012 January 4-6. Globally, FIP bias
decreases throughout the AR. We analyzed areas of significant plasma
composition changes within the decaying AR and found that small-scale
evolution in the photospheric magnetic field is closely linked to the
FIP bias evolution observed in the corona. During the AR’s decay
phase, small bipoles emerging within supergranular cells reconnect
with the pre-existing AR field, creating a pathway along which
photospheric and coronal plasmas can mix. The mixing timescales are
shorter than those of plasma enrichment processes. Eruptive activity
also results in shifting the FIP bias closer to photospheric in the
affected areas. Finally, the FIP bias still remains dominantly coronal
only in a part of the AR’s high-flux density core. We conclude that
in the decay phase of an AR’s lifetime, the FIP bias is becoming
increasingly modulated by episodes of small-scale flux emergence,
i.e., decreasing the AR’s overall FIP bias. Our results show that
magnetic field evolution plays an important role in compositional
changes during AR development, revealing a more complex relationship
than expected from previous well-known Skylab results showing that
FIP bias increases almost linearly with age in young ARs.

---------------------------------------------------------
Title: The energetics of a global shock wave in the low solar corona
Authors: Long, David; Baker, Deborah; Williams, David; Carley, Eoin;
Gallagher, Peter; Zucca, Pietro
2015TESS....140706L Altcode:
As the most energetic eruptions in the solar system, coronal mass
ejections (CMEs) can produce shock waves at both their front and flanks
as they erupt from the Sun into the heliosphere. However, the amount of
energy produced in these eruptions, and the proportion of their energy
required to produce the waves, is not well characterised. Here we use
observations of a solar eruption from 2014 February 25 to estimate
the energy budget of an erupting CME and the globally-propagating
"EIT wave" produced by the rapid expansion of the CME flanks in the
low solar corona. The "EIT wave" is shown using a combination of
radio spectra and extreme ultraviolet images to be a shock front
with a Mach number greater than one. Its initial energy is then
calculated using the Sedov-Taylor blast-wave approximation, which
provides an approximation for a shock front propagating through a
region of variable density. This approach provides an initial energy
estimate of ~2.8 x 10^31 ergs to produce the "EIT wave", which is
approximately 10% the kinetic energy of the associated CME (shown to
be ~2.5 x 10^32 ergs). These results indicate that the energy of the
"EIT wave" may be significant and must be considered when estimating
the total energy budget of solar eruptions.

---------------------------------------------------------
Title: The Energetics of a Global Shock Wave in the Low Solar Corona
Authors: Long, David M.; Baker, Deborah; Williams, David R.; Carley,
Eoin P.; Gallagher, Peter T.; Zucca, Pietro
2015ApJ...799..224L Altcode: 2014arXiv1412.2964L
As the most energetic eruptions in the solar system, coronal mass
ejections (CMEs) can produce shock waves at both their front and flanks
as they erupt from the Sun into the heliosphere. However, the amount of
energy produced in these eruptions, and the proportion of their energy
required to produce the waves, is not well characterized. Here we use
observations of a solar eruption from 2014 February 25 to estimate
the energy budget of an erupting CME and the globally propagating
"EIT wave" produced by the rapid expansion of the CME flanks in the
low solar corona. The "EIT wave" is shown using a combination of radio
spectra and extreme ultraviolet images to be a shock front with a
Mach number greater than one. Its initial energy is then calculated
using the Sedov-Taylor blast-wave approximation, which provides an
approximation for a shock front propagating through a region of variable
density. This approach provides an initial energy estimate of ≈2.8 ×
1031 erg to produce the "EIT wave," which is approximately
10% the kinetic energy of the associated CME (shown to be ≈2.5 ×
1032 erg). These results indicate that the energy of the
"EIT wave" may be significant and must be considered when estimating
the total energy budget of solar eruptions.

---------------------------------------------------------
Title: How Can Active Region Plasma Escape into the Solar Wind from
Below a Closed Helmet Streamer?
Authors: Mandrini, C. H.; Nuevo, F. A.; Vásquez, A. M.; Démoulin,
P.; van Driel-Gesztelyi, L.; Baker, D.; Culhane, J. L.; Cristiani,
G. D.; Pick, M.
2014SoPh..289.4151M Altcode: 2014arXiv1409.7369M; 2014SoPh..tmp..115M
Recent studies show that active-region (AR) upflowing plasma,
observed by the EUV-Imaging Spectrometer (EIS) onboard Hinode, can
gain access to open-field lines and be released into the solar wind
(SW) via magnetic-interchange reconnection at magnetic null-points in
pseudo-streamer configurations. When only one bipolar AR is present
on the Sun and is fully covered by the separatrix of a streamer, such
as AR 10978 in December 2007, it seems unlikely that the upflowing AR
plasma can find its way into the slow SW. However, signatures of plasma
with AR composition have been found at 1 AU by Culhane et al. (Solar
Phys.289, 3799, 2014) that apparently originated west of AR 10978. We
present a detailed topology analysis of AR 10978 and the surrounding
large-scale corona based on a potential-field source-surface (PFSS)
model. Our study shows that it is possible for the AR plasma to move
around the streamer separatrix and be released into the SW via magnetic
reconnection, which occurs in at least two main steps. We analyse data
from the Nançay Radioheliograph (NRH) in a search for evidence of the
chain of magnetic reconnections that we propose. We find a noise storm
above the AR and several varying sources at 150.9 MHz. Their locations
suggest that they might be associated with particles accelerated during
the first-step reconnection process at a null point well outside of
the AR. We find no evidence of the second reconnection step in the
radio data, however. Our results demonstrate that even when it appears
highly improbable for the AR plasma to reach the SW, indirect channels
involving a sequence of reconnections can make it possible.

---------------------------------------------------------
Title: Tracking Solar Active Region Outflow Plasma from Its Source
to the Near-Earth Environment
Authors: Culhane, J. L.; Brooks, D. H.; van Driel-Gesztelyi, L.;
Démoulin, P.; Baker, D.; DeRosa, M. L.; Mandrini, C. H.; Zhao, L.;
Zurbuchen, T. H.
2014SoPh..289.3799C Altcode: 2014SoPh..tmp...90C; 2014arXiv1405.2949C
Seeking to establish whether active-region upflow material contributes
to the slow solar wind, we examine in detail the plasma upflows from
Active Region (AR) 10978, which crossed the Sun's disc in the interval 8
to 16 December 2007 during Carrington rotation (CR) 2064. In previous
work, using data from the Hinode/EUV Imaging Spectrometer, upflow
velocity evolution was extensively studied as the region crossed the
disc, while a linear force-free-field magnetic extrapolation was used
to confirm aspects of the velocity evolution and to establish the
presence of quasi-separatrix layers at the upflow source areas. The
plasma properties, temperature, density, and first ionisation potential
bias [FIP-bias] were measured with the spectrometer during the disc
passage of the active region. Global potential-field source-surface
(PFSS) models showed that AR 10978 was completely covered by the
closed field of a helmet streamer that is part of the streamer
belt. Therefore it is not clear how any of the upflowing AR-associated
plasma could reach the source surface at 2.5 R⊙ and
contribute to the slow solar wind. However, a detailed examination of
solar-wind in-situ data obtained by the Advanced Composition Explorer
(ACE) spacecraft at the L1 point shows that increases in
O7+/O6+, C6+/C5+, and Fe/O -
a FIP-bias proxy - are present before the heliospheric current-sheet
crossing. These increases, along with an accompanying reduction in
proton velocity and an increase in density are characteristic of
both AR and slow-solar-wind plasma. Finally, we describe a two-step
reconnection process by which some of the upflowing plasma from the
AR might reach the heliosphere.

---------------------------------------------------------
Title: VIRUS instrument enclosures
Authors: Prochaska, T.; Allen, R.; Mondrik, N.; Rheault, J. P.;
Sauseda, M.; Boster, E.; James, M.; Rodriguez-Patino, M.; Torres, G.;
Ham, J.; Cook, E.; Baker, D.; DePoy, Darren L.; Marshall, Jennifer L.;
Hill, G. J.; Perry, D.; Savage, R. D.; Good, J. M.; Vattiat, Brian L.
2014SPIE.9147E..6UP Altcode:
The Visible Integral-Field Replicable Unit Spectrograph (VIRUS)
instrument will be installed at the Hobby-Eberly Telescope† in the
near future. The instrument will be housed in two enclosures that are
mounted adjacent to the telescope, via the VIRUS Support Structure
(VSS). We have designed the enclosures to support and protect the
instrument, to enable servicing of the instrument, and to cool the
instrument appropriately while not adversely affecting the dome
environment. The system uses simple HVAC air handling techniques in
conjunction with thermoelectric and standard glycol heat exchangers to
provide efficient heat removal. The enclosures also provide power and
data transfer to and from each VIRUS unit, liquid nitrogen cooling to
the detectors, and environmental monitoring of the instrument and dome
environments. In this paper, we describe the design and fabrication
of the VIRUS enclosures and their subsystems.

---------------------------------------------------------
Title: Coronal Magnetic Reconnection Driven by CME Expansion—the
2011 June 7 Event
Authors: van Driel-Gesztelyi, L.; Baker, D.; Török, T.; Pariat, E.;
Green, L. M.; Williams, D. R.; Carlyle, J.; Valori, G.; Démoulin,
P.; Kliem, B.; Long, D. M.; Matthews, S. A.; Malherbe, J. -M.
2014ApJ...788...85V Altcode: 2014arXiv1406.3153V
Coronal mass ejections (CMEs) erupt and expand in a magnetically
structured solar corona. Various indirect observational pieces of
evidence have shown that the magnetic field of CMEs reconnects with
surrounding magnetic fields, forming, e.g., dimming regions distant
from the CME source regions. Analyzing Solar Dynamics Observatory
(SDO) observations of the eruption from AR 11226 on 2011 June 7, we
present the first direct evidence of coronal magnetic reconnection
between the fields of two adjacent active regions during a CME. The
observations are presented jointly with a data-constrained numerical
simulation, demonstrating the formation/intensification of current
sheets along a hyperbolic flux tube at the interface between the CME
and the neighboring AR 11227. Reconnection resulted in the formation of
new magnetic connections between the erupting magnetic structure from
AR 11226 and the neighboring active region AR 11227 about 200 Mm from
the eruption site. The onset of reconnection first becomes apparent
in the SDO/AIA images when filament plasma, originally contained
within the erupting flux rope, is redirected toward remote areas in
AR 11227, tracing the change of large-scale magnetic connectivity. The
location of the coronal reconnection region becomes bright and directly
observable at SDO/AIA wavelengths, owing to the presence of down-flowing
cool, dense (1010 cm-3) filament plasma in its
vicinity. The high-density plasma around the reconnection region is
heated to coronal temperatures, presumably by slow-mode shocks and
Coulomb collisions. These results provide the first direct observational
evidence that CMEs reconnect with surrounding magnetic structures,
leading to a large-scale reconfiguration of the coronal magnetic field.

---------------------------------------------------------
Title: Spectroscopic measurements of EUV ejecta in a CME: a
high-blueshift trailing thread
Authors: Williams, David; Baker, Deborah; van Driel-Gesztelyi, Lidia;
Green, Lucie
2014IAUS..300..464W Altcode:
The mass of erupting prominence material can be inferred from the
obscuration of emission behind this mass of cool plasma thanks to
the rapid cadence of SDO/AIA images in the short EUV wavelength range
(Carlyle et al. 2013, these proceedings). In comparing this approach
with spectral observations from Hinode/EIS, to monitor contributions
from emission seen around the erupting prominence material, we have
found an intriguing component of blue-shifted emission, trailing
the erupting prominence, with Doppler shifts on the order of 350 km
s-1 in bright lines of both He ii and Fe xii.

---------------------------------------------------------
Title: FIP bias in a sigmoidal active region
Authors: Baker, D.; Brooks, D. H.; Démoulin, P.; van Driel-Gesztelyi,
Lidia; Green, L. M.; Steed, K.; Carlyle, J.
2014IAUS..300..222B Altcode:
We investigate first ionization potential (FIP) bias levels in
an anemone active region (AR) - coronal hole (CH) complex using an
abundance map derived from Hinode/EIS spectra. The detailed, spatially
resolved abundance map has a large field of view covering 359” ×
485”. Plasma with high FIP bias, or coronal abundances, is concentrated
at the footpoints of the AR loops whereas the surrounding CH has a low
FIP bias, ~1, i.e. photospheric abundances. A channel of low FIP bias
is located along the AR's main polarity inversion line containing a
filament where ongoing flux cancellation is observed, indicating a
bald patch magnetic topology characteristic of a sigmoid/flux rope
configuration.

---------------------------------------------------------
Title: Active region upflow plasma: its relation to small activity
and the solar wind
Authors: Mandrini, Cristina H.; Culhane, J. Leonard; Cristiani,
Germán; Vásquez, Alberto; Van Driel-Gesztelyi, Lidia; Baker, Deborah;
Pick, Monique; Demoulin, Pascal; Nuevo, Federico
2014cosp...40E1979M Altcode:
Recent studies show that active region (AR) upflowing plasma,
observed by the Hinode EUV Imaging Spectrometer (EIS), can gain
access to open field lines and be released into the solar wind via
magnetic interchange reconnection occurring below the source surface
at magnetic null-points in pseudo-streamer configurations. When only
one simple bipolar AR is present on the Sun and it is fully covered by
the separatrix of a streamer, like AR 10978 on December 2007, it seems
unlikely that the upflowing AR plasma could find its way into the slow
solar wind. However, signatures of plasma with AR composition at 1 AU
that appears to originate from the West of AR 10978 were recently found
by Culhane and coworkers. We present a detailed topology analysis of
AR 10978 based on a linear force-free magnetic field model at the AR
scale, combined with a global PFSS model. This allows us, on one hand,
to explain the variations observed in the upflows to the West of the
AR as the result of magnetic reconnection at quasi-separatrix layers
(QSLs). While at a global scale, we show that reconnection, occurring
in at least two main steps, first at QSLs and later at a high-altitude
coronal null-point, allows the AR plasma to get around the topological
obstacle of the streamer separatrix and be released into the solar wind.

---------------------------------------------------------
Title: Magnetic reconnection driven by filament eruption in the 7
June 2011 event
Authors: van Driel-Gesztelyi, L.; Baker, D.; Török, T.; Pariat, E.;
Green, L. M.; Williams, D. R.; Carlyle, J.; Valori, G.; Démoulin,
P.; Matthews, S. A.; Kliem, B.; Malherbe, J. -M.
2014IAUS..300..502V Altcode:
During an unusually massive filament eruption on 7 June 2011,
SDO/AIA imaged for the first time significant EUV emission around a
magnetic reconnection region in the solar corona. The reconnection
occurred between magnetic fields of the laterally expanding CME
and a neighbouring active region. A pre-existing quasi-separatrix
layer was activated in the process. This scenario is supported by
data-constrained numerical simulations of the eruption. Observations
show that dense cool filament plasma was re-directed and heated in
situ, producing coronal-temperature emission around the reconnection
region. These results provide the first direct observational evidence,
supported by MHD simulations and magnetic modelling, that a large-scale
re-configuration of the coronal magnetic field takes place during
solar eruptions via the process of magnetic reconnection.

---------------------------------------------------------
Title: Magnetic Polarity Streams and Subsurface Flows
Authors: Howe, R.; Baker, D.; Harra, L.; van Driel-Gesztelyi, L.;
Komm, R.; Hill, F.; González Hernández, I.
2013ASPC..478..291H Altcode:
An important feature of the solar cycle is the transport of unbalanced
magnetic flux from active regions towards the poles, which eventually
results in polarity reversal. This transport takes the form of distinct
“polarity streams” that are visible in the magnetic butterfly
diagram. We compare the poleward migration rate estimated from such
streams to that derived from the subsurface meridional flows measured
in helioseismic data from the GONG network since 2001, and find that
the results are in reasonable agreement.

---------------------------------------------------------
Title: Plasma Composition in a Sigmoidal Anemone Active Region
Authors: Baker, D.; Brooks, D. H.; Démoulin, P.; van Driel-Gesztelyi,
L.; Green, L. M.; Steed, K.; Carlyle, J.
2013ApJ...778...69B Altcode: 2013arXiv1310.0999B
Using spectra obtained by the EUV Imaging Spectrometer (EIS) instrument
onboard Hinode, we present a detailed spatially resolved abundance map
of an active region (AR)-coronal hole (CH) complex that covers an area
of 359” × 485”. The abundance map provides first ionization potential
(FIP) bias levels in various coronal structures within the large EIS
field of view. Overall, FIP bias in the small, relatively young AR
is 2-3. This modest FIP bias is a consequence of the age of the AR,
its weak heating, and its partial reconnection with the surrounding
CH. Plasma with a coronal composition is concentrated at AR loop
footpoints, close to where fractionation is believed to take place in
the chromosphere. In the AR, we found a moderate positive correlation
of FIP bias with nonthermal velocity and magnetic flux density, both
of which are also strongest at the AR loop footpoints. Pathways of
slightly enhanced FIP bias are traced along some of the loops connecting
opposite polarities within the AR. We interpret the traces of enhanced
FIP bias along these loops to be the beginning of fractionated plasma
mixing in the loops. Low FIP bias in a sigmoidal channel above the
AR's main polarity inversion line, where ongoing flux cancellation is
taking place, provides new evidence of a bald patch magnetic topology
of a sigmoid/flux rope configuration.

---------------------------------------------------------
Title: Revisiting the Distribution and Properties of Shatter Cones
at the Sudbury Impact Structure, Canada
Authors: Osinski, G. R.; Ferrière, L.; Kring, D. A.; Anders, D.;
Armstrong, K.; Baker, D.; Bamberg, M.; Beddingfield, C.; Gaither,
T.; Harrison, T.; Huber, M. S.; Hurwitz, D.; Jaret, S.; Kramer, G.;
Kuriyama, Y.; Lucas, M.; Marion, C. L.; Mercer, C.; Mount, C.; Neish,
C.; Nuhn, A.; Ostrach, L.; Pickersgill, A.; Pilles, E.; Potter,
R. W. K.; Ryan, A.; Sharp, M.; Swartz, N.; Thomson, O.; Veto, M.;
Wielicki, M. M.; Wright, S.; Zanetti, M.
2013LPICo1737.3061O Altcode:
Here, we present the first results of a new multi-year research program
that aims to systematically map the distribution of shatter cones and
their physical properties around the Sudbury structure.

---------------------------------------------------------
Title: 76 T dwarfs from the UKIDSS LAS: benchmarks, kinematics and
an updated space density
Authors: Burningham, Ben; Cardoso, C. V.; Smith, L.; Leggett,
S. K.; Smart, R. L.; Mann, A. W.; Dhital, S.; Lucas, P. W.; Tinney,
C. G.; Pinfield, D. J.; Zhang, Z.; Morley, C.; Saumon, D.; Aller,
K.; Littlefair, S. P.; Homeier, D.; Lodieu, N.; Deacon, N.; Marley,
M. S.; van Spaandonk, L.; Baker, D.; Allard, F.; Andrei, A. H.; Canty,
J.; Clarke, J.; Day-Jones, A. C.; Dupuy, T.; Fortney, J. J.; Gomes,
J.; Ishii, M.; Jones, H. R. A.; Liu, M.; Magazzú, A.; Marocco, F.;
Murray, D. N.; Rojas-Ayala, B.; Tamura, M.
2013MNRAS.433..457B Altcode: 2013arXiv1304.7246B; 2013MNRAS.tmp.1507B
We report the discovery of 76 new T dwarfs from the UKIRT Infrared
Deep Sky Survey (UKIDSS) Large Area Survey (LAS). Near-infrared broad-
and narrow-band photometry and spectroscopy are presented for the
new objects, along with Wide-field Infrared Survey Explorer (WISE)
and warm-Spitzer photometry. Proper motions for 128 UKIDSS T dwarfs
are presented from a new two epoch LAS proper motion catalogue. We
use these motions to identify two new benchmark systems: LHS 6176AB,
a T8p+M4 pair and HD 118865AB, a T5.5+F8 pair. Using age constraints
from the primaries and evolutionary models to constrain the radii,
we have estimated their physical properties from their bolometric
luminosity. We compare the colours and properties of known benchmark
T dwarfs to the latest model atmospheres and draw two principal
conclusions. First, it appears that the H - [4.5] and J - W2 colours
are more sensitive to metallicity than has previously been recognized,
such that differences in metallicity may dominate over differences in
Teff when considering relative properties of cool objects
using these colours. Secondly, the previously noted apparent dominance
of young objects in the late-T dwarf sample is no longer apparent when
using the new model grids and the expanded sample of late-T dwarfs and
benchmarks. This is supported by the apparently similar distribution
of late-T dwarfs and earlier type T dwarfs on reduced proper motion
diagrams that we present. Finally, we present updated space densities
for the late-T dwarfs, and compare our values to simulation predictions
and those from WISE.

---------------------------------------------------------
Title: Are subsurface flows and coronal holes related?
Authors: Komm, R.; Howe, R.; González Hernández, I.; Harra, L.;
Baker, D.; van Driel-Gesztelyi, L.
2013JPhCS.440a2022K Altcode:
We study synoptic maps of solar subsurface flows covering six Carrington
rotations (2050 to 2055). The subsurface flows are determined with
a ring-diagram analysis of GONG high-resolution Doppler data. We
identify the locations of coronal holes in synoptic maps of EUV images
at 195Å from the EIT instrument and determine the characteristics
of associated subsurface flows. We study two long-lived coronal holes
that are present during this epoch. We find that large-scale patterns
are present in the subsurface flows but appear to be unrelated to
these coronal holes. The horizontal subsurface flows associated with
the two long-lived coronal holes are weakly divergent (upflows) with
small cyclonic vorticity. These flows are thus similar to subsurface
flows of quiet regions with regard to the vertical flows and similar
to flows of active regions with regard to vorticity.

---------------------------------------------------------
Title: Can we detect local helioseismic parameter shifts in coronal
holes?
Authors: Howe, R.; Haber, D. A.; Bogart, R. S.; Zharkov, S.; Baker,
D.; Harra, L.; van Driel-Gesztelyi, L.
2013JPhCS.440a2019H Altcode:
Changes in helioseismic mode parameters in active regions and across
the solar disk are well documented, but local magnetic activity
and geometric effects may not account for all of the scatter seen
in the results. We use results from the Helioseismic and Magnetic
Imager ring-diagram pipeline for Carrington rotation 2113 to look for
differences in mode amplitude and frequency between coronal holes and
other quiet-Sun regions. While we do not find a systematic difference,
the results do suggest that the correlation between magnetic activity
index and mode parameters shows less scatter in coronal hole regions
than in general quiet Sun.

---------------------------------------------------------
Title: Subsurface flows associated with non-Joy oriented active
regions: a case study
Authors: González Hernández, Irene; Komm, Rudolf; van
Driel-Gesztelyi, Lidia; Baker, Deborah; Harra, Louise; Howe, Rachel
2013JPhCS.440a2050G Altcode:
Non-Joy oriented active regions (ARs) are a challenge for solar magnetic
field modelers. Although significant deviations from Joy's law are
relatively rare for simple bipolar ARs, understanding the causes of
their particularity could be critical for the big picture of the solar
dynamo. We explore the possibility of the sub-surface local dynamics
being responsible for the significant rotation of these ARs. We apply
the ring-diagram technique, a local helioseismology method, to infer
the flows under and surrounding a non-Joy oriented AR and present the
results of a case study in this paper.

---------------------------------------------------------
Title: The 3D Geometry of Active Region Upflows Deduced from Their
Limb-to-Limb Evolution
Authors: Démoulin, P.; Baker, D.; Mandrini, C. H.; van
Driel-Gesztelyi, L.
2013SoPh..283..341D Altcode: 2012arXiv1211.5962D
We analyze the evolution of coronal plasma upflows from the edges of
AR 10978, which has the best limb-to-limb data coverage with Hinode's
EUV Imaging Spectrometer (EIS). We find that the observed evolution is
largely due to the solar rotation progressively changing the viewpoint
of nearly stationary flows. From the systematic changes in the upflow
regions as a function of distance from disc center, we deduce their
3D geometrical properties as inclination and angular spread in three
coronal lines (Si VII, Fe XII, and Fe XV). In agreement with magnetic
extrapolations, we find that the flows are thin, fan-like structures
rooted in quasi separatrix layers (QSLs). The fans are tilted away
from the AR center. The highest plasma velocities in these three
spectral lines have similar magnitudes and their heights increase with
temperature. The spatial location and extent of the upflow regions
in the Si VII, Fe XII, and Fe XV lines are different owing to i)
temperature stratification and ii) line of sight integration of the
spectral profiles with significantly different backgrounds. We conclude
that we sample the same flows at different temperatures. Further,
we find that the evolution of line widths during the disc passage is
compatible with a broad range of velocities in the flows. Everything
considered, our results are compatible with the AR upflows originating
from reconnections along QSLs between over-pressure AR loops and
neighboring under-pressure loops. The flows are driven along magnetic
field lines by a pressure gradient in a stratified atmosphere. Our
interpretation of the above results is that, at any given time, we
observe the superposition of flows created by successive reconnections,
leading to a broad velocity distribution.

---------------------------------------------------------
Title: Mass Estimates of Rapidly Moving Prominence Material from
High-cadence EUV Images
Authors: Williams, David R.; Baker, Deborah; van Driel-Gesztelyi, Lidia
2013ApJ...764..165W Altcode: 2013arXiv1301.4271W
We present a new method for determining the column density of erupting
filament material using state-of-the-art multi-wavelength imaging
data. Much of the prior work on filament/prominence structure can
be divided between studies that use a polychromatic approach with
targeted campaign observations and those that use synoptic observations,
frequently in only one or two wavelengths. The superior time resolution,
sensitivity, and near-synchronicity of data from the Solar Dynamics
Observatory's Advanced Imaging Assembly allow us to combine these
two techniques using photoionization continuum opacity to determine
the spatial distribution of hydrogen in filament material. We apply
the combined techniques to SDO/AIA observations of a filament that
erupted during the spectacular coronal mass ejection on 2011 June 7. The
resulting "polychromatic opacity imaging" method offers a powerful way
to track partially ionized gas as it erupts through the solar atmosphere
on a regular basis, without the need for coordinated observations,
thereby readily offering regular, realistic mass-distribution estimates
for models of these erupting structures.

---------------------------------------------------------
Title: Plasma outflows at the border of active regions and the
solar wind
Authors: Nuevo, F. A.; Mandrini, C. H.; Vásquez, A. M.; Deumoulin,
P.; Van Driel-Gesztely, L.; Baker, D.; Cristiani, G. D.; Pick, M.;
Culhane, J. L.
2013BAAA...56..387N Altcode:
We present a detailed topological analysis of active region (AR)
10978; based on a Potential Field Source Surface (PFSS) model. AR
10978 is a standard bipolar region which appears fully covered by
the magnetic field lines of a coronal streamer. Despite this simple
magnetic configuration; our analysis shows that it is possible for
the AR plasma; contained in the outflows observed at the AR borders;
to be released into the solar wind via magnetic reconnection.

---------------------------------------------------------
Title: Magnetic Topology of Active Regions and Coronal Holes:
Implications for Coronal Outflows and the Solar Wind
Authors: van Driel-Gesztelyi, L.; Culhane, J. L.; Baker, D.; Démoulin,
P.; Mandrini, C. H.; DeRosa, M. L.; Rouillard, A. P.; Opitz, A.;
Stenborg, G.; Vourlidas, A.; Brooks, D. H.
2012SoPh..281..237V Altcode: 2012SoPh..tmp..228V
During 2 - 18 January 2008 a pair of low-latitude opposite-polarity
coronal holes (CHs) were observed on the Sun with two active regions
(ARs) and the heliospheric plasma sheet located between them. We use
the Hinode/EUV Imaging Spectrometer (EIS) to locate AR-related outflows
and measure their velocities. Solar-Terrestrial Relations Observatory
(STEREO) imaging is also employed, as are the Advanced Composition
Explorer (ACE) in-situ observations, to assess the resulting impacts on
the solar wind (SW) properties. Magnetic-field extrapolations of the two
ARs confirm that AR plasma outflows observed with EIS are co-spatial
with quasi-separatrix layer locations, including the separatrix of a
null point. Global potential-field source-surface modeling indicates
that field lines in the vicinity of the null point extend up to the
source surface, enabling a part of the EIS plasma upflows access
to the SW. We find that similar upflow properties are also observed
within closed-field regions that do not reach the source surface. We
conclude that some of plasma upflows observed with EIS remain confined
along closed coronal loops, but that a fraction of the plasma may be
released into the slow SW. This suggests that ARs bordering coronal
holes can contribute to the slow SW. Analyzing the in-situ data, we
propose that the type of slow SW present depends on whether the AR is
fully or partially enclosed by an overlying streamer.

---------------------------------------------------------
Title: Identifying the Main Driver of Active Region Outflows
Authors: Baker, D.; van Driel-Gesztelyi, L.; Mandrini, C. H.;
Démoulin, P.; Murray, M. J.
2012ASPC..454..425B Altcode:
Hinode's EUV Imaging Spectrometer (EIS) has discovered ubiquitous
outflows of a few to 50 km s-1 from active regions (ARs). The
characteristics of these outflows are very curious in that they are
most prominent at the AR boundary and appear over monopolar magnetic
areas. They are linked to strong non-thermal line broadening and
are stronger in hotter EUV lines. The outflows persist for at least
several days. Whereas red-shifted down flows observed in AR closed
loops are well understood, to date there is no general consensus
for the mechanism(s) driving blue-shifted AR-related outflows. We
use Hinode EIS and X-Ray Telescope observations of AR 10942 coupled
with magnetic modeling to demonstrate for the first time that the
outflows originate from specific locations of the magnetic topology
where field lines display strong gradients of magnetic connectivity,
namely quasi-separatrix layers (QSLs), or in the limit of infinitely
thin QSLs, separatrices. The strongest AR outflows were found to be
in the vicinity of QSL sections located over areas of strong magnetic
field. We argue that magnetic reconnection at QSLs, separating closed
field lines of the AR and either large-scale externally connected or
‘open’ field lines, is a viable mechanism for driving AR outflows
which are potentially sources of the slow solar wind. In fact, magnetic
reconnection along QSLs (including separatricies) is the first theory
to explain the most puzzling characteristics of the outflows, namely
their occurrence over monopolar areas at the periphery of ARs and
their longevity.

---------------------------------------------------------
Title: Sunspot Light-Bridges - A Bridge Between the Photosphere and
the Corona?
Authors: Matthews, S.; Baker, D.; Domínguez, S. V.
2012ASPC..454..209M Altcode: 2010arXiv1004.3879M
Recent observations of sunspot light-bridges (LBs) have shed new
light on the fact that they are often associated with significant
chromospheric activity. In particular chromospheric jets (Shimizu
et al. 2009) persisting over a period of days have been identified,
sometimes associated with large downflows at the photospheric level
(Louis et al. 2009). One possible explanation for this activity is
reconnection low in the atmosphere. LBs have also been associated with
a constant brightness enhancement in the 1600 Å passband of TRACE,
and the heating of 1 MK loops. Using data from EIS, SOT and STEREO
EUVI we investigate the response of the transition region and lower
corona to the presence of a LB.

---------------------------------------------------------
Title: Magnetic topology, coronal outflows, and the solar wind
Authors: Mandrini, Cristina H.; Culhane, J. Leonard; Vourlidas,
Angelos; Demoulin, Pascal; Stenborg, Guillermo; Opitz, Andrea;
Rouillard, Alexis; Van Driel-Gesztelyi, Lidia; Baker, Deborah; DeRosa,
Marc; Brooks, David
2012cosp...39.1173M Altcode: 2012cosp.meet.1173M
During 2-18 January 2008 a pair of low-latitude opposite polarity
coronal holes were observed on the Sun flanked by two ARs with
the heliospheric plasma sheet between them. Hinode/EUV Imaging
Telescope (EIS) is used to locate AR-related outflows and measure their
velocities. The Advanced Composition Explorer (ACE) in-situ observations
are employed to assess the resulting impacts on the interplanetary solar
wind (SW). Magnetic field extrapolations of the two ARs confirm that AR
plasma outflows observed with EIS are co-spatial with quasi-separatrix
layer locations, including the separatrix of a null point. Global
potential field source-surface modeling indicates that field lines
in the vicinity of the null point extend up to the source-surface,
enabling a part of the EIS plasma upflows access to the SW. Similar
upflow magnitude is also observed within closed field regions. Though
part of the plasma upflows observed with EIS remain confined along
closed coronal loops, a subset of them are indeed able to make their
imprint in the slow SW, making ARs bordering coronal holes a slow
SW contributor.

---------------------------------------------------------
Title: Are subsurface flows and coronal holes related?
Authors: Komm, Rudolf W.; Howe, R.; González Hernández, I.; Harra,
L.; Baker, D.; van Driel-Gesztelyi, L.
2012shin.confE.120K Altcode:
We study subsurface flows measured with a ring-diagram analysis of GONG
high-resolution Doppler data. In previous studies, we have focused on
the relationship between active regions and subsurface flows associated
with them. Synoptic subsurface flow maps show also large-scale patterns
that are not obviously associated with active regions. It is unknown
whether these flow patterns correlate with any large-scale magnetic
features. Here, we explore whether there is a relationship between
subsurface flows and coronal features. We analyze synoptic maps of
subsurface flows covering 18 Carrington rotations during the years
2006 and 2007 (CR 2038-2055). Long-lived coronal holes are present
during this epoch at low latitudes, which are accessible by ring-diagram
analysis of GONG data. We compare subsurface flow maps with EIT synoptic
maps of EUV images at 195A (http://sun.stanford.edu/synop/EIT/) and
will present the latest results.

---------------------------------------------------------
Title: Nonlinear Force-Free Extrapolation of Emerging Flux with a
Global Twist and Serpentine Fine Structures
Authors: Valori, G.; Green, L. M.; Démoulin, P.; Vargas Domínguez,
S.; van Driel-Gesztelyi, L.; Wallace, A.; Baker, D.; Fuhrmann, M.
2012SoPh..278...73V Altcode:
We study the flux emergence process in NOAA active region 11024, between
29 June and 7 July 2009, by means of multi-wavelength observations
and nonlinear force-free extrapolation. The main aim is to extend
previous investigations by combining, as much as possible, high spatial
resolution observations to test our present understanding of small-scale
(undulatory) flux emergence, whilst putting these small-scale events
in the context of the global evolution of the active region. The
combination of these techniques allows us to follow the whole process,
from the first appearance of the bipolar axial field on the east limb,
until the buoyancy instability could set in and raise the main body
of the twisted flux tube through the photosphere, forming magnetic
tongues and signatures of serpentine field, until the simplification
of the magnetic structure into a main bipole by the time the active
region reaches the west limb. At the crucial time of the main emergence
phase high spatial resolution spectropolarimetric measurements of the
photospheric field are employed to reconstruct the three-dimensional
structure of the nonlinear force-free coronal field, which is then
used to test the current understanding of flux emergence processes. In
particular, knowledge of the coronal connectivity confirms the identity
of the magnetic tongues as seen in their photospheric signatures,
and it exemplifies how the twisted flux, which is emerging on small
scales in the form of a sea-serpent, is subsequently rearranged by
reconnection into the large-scale field of the active region. In
this way, the multi-wavelength observations combined with a nonlinear
force-free extrapolation provide a coherent picture of the emergence
process of small-scale magnetic bipoles, which subsequently reconnect
to form a large-scale structure in the corona.

---------------------------------------------------------
Title: Forecasting a CME by Spectroscopic Precursor?
Authors: Baker, D.; van Driel-Gesztelyi, L.; Green, L. M.
2012SoPh..276..219B Altcode:
Multi-temperature plasma flows resulting from the interaction between
a mature active region (AR) inside an equatorial coronal hole (CH) are
investigated. Outflow velocities observed by Hinode EIS ranged from a
few to 13 km s−1 for three days at the AR's eastern and
western edges. However, on the fourth day, velocities intensified up to
20 km s−1 at the AR's western footpoint about six hours
prior to a CME. 3D MHD numerical simulations of the observed magnetic
configuration of the AR-CH complex showed that the expansion of the
mature AR's loops drives persistent outflows along the neighboring CH
field (Murray et al. in Solar Phys.261, 253, 2010). Based on these
simulations, intensification of outflows observed pre-eruption on
the AR's western side where same-polarity AR and CH field interface,
is interpreted to be the result of the expansion of a sigmoidal
AR, in particular, a flux rope containing a filament that provides
stronger compression of the neighboring CH field on this side of the
AR. Intensification of outflows in the AR is proposed as a new type
of CME precursor.

---------------------------------------------------------
Title: The Research Experience for Undergraduates Program in Solar
and Space Physics at the University of Colorado
Authors: Snow, M.; Wood, E.; Cobabe-Amman, E.; Baker, D.; Renfrow, S.
2011ASPC..443..332S Altcode:
The Research Experience for Undergraduates (REU) program in Solar
and Space Physics is a collaboration between the University of
Colorado's Laboratory for Atmospheric and Space Physics (LASP), the
National Center for Atmospheric Research's High Altitude Observatory
(HAO), the National Oceanic and Atmospheric Administration's Space
Weather Prediction Center (SWPC), the Southwest Research Institute
(SwRI), and Northwest Research Associates' Colorado Research Associates
(CoRA). The goal of the program is to give students real-world, hands-on
experience doing research with scientist mentors and to further their
intended careers. Our program began in 2007 and is entering its
fourth year. Mentors from the member institutions have supervised over
fifty research projects dealing with all aspects of Solar and Space
Physics. The students begin their eight-week visit to Boulder with a
week of classes on the Sun-Earth system as well as practical courses
on data analysis and the IDL programming language. The students give a
30 minute oral presentation of their project as well as a poster in a
student symposium at the end of the program. Throughout the summer, the
students give progress reports at weekly brown-bag lunch meetings. In
addition to their own research projects at their host institution, the
students tour and meet scientists from the partner institutions as the
weekly lunches rotate from site to site. There are also opportunities
for students to network with scientists in an informal way at the
excursions we organize which include barbecues and weekend outings.

---------------------------------------------------------
Title: The discovery of the T8.5 dwarf UGPS J0521+3640
Authors: Burningham, Ben; Lucas, P. W.; Leggett, S. K.; Smart, R.;
Baker, D.; Pinfield, D. J.; Tinney, C. G.; Homeier, D.; Allard, F.;
Zhang, Z. H.; Gomes, J.; Day-Jones, A. C.; Jones, H. R. A.; Kovács,
G.; Lodieu, N.; Marocco, F.; Murray, D. N.; Sipőcz, B.
2011MNRAS.414L..90B Altcode: 2011arXiv1104.1526B
We have carried out a search for late-type T dwarfs in the UKIRT
Infrared Deep Sky Survey Galactic Plane Survey 6th Data Release. The
search yielded two persuasive candidates, both of which have been
confirmed as T dwarfs. The brightest, UGPS J0521+3640, has been
assigned the spectral type T8.5 and appears to lie at a distance of
7-9 pc. The fainter of the two, UGPS J0652+0324, is classified as a
T5.5 dwarf and lies at an estimated distance of 28-37 pc. Warm-Spitzer
observations in IRAC channels 1 and 2, taken as part of the GLIMPSE360
Legacy Survey, are available for UGPS J0521+3640 and we used these data
with the near-infrared spectroscopy to estimate its properties. We find
best-fitting solar metallicity BT-Settl models for Teff=
600 and 650 K and log g= 4.5 and 5.0. These parameters suggest a mass
between 14 and 32MJ for an age between 1 and 5 Gyr. The
proximity of this very cool T dwarf, and its location in the Galactic
plane, makes it an ideal candidate for high-resolution adaptive optics
imaging to search for cool companions.

---------------------------------------------------------
Title: GRB 110112A: WHT candidate afterglow/host galaxy.
Authors: Levan, A. J.; Tanvir, N. R.; Baker, D.
2011GCN.11559....1L Altcode: 2011GCN..11559...1L
No abstract at ADS

---------------------------------------------------------
Title: Drivers of solar coronal dynamics
Authors: Baker, Deborah
2011PhDT.......380B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Using MHD modeling to specify inner heliosphere conditions
during the three MESSENGER Mercury flybys
Authors: Farr, N. L.; Baker, D.; Odstrcil, D.; Anderson, B. J.; Benna,
M.; Gloeckler, G.; Korth, H.; Mayer, L. R.; Raines, J. M.; Schriver,
D.; Slavin, J. A.; Solomon, S. C.; Travnicek, P. M.; Zurbuchen, T.
2010AGUFMSH42A..06F Altcode:
The three successful flybys of Mercury by the MESSENGER spacecraft
occurred, respectively, on 14 January 2008, 6 October 2008, and 29
September 2009. In order to provide contextual information about the
solar wind properties and the interplanetary magnetic field (IMF)
near the planet at those times, we have used an empirical modeling
technique combined with a numerical physics-based solar wind model. The
Wang-Sheeley-Arge (WSA) method uses solar photospheric magnetic field
observations (from Earth-based instruments) in order to estimate the
inner heliospheric radial flow speed and radial magnetic field out to
21.5 solar radii from the Sun. This information is then used as input to
the global numerical magnetohydrodynamic model, ENLIL, which calculates
solar wind velocity, density, temperature, and magnetic field strength
and polarity throughout the inner heliosphere. WSA-ENLIL calculations
are presented for the several-week period encompassing each of the
flybys. This information in conjunction with available MESSENGER
data aid in understanding the Mercury flyby observations and provide
a basis for subsequent global magnetospheric modeling. We find that
during all three flybys the solar wind conditions were quiescent and
would have provided only modest dynamic driving forces for Mercury’s
magnetospheric system. We present data-model comparisons for ACE,
STEREO-A and -B, and MESSENGER for all of these cases.

---------------------------------------------------------
Title: Extreme Solar System in the Undergraduate Classroom
Authors: Baker, D.
2010AGUFMED23A0699B Altcode:
One of the greatest challenges for science educators today is to
engage non-science students in the scientific process - to help them
realize that science is cool, interesting, and fun. With NASA’s Year
of the Solar System beginning in October 2010, a course that explores
some of the most extreme places in our Solar System may be just the
hook needed to improve attitudes toward science. We use three unique
inquiry-based approaches in a freshman-level introductory science course
to engage non-science students: 1) Emphasis on “extreme” phenomena
in our Solar System, 2) Research papers and oral presentations in which
“extreme experts” (students) try to convince a mock NASA panel where
the next planetary mission should be, and 3) Science Portfolios in which
students ask their own scientific questions, design their own scientific
experiments, and evaluate their own scientific growth. The effectiveness
of these approaches (as determined from pre-/post- surveys, focus
groups, and other instruments) will be presented. Preliminary results
show that students become less intimidated by science and feel that
science has become more important in their everyday lives.

---------------------------------------------------------
Title: Cratering on Mercury: Insights from the MESSENGER Flybys
Authors: Chapman, C. R.; Strom, R. G.; Fassett, C. I.; Prockter, L. M.;
Head, J. W.; Solomon, S. C.; Banks, M. E.; Baker, D.; Merline, W. J.
2010M&PSA..73.5325C Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Outflows at the Edges of an Active Region in a Coronal Hole:
A Signature of Active Region Expansion?
Authors: Murray, M. J.; Baker, D.; van Driel-Gesztelyi, L.; Sun, J.
2010SoPh..261..253M Altcode: 2009arXiv0912.1246M
Outflows of plasma at the edges of active regions surrounded by quiet
Sun are now a common observation with the Hinode satellite. While there
is observational evidence to suggest that the outflows are originating
in the magnetic field surrounding the active regions, there is no
conclusive evidence that reveals how they are driven. Motivated
by observations of outflows at the periphery of a mature active
region embedded in a coronal hole, we have used a three-dimensional
simulation to emulate the active region's development in order to
investigate the origin and driver of these outflows. We find that
outflows are accelerated from a site in the coronal hole magnetic
field immediately surrounding the active region and are channelled
along the coronal hole field as they rise through the atmosphere. The
plasma is accelerated simply as a result of the active region
expanding horizontally as it develops. Many of the characteristics
of the outflows generated in the simulation are consistent with
those of observed outflows: velocities up to 45 km s−1,
properties akin to the coronal hole, proximity to the active region's
draining loops, expansion with height, and projection over monopolar
photospheric magnetic concentrations. Although the horizontal expansion
occurs as a consequence of the active region's development in the
simulation, expansion is also a general feature of established active
regions. Hence, it is entirely possible and plausible that the expansion
acceleration mechanism displayed in the simulation is occurring in
active regions on the Sun and, in addition to reconnection, is driving
the outflows observed at their edges.

---------------------------------------------------------
Title: Magnetic reconnection along QSLs -a major driver of active
region outflows
Authors: Baker, Deborah; van Driel-Gesztelyi, Lidia; Mandrini,
Cristina H.; Demoulin, Pascal
2010cosp...38.2926B Altcode: 2010cosp.meet.2926B
The relationship between quasi-separatrix layers (QSLs), or in the limit
of infinitely thin QSLs, separatrices, and various activity phenomena
has been explored in many different solar magnetic configurations
across all scales in recent years. In the absence of magnetic nulls,
fast reconnec-tion along QSLs, which are specific locations in the
magnetic topology where field lines display strong gradients of
magnetic connectivity, was identified as the main physical process
at the origin of flares. Recently, it was shown that fast (tens of
km/s) persistent hot plasma upflows in active regions (ARs) can also
be linked to locations of QSLs. It is likely that these upflows that
occur at the edges of ARs over unipolar magnetic field concentrations
are accelerated by magnetic reconnection along QSLs. We will show
multi-temperature spectral scan observations from Hinode's EIS combined
with magnetic modeling of QSLs in two ARs observed on 20-21 February
2007 and 11 January 2008. The latter AR is observed and modeled when
it is in the vicinity of the solar central meridian where there are no
projection effects, thereby eliminating ambiguity linking the origin
of multi-temperature observations of AR upflows to QSLs. We use the
Potential Source Surface Model to look for open field lines in the
vicinity of upflows and QSL locations in order to demonstrate whether
these upflows become outflows and can contribute to the solar wind.

---------------------------------------------------------
Title: Interacting active regions and coronal holes: implications
for coronal outflows and solar wind structure
Authors: Culhane, J. Leonard; Baker, Deborah; Rouillard, Alexis;
van Driel-Gesztelyi, Lidia
2010cosp...38.1863C Altcode: 2010cosp.meet.1863C
When active regions are adjacent to coronal holes a variety of magnetic
field interactions can result. These may include the interchange
reconnection between the closed active region (AR) fields and the
open field of the coronal hole (CH), leading to fast and significant
evolution of coronal hole boundaries. Outcomes may include variability
of -or changes in, active region-associated hot plasma outflows seen
with Hinode/EIS and the modulation of the solar wind flows on open
field lines. Depending on their relative positions on the Sun, the
AR-CH interactions may have their signatures embedded in co-rotating
interaction regions (CIRs) or rarefaction regions. During two intervals
-8/11 January, 2008 and 7/9 December, 2008, we have made observations
with Hinode of two oppositely configured situations on the Sun. For
8/11 January, the coronal hole leads the active region while for
7/9 December the order is reversed. The Hinode EIS instrument is
used to locate outflows and measure their velocities while the XRT
is used to image the source regions, including the variable nature
of the outflows. SOHO EIT imaging is used to follow the longer-term
evolution of the coronal hole boundaries while MDI is used to observe
changes in the magnetic field. STEREO imaging and in-situ data are also
employed -as are ACE observations, to assess the resulting impacts on
interplanetary solar wind structures. The contrasting behaviour that
results from magnetic interactions in the two different configurations
is described and assessed.

---------------------------------------------------------
Title: Intensification of Plasma Upflows in an Active Region---Coronal
Hole Complex: A CME Precursor
Authors: Baker, D.; van Driel-Gesztelyi, L.; Murray, M. J.; Green,
L. M.; Török, T.; Sun, J.
2009ASPC..415...75B Altcode:
We investigate the plasma flows resulting from the interaction between
a mature active region (AR) and a surrounding equatorial coronal hole
(CH) observed by Hinode's EIS and XRT from 15 to 18 October 2007. For 3
days, EIS velocity maps showed upflows at the AR's eastern and western
edges that were consistently between 5 and 10 km s-1, whereas
downflows of up to 30 km s-1 were seen in AR loops. However,
on 18 October, velocity profiles of hotter coronal lines revealed
intensification in upflow velocities of up to 18 km s-1
at the AR's western footpoints 4.5 hours prior to a CME. We compare
the AR's plasma flows with 2.5D MHD numerical simulations of the
magnetic configuration, which show that expansion of the mature AR's
loops drives upflows along the neighboring CH field. Further, the
intensification of upflows observed on the AR's western side prior to
a CME is interpreted to be the result of the expansion of a flux rope
containing a filament further compressing the neighboring CH field.

---------------------------------------------------------
Title: Particle Transport and Acceleration in Mercury’s
Magnetosphere during the MESSENGER Flybys
Authors: Schriver, D.; Travnicek, P. M.; Paral, J.; Slavin, J. A.;
Sarantos, M.; Anderson, B. J.; Korth, H.; Zurbuchen, T.; Baker, D.;
Benna, M.; Killen, R. M.; McClintock, W. E.; Ho, G. C.; Krimigis,
S. M.; McNutt, R. L.; Solomon, S. C.
2009AGUFM.P24A..07S Altcode:
The first two MESSENGER flybys on 14 January 2008 and 6 October 2008
encountered very different solar wind interplanetary magnetic field
(IMF) conditions. During the first flyby the IMF was northward, while
during the second it was southward; in addition, during both flybys
the IMF had a large radial (planetward) component. As is well known at
the Earth, the orientation of the IMF strongly influences the structure
and dynamics of the planetary magnetosphere, and this in turn strongly
affects how particles are transported and accelerated as they move
through the magnetosphere. To examine the transport, distribution,
and energization of plasma (including heavy ions) for the solar
wind conditions during the MESSENGER flybys, three-dimensional global
hybrid simulations of Mercury’s magnetosphere are used to provide the
electric and magnetic field configuration at the time of the flybys,
and particle trajectories are then traced through the magnetospheric
system. Because electrons are included as a massless fluid in the
hybrid simulations, electron transport is also examined using this
technique. In particular, these calculations permit an examination of
acceleration near reconnection regions, as well as the formation and
dynamics of the quasi-stable particle ring around Mercury and sputtering
as a source of the planet’s exosphere. Simulation results provide
a basis for comparison with MESSENGER data from the first two flybys,
as well as from the third flyby on 29 September 2009.

---------------------------------------------------------
Title: MHD modeling of the interaction of the magnetosphere of
Mercury with the solar wind during the MESSENGER flybys
Authors: Benna, M.; Anderson, B. J.; Baker, D.; Boardsen, S. A.;
Killen, R. M.; Korth, H.; Krimigis, S. M.; Purucker, M. E.; McNutt,
R. L.; Raines, J. M.; McClintock, W. E.; Sarantos, M.; Slavin, J. A.;
Solomon, S. C.; Schriver, D.; Travnicek, P.; Zurbuchen, T.
2009AGUFM.P24A..08B Altcode:
The MESSENGER spacecraft flybys of Mercury on 14 January 2008 and 6
October 2008 provided a special opportunity to study the magnetosphere
of the innermost planet under different solar wind and interplanetary
magnetic field conditions. The model presented in this paper is based on
the solution of the three-dimensional, multi-fluid magnetohydrodynamic
(MHD) equations for solar wind protons and electrons in the absence
of mass loading. In this study we provide new estimates of Mercury’s
intrinsic magnetic field and the solar wind conditions that prevailed
at the time of these two flybys. We show that the location of the
boundary layers and the strength of the magnetic field along the
spacecraft trajectory are consistent with a planetary magnetic dipole
having a magnitude of 210 RM3 nT and an offset of 0.18 RM to the north
of the equator, where RM is Mercury’s radius. A comparison between
the magnetospheric structures generated under northward and southward
interplanetary magnetic field (IMF) orientations confirms that dayside
and nightside reconnections are efficient drivers of energy transfer
between the solar wind and the magnetosphere. Analysis of the plasma
flow reveals the existence of a stable drift belt around the planet;
such a belt can account for the locations of diamagnetic decreases
observed during both flybys by the MESSENGER Magnetometer. Moreover,
we deduce that the variability in the ion impact rate at the cusps
as a result of the very different magnetosphere configurations can
provide a possible explanation for the variability in the north-south
asymmetry of exospheric sodium observed in Mercury’s neutral tail.

---------------------------------------------------------
Title: MESSENGER X-Ray Spectrometer and Energetic Particle
Spectrometer Observations of Energetic Electrons during the Mercury
Flybys
Authors: Starr, R. D.; Ho, G. C.; Anderson, B. J.; Andrews, G. B.;
Baker, D.; Gold, R. E.; Krimigis, S. M.; McNutt, R. L.; Nittler, L.;
Rhodes, E. A.; Schlemm, C. E.; Slavin, J. A.; Solomon, S. C.
2009AGUFM.P21A1195S Altcode:
The X-Ray Spectrometer (XRS) onboard the MESSENGER spacecraft will
determine elemental abundances on the surface of Mercury by measuring
fluorescent X-ray emissions induced on the planet’s surface by the
incident solar X-ray flux. The most prominent fluorescent lines are
the Kα lines from the elements Mg, Al, Si, S, Ca, Ti, and Fe (1-10
keV). The Energetic Particle Spectrometer (EPS) observes both ions and
electrons (&gt;35 keV) accelerated in Mercury’s magnetosphere. EPS
measurements will help characterize magnetospheric-particle
contributions to Mercury’s magnetic field, as well as characterize
energy conversion processes in the vicinity of, and within, the
magnetosphere. Prior to entering orbit about Mercury in March 2011,
MESSENGER has flown by the planet three times for spacecraft-trajectory
gravity assists and scientific observations. Solar X-ray emissions
during the flybys have been an order of magnitude lower than expected,
and no X-ray signal has been detected from the planet. Nevertheless, the
XRS has measured several count-rate spikes before (by ~5 minutes) and
after (~7 minutes) closest approach whose signatures clearly identify
their origin as electrons (~10-30 keV) interacting in the XRS detector
material. Electron-induced fluorescence and bremsstrahlung are evident
in the XRS gas proportional counters. Measured spectra are well modeled
by kappa function electron distributions impinging on the XRS Mg and Al
filters, Be windows, and Be-Cu collimator. However, no corresponding
signal is observed by the EPS for these events. Modeling of at least
one of these events suggests sufficient electron flux above 35 keV
to be detectable by EPS. A possible scenario is that the XRS detected
highly anisotropic and short-duration electron bursts that were not in
the EPS field-of-view, implying an exceptionally narrow pitch angle
distribution. The energetic electron observations made by the EPS
and XRS provide a basis for assessing the electron distributions at
Mercury during MESSENGER flybys.

---------------------------------------------------------
Title: Determining Mean Electron Temperature Variation Along Magnetic
Field Lines in the Earth's Plasma-sheet Using Multipoint Measurements
From Cluster
Authors: Presicci, M. R.; Baker, D.
2009AGUFMSM43A1737P Altcode:
Multi-point electron temperature measurements from the Cluster
constellation of spacecraft orbiting in tetrahedral formation provide
a framework for calculating the local electron temperature dependence
on plasma sheet location. Separate parallel and perpendicular
temperature components may vary strongly along two or even three
dominant directions. Nevertheless, six representative plasma sheet
crossings using varying Cluster tetrahedron scale sizes indicate the
mean temperature variation in a given direction is dominated by the
component along a single direction of maximal temperature change. The
temperature variation perpendicular to this dominant direction is
relatively small. Because plasma transport occurs preferentially
along the direction of the magnetic field, it is reasonable to infer
the temperature should be constant along B-field lines. However, the
observed magnetic field, and Tsyganenko-modeled field for our crossings
have significant component along the dominant direction, and so exhibit
large temperature variation along B. Temperature variations may persist
regardless of plasma mixing in the plasma sheet. Implications for
plasma sheet models, Alfven waves, and field-line resonances will be
presented based on plasma, energetic particle and magnetic field line
detailed analysis.

---------------------------------------------------------
Title: The Space Environment of Mercury at the Time of the Third
MESSENGER Flyby: Solar Wind and IMF Modeling of Upstream Conditions
Authors: Odstrcil, D.; Baker, D.; Anderson, B. J.; Mayer, L. R.;
Slavin, J. A.; Solomon, S. C.
2009AGUFM.P24A..02O Altcode:
The third flyby of Mercury by the MESSENGER spacecraft occurred on
29 September 2009. In order to provide contextual information about
the solar wind properties and the interplanetary magnetic field (IMF)
near the planet, we have used an empirical modeling technique combined
with a numerical-physics-based solar wind model. The Wang-Sheeley-Arge
(WSA) method uses solar photospheric magnetic field observations (from
Earth-based instruments) to estimate inner heliospheric conditions
out to 21.5 solar radii from the Sun. This information is then used
as input to the global numerical magnetohydrodynamic model, ENLIL,
which calculates solar wind velocity, density, temperature, and magnetic
field strength and polarity throughout the inner heliosphere. WSA-ENLIL
calculations for the several-week period encompassing MESSENGER’s
third Mercury flyby provide a critical context for understanding flyby
observations and global magnetospheric modeling results.

---------------------------------------------------------
Title: Systematics of Electron Flux Decay Lifetimes in the Outer
Radiation Belts
Authors: Kanekal, S. G.; Fennell, J.; Baker, D.; Blake, J. B.
2009AGUFMSM23A1584K Altcode:
The fluxes of energetic electrons in the outer belt are highly dynamic
often varying by several orders of magnitude in a matter of a few
days. This variability is the result of balance between energization
and loss processes. Wave-particle interactions have long been known to
cause particle precipitation. Some of the types of waves responsible for
particle loss include the EMIC, and the VLF chorus waves. The latter
are thought to be important outside the plasmapause whereas inside
the plasmapause EMIC waves cause particle loss due to pitch angle
scattering. Particle interactions with different types of waves may
result in differeent decay timescales. We will report on investigations
of electron flux decay times. The aim our research is to delineate
the role played by various plasma waves such as plasmaspheric hiss,
chorus and EMIC in electron precipitation leading to flux depletion. Our
preliminary investigations show a clustering of decay time scales with
a preponderance of lifetimes of 5, 10.5, and 17.5 days albeit for a
limited data set. This study will use data from multiple spacecraft
such as SAMPEX, Polar and HEO to measure electron flux decay times
over the entire outer zone. We will also examine decay times as a
function of electron energy and cover electron events over nearly
a solar cycle. Such a full and detailed study has the potential to
examine the conditions under which distinct decay processes may operate.

---------------------------------------------------------
Title: Building upon the Electronic Geophysical Year (eGY) Experience:
Transitioning Research Results to Operations (Invited)
Authors: Baker, D.
2009AGUFMSA34A..06B Altcode:
The past 15 years have seen the development of many cost effective
ways to acquire, store, and exchange data. We have the potential
to expand the exchange of data by allowing working scientists and
operational agencies to access and manipulate information and models
from large interdisciplinary centers as well as from small, previously
isolated, research groups. The key to this technology requires adoption
of community-developed standards for data storage and description to
form an ”Informatics Commons.” Scientific societies currently promote
the establishment of a system of Virtual Observatories. The Electronic
Geophysical Year (eGY) concept (2007-2008) embraced all available and
upcoming geophysical data (e.g., atmospheric, geomagnetic, ionospheric,
magnetospheric, etc.) and advocated organizing them into a series of
virtual geophysical observatories deployed in cyberspace. This concept
allows access to all available data through the Internet and World Wide
Web, taking advantage of existing networking hardware and software
technologies (e.g., Internet, XML, Service-Oriented Architectures,
Semantic Web, etc.). The eGY provided an international focus for a
resolve to address the issues of data release, data discovery, and
data preservation. This effort can help revolutionize the transition
of basic research to a state of operational readiness.

---------------------------------------------------------
Title: Energetic electrons response to ULF waves induced by
interplanetary shocks in the outer radiation belt
Authors: Zong, Q.; Li, X.; Zhou, X.; Pu, Z.; Song, P.; Baker, D.;
Fritz, T. A.; Daly, P. W.; Dunlop, M. W.
2009AGUFMSM34A..06Z Altcode:
Strong interplanetary shock interactions with the Earth's
magnetosphere have great impacts on energetic particle dynamics in
the magnetosphere. An interplanetary shock on 7 November 2004 (with
the maximum solar wind dynamic pressure of ∼ 70 nPa) was observed
by the Cluster constellation to induce significant ULF waves in the
plasmasphere boundary, and energetic electrons (up to 2 MeV) were
almost simultaneously accelerated when the interplanetary shock
impinged upon the magnetosphere. In this paper, the relationship
between the energetic electron bursts and the large shock-induced ULF
waves is studied. It is shown that the energetic electrons could be
accelerated and decelerated by the observed ULF wave electric fields,
and the distinct wavenumber of the poloidal and toroidal waves at
different locations also indicates the different energy ranges of
electrons resonating with these waves. For comparison, a rather weak
interplanetary shock on 30 August 2001 (dynamic pressure { ∼} 2.7 nPa)
is also investigated. It is found that interplanetary shocks or solar
wind pressure pulses with even small dynamic pressure change can have
a non-negligible role in the radiation belt dynamics.

---------------------------------------------------------
Title: Mercury’s atmosphere and magnetosphere: MESSENGER third
flyby observations (Invited)
Authors: Slavin, J. A.; Anderson, B. J.; Baker, D.; Benna, M.;
Boardsen, S. A.; Johnson, C. L.; Gloeckler, G.; Gold, R. E.; Killen,
R. M.; Korth, H.; Krimigis, S. M.; McClintock, W. E.; McNutt, R. L.;
Purucker, M. E.; Sarantos, M.; Schriver, D.; Solomon, S. C.; Sprague,
A. L.; Vervack, R. J.; Zurbuchen, T.; Travnicek, P.
2009AGUFM.P24A..01S Altcode:
MESSENGER’s third flyby of Mercury en route to orbit insertion
about the innermost planet took place on 29 September 2009. The
earlier 14 January and 6 October 2008 encounters revealed that
Mercury’s magnetic field is highly dipolar and stable over the
35 years since its discovery by Mariner 10; that a structured,
temporally variable exosphere extends to great altitudes on the
dayside and forms a long tail in the anti-sunward direction; a cloud
of planetary ions encompasses the magnetosphere from the dayside bow
shock to the downstream magnetosheath and magnetotail; and that the
magnetosphere undergoes extremely intense magnetic reconnection in
response to variations in the interplanetary magnetic field. Here we
report on new results derived from observations from MESSENGER’s
Mercury Atmospheric and Surface Composition Spectrometer (MASCS),
Magnetometer (MAG), and Energetic Particle and Plasma Spectrometer
(EPPS) taken during the third flyby.

---------------------------------------------------------
Title: Mercury's magnetosphere-solar wind interaction under northward
and southward interplanetary magnetic field during the MESSENGER
flybys
Authors: Travnicek, P. M.; Schriver, D.; Hellinger, P.; Hercik, D.;
Slavin, J. A.; Sarantos, M.; Anderson, B. J.; Korth, H.; Zurbuchen,
T.; Baker, D.; Benna, M.; Sprague, A. L.; Killen, R. M.; McClintock,
W. E.; Ho, G. C.; Krimigis, S. M.; McNutt, R. L.; Solomon, S. C.
2009AGUFM.P21A1204T Altcode:
Analysis of global hybrid simulations of Mercury's magnetosphere--solar
wind interaction under northward and southward interplanetary magnetic
field (IMF) orientations provides a context for evaluating observations
during MESSENGER's first two encounters with Mercury. The global
kinetic simulations reveal the basic structure of this interaction,
including a bow shock, ion foreshock, magnetosheath, cusp regions,
magnetopause, and a closed ion ring belt formed around the planet
within the magnetosphere. The two different IMF orientations induce
different locations of ion foreshock and different magnetospheric
properties: the dayside magnetosphere is smaller and cusps are at
lower latitudes for southward IMF than for northward IMF, whereas
for southward IMF the nightside magnetosphere is larger and exhibits
a thin current sheet with signatures of magnetic reconnection and
plasmoid formation. For the two IMF orientations the ion foreshock and
quasi-parallel magnetosheath manifest ion-beam-driven large-amplitude
oscillations, whereas the quasi-perpendicular magnetosheath shows
ion-temperature-anisotropy-driven wave activity. The ions in Mercury's
belt remain quasi-trapped for a limited time before they are either
absorbed by Mercury's surface or escape from the magnetosphere.

---------------------------------------------------------
Title: The role of Shabansky orbits in the generation of
compression-related EMIC waves
Authors: McCollough, J. P.; Elkington, S. R.; Baker, D.
2009AGUFMSM43C..08M Altcode:
Electromagnetic ion-cyclotron (EMIC) waves arise from temperature
anisotropies in trapped warm plasma populations. In particular, EMIC
waves at high L values near local noon are often found to be related
to magnetospheric compression events. There are several possible
mechanisms that can generate these temperature anisotropies: energizing
processes, including adiabatic compression and shock-induced and radial
transport; and non-energizing processes, such as drift shell splitting
and the effects of off-equatorial minima on particle populations. In
this work we investigate the role of off-equatorial minima in the
generation of temperature anisotropies both at the magnetic equator
and at higher latitudes. There are two kinds of behavior particles
undergo in response: particles with high equatorial pitch angles
(EPAs) are forced to execute so-called Shabanksy orbits and mirror
at high latitudes without passing through the equator, and those with
lower EPAs will pass through the equator with higher EPAs than before;
as a result, perpendicular energies increase at the cost of parallel
energies. By using a 3D particle tracing code in a tunable analytic
compressed-dipole field, we parameterize the effects of Shabansky
orbits on the anisotropy of the warm plasma. These results as well
as evidence from simulations of a real event in which EMIC waves were
observed (the compression event of 29 June 2007) are presented.

---------------------------------------------------------
Title: The Impact of the Virtual Observatories on Space Weather
Science, Modeling, and Predictions (Invited)
Authors: Green, J. C.; Weigel, R. S.; Kihn, E. A.; Baker, D.
2009AGUFMSH54A..04G Altcode:
Five years ago, the NASA Living with a Star program funded a group of
Virtual Observatories intended to “integrate data and models across
many missions, data centers, agencies and countries”. Each observatory
was designed to meet the unique needs of specific heliophysics research
communities. One of the observatories funded under this program,
that will be the main focus of this presentation, was the Virtual
Radiation Belt Observatory. This observatory was to accelerate science
and modeling by helping scientists overcome research challenges such
as the lack of publicly available observational and model data, data
inter-calibration differences, and limited access to common analysis
tools. The research advancements were expected to feed-back into
better models that ultimately would benefit space weather users such
as satellite operators and designers. Using ViRBO as the main example,
this presentation will demonstrate how the virtual observatories have
benefited the space weather community and identify areas for possible
improvement. We review the initial vision for the observatories,
present their current implementation, and provide example cases
describing how the observatories have been successfully used.

---------------------------------------------------------
Title: A Remarkable Natural Experiment: The Extremely Quiet Sun
(2007-2009) and its Effect on Earth's Radiation Belts
Authors: Farr, N. L.; Baker, D.; Kanekal, S. G.; Li, X.
2009AGUFMSM21B..05F Altcode:
In late 2008 and into 2009, the Earth’s electron radiation belts
have virtually disappeared. This is unprecedented in the observational
record. The Sun has been going through its most profound minimum
of activity in the modern era. The paucity of sunspot activity and
the associated absence of major solar coronal mass ejections has,
in turn, meant that no large geomagnetic storms or other such space
weather events have occurred within the Earth’s magnetosphere. The
minimum of solar activity has led to an almost complete cessation of
external drivers - and the radiation regions around the Earth (the
Van Allen radiation belts) have thereby attained their most reduced,
quiescent state ever directly witnessed. The events now underway with
the quiet Sun offer a rich opportunity to see how quickly, effectively,
and completely the radiation belts can naturally be depleted toward
their putative ground state. We observe that the electron radiation
belt fluxes (E &gt; 2 MeV) in 2009 have been reduced by a factor of
10 4-10 5-compared to 2003-2004. Moreover, the slot region between
the inner and outer Van Allen belts has spread outward to L &gt; 4,
thereby making a broad region devoid of electrons in what previously
was the heart of the outer zone.

---------------------------------------------------------
Title: Severe Space Weather Events: Global Geospace Responses to
Powerful Solar Wind Drivers (Invited)
Authors: Baker, D.
2009AGUFMSM34A..05B Altcode:
Recent international space science programs have made a concerted effort
to study activity on the Sun, the propagation of energy bursts from
the Sun to near-Earth space, energy coupling into the magnetosphere,
and its redistribution and deposition in the upper and middle
atmosphere. Extreme solar, geomagnetic and solar wind conditions can be
observed by a large international array of satellites and ground-based
sensors. We discuss the types of space weather-related problems that
have been identified in recent times and consider examples of space
weather-induced spacecraft (and ground-based) anomalies and failures
that affect both civilian and military systems. Special attention will
be given to delineating the specific kinds of geospace responses that
occur for different transient solar wind drivers. In this context,
we discuss near-term plans to consolidate and integrate understanding
as an important component of the community effort to propose technical
and operational solutions to space weather problems. I will focus on
new scientific advancement that is needed for successful space weather
programs and will describe actions that can help assure a good future
integrated space weather program.

---------------------------------------------------------
Title: Magnetic Reconnection along Quasi-separatrix Layers as a
Driver of Ubiquitous Active Region Outflows
Authors: Baker, D.; van Driel-Gesztelyi, L.; Mandrini, C. H.;
Démoulin, P.; Murray, M. J.
2009ApJ...705..926B Altcode: 2009arXiv0909.4738B
Hinode's EUV Imaging Spectrometer (EIS) has discovered ubiquitous
outflows of a few to 50 km s-1 from active regions
(ARs). These outflows are most prominent at the AR boundary and
appear over monopolar magnetic areas. They are linked to strong
non-thermal line broadening and are stronger in hotter EUV lines. The
outflows persist for at least several days. Using Hinode EIS and X-Ray
Telescope observations of AR 10942 coupled with magnetic modeling,
we demonstrate that the outflows originate from specific locations
of the magnetic topology where field lines display strong gradients
of magnetic connectivity, namely quasi-separatrix layers (QSLs),
or in the limit of infinitely thin QSLs, separatrices. We found the
strongest AR outflows to be in the vicinity of QSL sections located over
areas of strong magnetic field. We argue that magnetic reconnection at
QSLs separating closed field lines of the AR and either large-scale
externally connected or "open" field lines is a viable mechanism for
driving AR outflows which are likely sources of the slow solar wind.

---------------------------------------------------------
Title: Signatures of interchange reconnection: STEREO, ACE and Hinode
observations combined
Authors: Baker, D.; Rouillard, A. P.; van Driel-Gesztelyi, L.;
Démoulin, P.; Harra, L. K.; Lavraud, B.; Davies, J. A.; Opitz, A.;
Luhmann, J. G.; Sauvaud, J. -A.; Galvin, A. B.
2009AnGeo..27.3883B Altcode: 2009arXiv0909.5624B
Combining STEREO, ACE and Hinode observations has presented an
opportunity to follow a filament eruption and coronal mass ejection
(CME) on 17 October 2007 from an active region (AR) inside a coronal
hole (CH) into the heliosphere. This particular combination of
"open" and closed magnetic topologies provides an ideal scenario for
interchange reconnection to take place. With Hinode and STEREO data
we were able to identify the emergence time and type of structure
seen in the in-situ data four days later. On the 21st, ACE observed
in-situ the passage of an ICME with "open" magnetic topology. The
magnetic field configuration of the source, a mature AR located
inside an equatorial CH, has important implications for the solar and
interplanetary signatures of the eruption. We interpret the formation of
an "anemone" structure of the erupting AR and the passage in-situ of the
ICME being disconnected at one leg, as manifested by uni-directional
suprathermal electron flux in the ICME, to be a direct result of
interchange reconnection between closed loops of the CME originating
from the AR and "open" field lines of the surrounding CH.

---------------------------------------------------------
Title: Myths and Mysteries of Solar Wind Speed and MeV Electrons in
the Magnetosphere
Authors: Li, X.; Baker, D.
2009EGUGA..11.2554L Altcode:
The remarkable correlation between high speed solar wind and the
enhancement of energetic electrons in the magnetosphere has been
identified for over four decades, yet the mystery of this correlation
remains. Recently, several interpretations about this correlation have
been proposed and most of them are incomplete and some of them may have
generated the widespread verdict (or myth) that enhanced ULF waves
alone lead to enhanced MeV electrons in the radiation belts. In this
presentation, we present a brief review of the association of high speed
solar wind and energetic electrons across the entire relevant energy
range (10s of keV to multi-MeV) and magnetospheric region (from inner
magnetosphere to cental plasmasheet). We discuss the incompleteness
of existing interpretations and we describe a more complete picture
in understanding this mystery.

---------------------------------------------------------
Title: Simulations of emerging flux in a coronal hole: oscillatory
reconnection
Authors: Murray, M. J.; van Driel-Gesztelyi, L.; Baker, D.
2009A&A...494..329M Altcode:
Context: Observations and simulations show that reconnection will
take place when a flux tube emerges into a coronal hole, which is
characterised by magnetic fieldlines “open” towards interplanetary
space. Although the mechanism by which reconnection is initiated has
been thoroughly studied, the long-term evolution of this reconnecting
magnetic system remains unreported. Aims: We aim to understand
the long-term evolution of the reconnecting flux tube and coronal
hole system and, in particular, to ascertain whether it can reach an
equilibrium state in which all reconnection has ceased. By determining
the evolution in this particular scenario, we aim to be able to
select a subset from the broad spectrum of reconnecting systems,
which will undergo the same progression to equilibrium. Methods:
Using a 2.5-dimensional numerical magnetohydrodynamic (MHD) code, we
evolve a simple stratified atmospheric domain, which is endowed with a
vertical magnetic field, representing the interior of a coronal hole,
and a horizontal buoyant flux tube that is placed near the bottom
of the domain. To investigate the long-term evolution of the system,
we continue to study the domain long after the flux tube has emerged
and reconnection has commenced between the magnetic fields of the
flux tube and coronal hole. Results: We find that a series of
reconnection reversals (or oscillatory reconnection) takes place,
whereby reconnection occurs in distinct bursts and the inflow and
outflow magnetic fields of one burst of reconnection become the
outflow and inflow fields in the following burst of reconnection,
respectively. During each burst of reconnection the gas pressure in the
bounded outflow regions increases above the level of that in the inflow
regions and, eventually, gives rise to a reconnection reversal. In
consecutive bursts of reconnection, the contrast in the gas pressure
across the boundaries of the inflow and outflow regions decreases and,
over time, the system settles towards equilibrium. Once the equilibrium
state is reached, all reconnection ceases. This is the first reported
instance of oscillatory reconnection initiated in a self-consistent
manner, and the signatures of the mechanism compare favourably with
observations of select flux emergence events and with solar and stellar
flares. Conclusions: Across the broader spectrum of reconnecting
systems, oscillatory reconnection will only occur if the outflow regions
are quasi-bounded during each burst of reconnection. The swaying outflow
jet and periodic heating signatures of oscillatory reconnection are
exceedingly similar to those exhibited by MHD modes and, in many
observations, distinction between the two mechanisms may be impossible.

---------------------------------------------------------
Title: Hinode EIS and XRT Observations of Hot Jets in Coronal Holes -
Does the Plasma Escape?
Authors: Baker, D.; van Driel-Gesztelyi, L.; Kamio, S.; Culhane,
J. L.; Harra, L. K.; Sun, J.; Young, P. R.; Matthews, S. A.
2008ASPC..397...23B Altcode:
X-ray jets have been detected in the extreme ultraviolet (EUV) and
soft X-ray observations of Hinode's EIS and XRT instruments. Both
instruments were used to observe the jets in polar and on-disk coronal
holes (CHs). Here, we present a multi-wavelength study of an X-ray
jet and its associated bright point found in an equatorial CH on 19
June 2007. Light curves (LCs) in 22 different emission lines were
compared to that of Hinode/XRT. As we found in a previous study of
two polar X-ray jets, this jet shows a post-jet increase in its EUV
LCs. The post-jet enhancement appears cooler than the jet. We suggest
this feature arises because the hot plasma of the jet, having failed to
reach escape speeds, cools and falls back along the near vertical paths
expected to be created by reconnection with open field lines of CHs. In
addition to the increase in post-jet EUV intensity, we found tentative
evidence of impact heating possibly caused by the fall-back of plasma.

---------------------------------------------------------
Title: Kriging Interpolation Algorithm for Displaying Global SABER
Infrared Measurements
Authors: Williams, J.; Coakley, H.; Baker, D.; Mlynczak, M.; Russell,
J., III
2008AGUSMSA41B..06W Altcode:
Three-dimensional atmospheric measurements from satellites are typically
unevenly sampled in resolution for both time and space. To create a
global representation for atmospheric trends analysis, an interpolation
method was implemented using SABER data from the NASA TIMED satellite. A
hybrid Kriging processing method was developed and validated. This
method shows significant improvements over a linear interpolation
model. Hybrid Kriging uses an adaptive statistical least-squares
approach to best give a continuous model of the relationship between
discrete data points. The algorithm has been rendered less processing
intensive, validated using infrared atmospheric data from the SABER
multi-channel scanning radiometer, and then displayed for scientific
analysis.

---------------------------------------------------------
Title: Outflows at the Edges of Active Regions: Contribution to
Solar Wind Formation?
Authors: Harra, L. K.; Sakao, T.; Mandrini, C. H.; Hara, H.; Imada,
S.; Young, P. R.; van Driel-Gesztelyi, L.; Baker, D.
2008ApJ...676L.147H Altcode:
The formation of the slow solar wind has been debated for many years. In
this Letter we show evidence of persistent outflow at the edges of
an active region as measured by the EUV Imaging Spectrometer on board
Hinode. The Doppler velocity ranged between 20 and 50 km s-1
and was consistent with a steady flow seen in the X-Ray Telescope. The
latter showed steady, pulsing outflowing material and some transverse
motions of the loops. We analyze the magnetic field around the active
region and produce a coronal magnetic field model. We determine from
the latter that the outflow speeds adjusted for line-of-sight effects
can reach over 100 km s-1. We can interpret this outflow as
expansion of loops that lie over the active region, which may either
reconnect with neighboring large-scale loops or are likely to open to
the interplanetary space. This material constitutes at least part of
the slow solar wind.

---------------------------------------------------------
Title: Erratum: "Outflows at the Edges of Active Regions: Contribution
to Solar Wind Formation?" (ApJ, 676, L147 [2008])
Authors: Harra, L. K.; Sakao, T.; Mandrini, C. H.; Hara, H.; Imada,
S.; Young, P. R.; van Driel-Gesztelyi, L.; Baker, D.
2008ApJ...677L.159H Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Interaction between emerging flux and coronal hole -
observations and simulations
Authors: van Driel-Gesztelyi, Lidia; Baker, Deborah; Murray, Michelle;
Demoulin, Pascal; Attrill, Gemma; Matthews, Sarah A.; Mandrini,
Cristina H.; Toeroek, Tibor
2008cosp...37.3288V Altcode: 2008cosp.meet.3288V
Flux emergence in the vicinity of or inside a coronal hole (CH) is
expected to induce magnetic reconnection between the closed emerging
and open CH magnetic field lines, resulting in an evolution of the
CH as formerly closed field lines become topologically open, while at
the same time, open field lines close down. Through two case studies
we show observational signatures of this (interchange) reconnection
process and discuss its implications. First, using SOHO EIT and MDI
data, we study a small active region (AR10869) emerging in the close
vicinity of a low-latitude coronal hole in April 2006. The interfacing
magnetic polarities between the AR and the CH were opposite, favourable
for magnetic reconnection. We indeed observe the coupled formation of
bright closed loops between the CH and the AR and coronal dimming on
the far side of the AR, which we interpret as evidence of interchange
reconnection. This process effectively modifies the CH boundary
(making it retreat), while simultaneously displacing open field lines
to the far side of the AR. In order to study this process in detail,
we perform 2.5D MHD simulations, which qualitatively reproduce important
aspects of the observations. We expect to find upflows of plasma at the
location where previously closed field lines are opening up as well as
on the reconnecting side, but since we had no spectroscopic data for
this event, we can not verify this. Therefore we analyze Hinode/EIS
line-of-sight velocity maps of another low-latitude CH with a small AR
in its midst observed on 18 Oct. 2007. We find that while closed loops
of the bipole are dominated by downflows in the Fe XII, Fe XIII and
Fe XV lines, the strongest coronal plasma upflows are indeed located
around and particularly at the "far side" of the bipolar AR, i.e. having
the same polarity as the dominant polarity of the CH. The emerging
biplole and the series of interchange reconnections it induces create
a significant additional plasma upflow in the CH, thus we identify
this outflow must contribute to the acceleration of the fast solar wind.

---------------------------------------------------------
Title: In situ observation of radiation belt particle response to
an interplanetary shock
Authors: Zong, Q.; Zhou, X.; Song, P.; Li, X.; Baker, D.; Fritz, T.
2007AGUFMSM33C..03Z Altcode:
Interplanetary shock is one of the most powerful drivers of magnetic
storms which often result in strong energetic particles enhancements
and the Van Allen radiation belt compression in the magnetosphere. The
elevated fluxes of the energetic particles have been proven to be
number one threat to space technological systems. How these particles
are accelerated is an important and active research subject in space
physics. In this study we show that after an interplanetary shock
impact on the magnetosphere, the acceleration of the energetic electrons
started nearly immediately in the radiation belt and lasted a few hours.

---------------------------------------------------------
Title: Hinode EUV Study of Jets in the Sun's South Polar Corona
Authors: Culhane, Len; Harra, Louise K.; Baker, Deborah; van
Driel-Gesztelyi, Lidia; Sun, Jian; Doschek, George A.; Brooks, David
H.; Lundquist, Loraine L.; Kamio, Suguru; Young, Peter R.; Hansteen,
Viggo H.
2007PASJ...59S.751C Altcode:
A number of coronal bright points and associated plasma jet features
were seen in an observation of the South polar coronal hole during
2007 January. The 40" wide slot was used at the focus of the Hinode
EUV Imaging Spectrometer to provide spectral images for two of these
events. Light curves are plotted for a number of emission lines that
include He II 256Å (0.079MK) and cover the temperature interval from
0.4MK to 5.0MK. Jet speed measurements indicate values less than the
escape velocity. The light curves show a post-jet enhancement in a
number of the cooler coronal lines indicating that after a few minutes
cooling, the plasma fell back to its original acceleration site. This
behavior has not been previously observed by e.g., the Yohkoh Soft
X-ray Telescope due to the comparatively high temperature cut-off
in its response. The observations are consistent with the existing
models that involve magnetic reconnection between emerging flux and the
ambient open field lines in the polar coronal hole. However we do not
have sufficient coverage of lines from lower temperature ion species
to register the Hα-emitting surge material that is associated with
some of these models.

---------------------------------------------------------
Title: Meteorite Collection on the Lunar Surface
Authors: Erikson, L.; Baker, D.; Rance, W. L.; Spahr, E.; Abbud-Madrid,
A.; Heeley, M. B.
2007LPICo1371.3052E Altcode: 2007eelo.work.3052E
No abstract at ADS

---------------------------------------------------------
Title: Evidence for interchange reconnection between a coronal hole
and an adjacent emerging flux region
Authors: Baker, D.; van Driel-Gesztelyi, L.; Attrill, G. D. R.
2007AN....328..773B Altcode:
Coronal holes are regions of dominantly monopolar magnetic field on the
Sun where the field is considered to be `open' towards interplanetary
space. Magnetic bipoles emerging in proximity to a coronal hole
boundary naturally interact with this surrounding "open" magnetic
field. In the case of oppositely aligned polarities between the active
region and the coronal hole, we expect interchange reconnection to
take place, driven by the coronal expansion of the emerging bipole as
well as occasional eruptive events. Using SOHO/EIT and SOHO/MDI data,
we present observational evidence of such interchange reconnection
by studying AR 10869 which emerged close to a coronal hole. We find
closed loops forming between the active region and the coronal hole
leading to the retreat of the hole. At the same time, on the far side
of the active region, we see dimming of the corona which we interpret
as a signature of field line `opening' there, as a consequence of a
topological displacement of the `open' field lines of the coronal hole.

---------------------------------------------------------
Title: Hinode Euv Study Of Jets In The Sun’s South Polar Corona
Authors: Culhane, J. L.; Brooks, D. H.; Doschek, G. A.; Harra, L. K.;
van Driel-Gesztelyi, L.; Baker, D.; Lundquist, L. L.; Hansteen, V. H.;
Kamio, S.
2007AAS...210.7201C Altcode: 2007BAAS...39..178C
Using the Hinode EUV Imaging Spectrometer coronal jets were observed
on 20-JAN-2007 over a range of emission lines and corresponding plasma
temperatures using the 40 arc sec wide slot images. In this preliminary
analysis, jet plasma temperature and emissivity have been estimated
while, based on assumptions about the jet morphology, electron density
estimates are given and jet velocity measured. The evolution of the
jets will be followed in a number of different EUV emission lines and
jet energy input as a function of time will be assessed with reference
to the magnetic field topologies involved.

---------------------------------------------------------
Title: Energy Transport, Storage, and Dissipation in the Magnetosphere
During Substorms.
Authors: Halford, A. J.; Baker, D.; Weygand, J.
2007AGUSMSM53A..04H Altcode:
Magnetospheric substorms represent a global interaction between the
solar wind, magnetosphere, and ionosphere. Energy transported from the
solar wind into the magnetosphere is largely stored in the tail until it
is released (primarily into the ionosphere and the ring current). The
Akasofu epsilon parameter (ɛ=4π L / μ v B2 sin 4 θ / 2), and
multiple empirically determined formulas for energy dissipation into
the ionosphere (joule heating and particle precipitation) and the ring
current have been considered for such global interactions. An energy
budget and estimation of total energy in the tail has been created for
12 isolated substorms that occurred during 2001. Considerable complexity
and individuality of substorms is observed with substantial differences
in the input and dissipation pattern for individual events. Our analysis
is compared with previous published results.

---------------------------------------------------------
Title: The D-CIXS X-ray spectrometer on the SMART-1 mission to the
Moon—First results
Authors: Grande, M.; Kellett, B. J.; Howe, C.; Perry, C. H.; Swinyard,
B.; Dunkin, S.; Huovelin, J.; Alha, L.; D'Uston, L. C.; Maurice, S.;
Gasnault, O.; Couturier-Doux, S.; Barabash, S.; Joy, K. H.; Crawford,
I. A.; Lawrence, D.; Fernandes, V.; Casanova, I.; Wieczorek, M.;
Thomas, N.; Mall, U.; Foing, B.; Hughes, D.; Alleyne, H.; Russell,
S.; Grady, M.; Lundin, R.; Baker, D.; Murray, C. D.; Guest, J.;
Christou, A.
2007P&SS...55..494G Altcode:
The SMART-1 mission has recently arrived at the Moon. Its payload
includes D-CIXS, a compact X-ray spectrometer. SMART-1 is a technology
evaluation mission, and D-CIXS is the first of a new generation
of planetary X-ray spectrometers. Novel technologies enable new
capabilities for measuring the fluorescent yield of a planetary surface
or atmosphere which is illuminated by solar X-rays. During the extended
SMART-1 cruise phase, observations of the Earth showed strong argon
emission, providing a good source for calibration and demonstrating
the potential of the technique. At the Moon, our initial observations
over Mare Crisium show a first unambiguous remote sensing of calcium
in the lunar regolith. Data obtained are broadly consistent with
current understanding of mare and highland composition. Ground truth
is provided by the returned Luna 20 and 24 sample sets.

---------------------------------------------------------
Title: End-to-End Modeling of the Solar Terrestrial System
Authors: Wiltberger, M.; Baker, D.
2007sdeh.book..217W Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Temporal variability of the MLTI region observed through five
years of SABER and TIMED
Authors: Remsberg, E. E.; Williams, J.; Turpin, T.; Mlynczak, M. G.;
Russell, J. M.; Baker, D.
2006AGUFMSA24A..07R Altcode:
The Sounding of the Atmosphere using Broadband Emission Radiometry
instrument has achieved nearly five years of flawless operation on the
NASA Thermosphere Ionosphere Mesosphere Energetics and Dynamics (TIMED)
satellite. The instrument offers an unprecedented data set of over
thirty products including, temperature, density, ozone, atomic species,
and thermodynamic parameters. The SABER data exhibit clear signals
associated with the decline of the current phase of the solar cycle,
particularly in the thermosphere and the NO(v) emission at 5.3 um,
which is observed to decrease by a factor of 2.5 since early 2002. Also
examined are the evolution of the thermal structure and chemical
composition during the five years in orbit. Mesospheric temperatures
are observed to decrease over the period, with the largest decreases
observed at the highest altitudes measured by SABER. These measurements
will be reviewed and placed in the context of the atmospheric response
to solar variability.

---------------------------------------------------------
Title: The Electric Field Wave Instrument on the Radiation Belt
Storm Probe Mission
Authors: Wygant, J. R.; Cattell, C. A.; Dombeck, J.; Bonnell, J.;
Mozer, F.; Bale, S.; Chaston, C.; Ergun, B.; Baker, D.; Li, X.; Hudson,
M. K.; Strangeway, R.; Alpert, J.; Brautigam, D.; Mann, I.; Foster, J.
2006AGUFMSM33A0331W Altcode:
The purpose of the Electric Field-Wave Instrument on the two RBSP
spacecraft is to investigate the role of plasma structures and waves
in the physical processes responsible for the acceleration, transport,
and loss of energetic particles in the inner magnetosphere of the
Earth. Some of these processes include: prompt acceleration induced
by powerful interplanetary shocks, acceleration by the large scale
convection electric field, abrupt energization by intense substorm
injection fronts propagating in from the tail, coherent and stochastic
radial transport by large scale MHD fluctuations, multi-step local
energization and cattering by whistler waves, and scattering and
energization by kinetic Alfven waves, ion cycltron waves, and other
small scale waves and structures. In order to understand the role of
these processes in accelerating particles, the EFW instrument measures
the three dimensional electric field from dc to greater than 500
kHz. The spin plane electric field vector is obtained from spherical
sensors at the ends of two pair of orthogonal booms with tip-to- tip
separations of 80 and 100 m. The spin axis measurement is obtained by
opposed stacer booms with a tip- to-tip separation of 12 meters or
greater. The electric field below 12 Hz is telemetered continuously
while higher time resolution is obtained from a programmable burst
memory with a maximum sampling rate for six quantities of greater 30,000
samples/s each. DC magnetic fields from the fluxgate magnetometer and
wave magnetic fields from the search coil, both associated with the
University of Iowa Instrument are input into the EFW instrument for
processing in the burst memory and in the Digital Signal Processing
Board (DSP). The DSP provides wave spectra and cross spectra of electric
and magnetic field data over the frequency range between 50 Hz and
10 kHz with a typical cadence of once per 12 seconds with a maximum
rate of ~ 1 Hz in order to provide continuous information on wave
properties including: the wave power, the normal direction, the phase
velocity, the waves electrostatic or electro-magnetic structure, the
longitudinal component of the electric field, the parallel component of
the electric field, and Poynting flux. The EFW instrument also provides
a wave electric field signal to the University of Iowa Instrument.

---------------------------------------------------------
Title: The Radiation Belt Storm Probes (RBSP) Energetic Particle,
Composition, and Thermal Plasma (ECT) Instrument Suite
Authors: Spence, H. E.; Kepko, E.; Reeves, G.; Funsten, H.; Thomsen,
M.; Henderson, M.; Friedl, R.; Skoug, R.; Jordanova, V.; Fennell,
J.; Blake, J. B.; Clemmons, J.; O'Brien, T.; Green, J.; Onsager, T.;
Elkington, S.; Baker, D.; Li, X.; Goldstein, J.; Young, D.; Jahn,
J.; Thorne, R.; Hudson, M.; Horne, R.; Bourdarie, S.; Mann, I.
2006AGUFMSM33A0335S Altcode:
The Energetic particle, Composition, and Thermal plasma (ECT) instrument
suite was selected recently by NASA as part of the Radiation Belt Storm
Probe (RBSP) mission. In this presentation, we summarize the RBSP-ECT
science investigation. The ECT suite contains a well-proven complement
of particle instruments to ensure the highest quality measurements in
the inner magnetosphere. The coordinated ECT particle measurements,
analyzed in combination with fields and waves observations and
state-of-the-art theory and modeling, are required for understanding
the acceleration, global distribution, and variability of radiation
belt electrons and ions, key science objectives of NASA's Living With
a Star program and the RBSP mission. ECT has four science objectives,
which consolidate the eight prioritized RBSP mission objectives. They
are: (1) determine the physical processes that produce radiation belt
enhancements; (2) determine the dominant mechanisms for relativistic
electron loss; (3) determine how the inner magnetospheric plasma
environment controls radiation belt acceleration/loss; and, (4)
develop empirical and physical models for understanding/predicting
radiation belt space weather effects. In this poster, we present an
overview of the science and measurements goals of the ECT suite as
well as the instruments required to achieve those goals.

---------------------------------------------------------
Title: Fuel Oxidizer Reaction Products (FORP) Contamination of Service
Module and Release of N-Nitrosodimethylamine in a Humid Environment
from Crew EVA Suits Contaminated with FORP
Authors: Schmidl, W.; Mikatarian, R.; Lam, C. -W.; West, B.; Buchanan,
V.; Dee, L.; Baker, D.; Koontz, S.
2006pmss.book..193S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: End-to-End Modeling of the Solar Terrestrial System
Authors: Wiltberger, M.; Baker, D.
2006SSRv..124..217W Altcode: 2007SSRv..tmp...54W
Traditionally modeling for space science has concentrated on developing
simulations for individual components of the solar terrestrial
system. In reality these regions are coupled together. This coupling can
be as simple as the driving of the magnetosphere ionosphere thermosphere
system by the solar wind or as a complicated as the feedback of the
ionospheric conductivity and currents on the magnetosphere. As part of
the CISM project we are beginning a concentrated effort to compressively
model the entire system. This approach includes chains of models. In the
first chain physics based numerical models are utilized while in the
second chain empirical models are coupled together. The first half of
this paper discusses the numerical modeling approach by highlighting the
coupling of pairs of regions within the system. In the second section
we present results from empirical models which are combined to make
long term forecasts of conditions in the geospace environment. It is
expected that a validated and reliable forecast model for space weather
can be obtained by combining the strongest elements of each chain.

---------------------------------------------------------
Title: Modeling the Self-Organized Critical Behavior of Earth's
Plasma Sheet Reconnection Dynamics
Authors: Klimas, A.; Uritsky, V.; Baker, D.
2006AGUSMSM22A..02K Altcode:
Analyses of Polar UVI auroral image data (Uritsky et al. JGR, 2002; GRL,
2003, 2006) show that bright night- side high-latitude UV emissions
exhibit so many of the key properties of systems in self-organized
criticality that an alternate interpretation has become virtually
impossible. It is now necessary to find and model the source of
this behavior. We note that the most common models of self-organized
criticality are numerical sandpiles. These are, at root, models that
govern the transport of some quantity from a region where it is loaded
to another where it is unloaded. Transport is enabled by the excitation
of a local threshold instability; it is intermittent and bursty, and
it exhibits a number of scale-free statistical properties. Searching
for a system in the magnetosphere that is analogous and that, in
addition, is known to produce auroral signatures, we focus on the
reconnection dynamics of the plasma sheet. In our previous work, a
driven reconnection model has been constructed and has been under study
(Klimas et al. JGR, 2004; GRL 2005). The transport of electromagnetic
(primarily magnetic) energy carried by the Poynting flux into the
reconnection region of the model has been examined. All of the analysis
techniques, and more, that have been applied to the auroral image
data have also been applied to this Poynting flux. Here, we report
new results showing that this model also exhibits so many of the key
properties of systems in self-organized criticality that an alternate
interpretation is implausible. Further, we find a strong correlation
between these key properties of the model and those of the auroral
UV emissions. We suggest that, in general, the driven reconnection
model is an important step toward a realistic plasma physical model
of self-organized criticality and we conclude, more specifically,
that it is also a step in the right direction toward modeling the
multiscale reconnection dynamics of the magnetotail.

---------------------------------------------------------
Title: Energetic Particle Modulation in the Radiation Belt Region
Authors: Zong, Q.; Fritz, T.; Baker, D.; Li, X.; Balogh, A.; Reme, H.
2006AGUSMSM52A..05Z Altcode:
One of open questions in the Earth's radiation belt is to determine
which processes dominant in accelerating magnetospheric several keV
electrons to MeV energies. In particular recent studies have emphasized
the question of the relative dominance of ULF and VLF wave acceleration
processes across the outer belt. Energetic electron and ion flux and
spectra variations associated with ULF waves in the inner magnetosphere
have been examined by using Cluster spacecraft data. The quasi-periodic
particle flux (electron 30 keV to 500 keV, proton 30 keV to 1.5
MeV) modulations are observed in the the region of L=5.3 to 11.7 at
MLT=8. The relative phase of energetic electron and ion are different in
the different location, also, depend on the energy of the particles. The
particle fluxes were found to be either 90 or 270 out of phase with the
magnetic variations. For the phase difference between the ion density
and the magnetic variation, this argues that the time-average Poynting
flux of the Pc5 wave along the ambient magnetic field is approximately
zero, this indicates that Pc5 waves are standing waves along the field
line. In-situ ULF measurements from inside geosynchronous orbit are not
commonly available. Multi-point measurements of the ULF wave electric
and magnetic field morphology, as well as radiation belt particle flux,
are made in this paper to examine the efficiency of the ULF process in
the outer belt. Cluster constellation allow to determine wave coherence
length and mode structure, which are critical parameters for determining
the efficiency of the ULF wave drift-resonance interaction.

---------------------------------------------------------
Title: Open exchange of data: the eGY pathway towards capacity
building.
Authors: Barton, C.; Baker, D.; Cobabe-Ammann, E.; Fox, P.; Kihn,
E.; Peterson, W. K.
2006cosp...36.2387B Altcode: 2006cosp.meet.2387B
The Electronic Geophysical Year 2007-2008 eGY uses the 50-year
anniversary of the acclaimed International Geophysical Year to
advance open access to data information and services The International
Polar Years of 1882-1882 and 1932-1933 taught us that free and open
exchange of data between nations is cost effective The International
Geophysical Year 1957-1958 taught us that free and open exchange
of data between scientific disciplines generates new and exciting
research The worldwide network of data centers and data standards
initiated during IGY continues to foster research to this day And
better things lie ahead As we approach the 50th anniversary of the
IGY the development of distributed data systems allows worldwide
connectivity to data and services at a level never before possible
Such systems virtual observatories and so forth expand the free open
and cross-disciplinary exchange of data by allowing users worldwide
to access and manipulate data from principal data centers as well as
from small previously isolated research groups The new information and
communication technologies require that we adopt community-developed
standards for data storage and description They also demand that we
recognize and accommodate the shift in effort from the user to the
provider that accompanies a change from the traditional user-pull to a
modern provider-push data environment eGY provides an opportunity for
coordinated discussions on data storage and description standards These
standards have implications for the infrastructure needed to access and

---------------------------------------------------------
Title: Outward radial diffusion during the main phase of a storm
Authors: Shprits, Y.; Thorne, R.; Friedel, R.; Reeves, G.; Fennell,
J.; Baker, D.; Kanekal, S.
2006cosp...36.1089S Altcode: 2006cosp.meet.1089S
The variability of the radiation belt electron fluxes is a result of
a competition between various source and loss processes which highly
depend on the evolution of the plasmaspheric and ring current plasma
populations Relativistic electrons can be accelerated by the inward
radial diffusion which is most efficient at higher L-shells and by
local acceleration which is most efficient right outside plasmasphere
Losses of relativistic electrons may result from pitch angle scattering
of electrons by various plasma waves and losses to magnetopause Using
observations from CRRES HEO and SAMPEX satellites and radial diffusion
modeling we show that magnetopause losses combined with outward radial
diffusion may produce significant depletions of the outer radiation
belt down to L 4 We also show that radial diffusion driven by gradients
in phase space density redistributes radiation belt fluxes and may
effectively work as a loss and source process

---------------------------------------------------------
Title: High Resolution Substorm Energetic Electrons seen in the
Magnetotail by all 4 CLUSTER satellites
Authors: Wu, P.; Fritz, T. A.; Reed, R. S.; Friedel, R.; Reeves, G.;
Baker, D.; Daly, P.
2005AGUFMSM32A..04W Altcode:
We report our examination of the 3-D pitch angle distributions (PAD) of
energetic electrons as the Cluster satellites cross the earth's plasma
sheet near their apogee in the nightside magnetosphere during the tail
season (July, August, September, October) of year 2005. We identified
several energetic electron injections in the tail plasma sheet
associated with substorm events. Those events are all associated with
continual switching of PADs from field aligned to the peak at 90 degree,
which indicated to us that those energetic electrons are accelerated
in different manners and they form different populations. The study
of the evolution of the PAD gave us an impression that the Fermi and
betatron accelerations play different roles along the tail. They compete
with each other, depend on the radial distance. However, this idea
needs to be further verified with the study of more events. The large
separations of the 4 Cluster satellites in this tail season of 2005
provide a good opportunity for us to identify more energetic electron
bursts events with better spatial and temporal clarity. Comparing
the observation from these 4 different satellites will allow us to
visualize the picture in many more dimensions and avoid vagueness as
much as we can. Together with our collaboration with LANL and LASP,
including more satellite data (e.g. Geosynchronous satellites, POLAR,
IMAGE), we will report on a more integrated picture of the magnetotail
energetic electron dynamics.

---------------------------------------------------------
Title: Earthward Flowing Plasmoid: Structure and Its Related Auroral
Signature
Authors: Fritz, T.; Zong, Q.; Baker, D.; Goldstein, M.; Daly, P.;
Fu, S.; Frey, H.; Balogh, A.; Reme, H.
2005AGUFMSM24A..03F Altcode:
An earthward-moving plasmoid on Oct. 28, 2002 has been observed by
the Cluster spacecraft with simultaneous auroral viewing by IMAGE
satellite. This offers the opportunity to ascertain the optical
signature and its evolution in the ionosphere of an earthward moving
plasmoid for the first time. The intensity of the current in the
center of the plasmoid is found to be weaker than that in the adjacent
region. Also, the directions of the current in the central part of
the plasmoid are different from the background cross-tail current:
they are more field-aligned. The calculation of J × B demonstrates
that the plasmoid is not a highly force-free structure. The unusually
large bipolar electric field found in the plasmoid (peak to peak values
6 and 8 mV/m) can be explained as a dawn-dusk polarization electric
field is generated to enhance the flows as predicted in the bubble
model. Broad-band electrostatic noise (BEN) and bursty electrostatic
electron cyclotron waves are found inside the plasmoid which are closely
associated with the acceleration of the plasma. Furthermore, IMAGE
data show the auroral forms moving to lower latitude, which is when
an earthward moving plasmoid observed by the Cluster spacecraft. Such
an equatorward auroral motion is consistent well with the observed
earthward moving plasmoid.

---------------------------------------------------------
Title: Global statistics of OH layer heights and double layers from
SABER limb measurements of OH Meinel emission at 1.6 and 2.0 μm.
Authors: Winick, J. R.; Wintersteiner, P. P.; Picard, R. H.; Taylor,
M. J.; Baker, D.; Mylnczak, M. G.; Russell, J. M.; Gordley, L. L.
2005AGUFMSA43A1095W Altcode:
Two of the 10 radiometers on the SABER instrument aboard the TIMED
spacecraft measure the limb profiles from the OH Meinel first-overtone
bands at 2.0 μm (OH-A) and at 1.6 μm (OH-B). The OH-A band originates
from high-lying vibrational states (v=8-9) of the OH ground electronic
state, while the OH-B band originates from low-lying vibrational states
(v=3-5). These provide limb radiance profiles continuously over a
latitude range 53S-82N or 82N-53S, depending upon the phase of the yaw
cycle. We have examined important characteristics of the volume emission
rate (VER) profiles of these bands that have been obtained by inverting
the radiance profiles. In particular, we characterize the global
occurrence probabilities of the heights of both layers as a function
of latitude, local time and season and note any differences in behavior
between the two bands. Although the OH layer is often considered to be
a fixed profile with a narrow peak near 87 km, a significant number of
the profiles show distinctly different behavior. Melo et al. (JGR, 2000)
reported that double-peaked layers were found in UARS/WINDI data 5-25%
of the time. SABER also sees double layers at least 10% of the time
and observes the peak VER at times below 80 km, altitudes not observed
in the WINDI data. We will examine the occurrence statistics of these
features and look for correlations with large tidal amplitudes and
temperature inversions that are simultaneously measured by SABER. These
correlations may hold clues to what dynamical processes could produce
such double peaks and anomalously low-altitude peaks.

---------------------------------------------------------
Title: Contribution of Radial Transport to the Deep Penetration of
Outer Belt Electrons During Oct-Nov Magnetic Storm of 2003
Authors: Li, X.; Barker, A.; Baker, D.; Selesnick, R.; Friedel, R.
2005AGUFMSM41D..06L Altcode:
During the geomagnetic storm of October/November 2003, the intensity
peak of the outer radiation belt electron moved from its nominal
position of L=4 to L=2.5 within a day. This event was correlated with
extremely high solar wind speeds and enhanced ULF wave power throughout
the inner magnetosphere, both are known to be associated with enhanced
radial transport of radiation belt electrons. A modeling effort was
made, using the measurements of relativistic electrons at geosynchronous
orbit as the source population and solar wind parameters as input to
a radial diffusion coefficient. We found that the deep penetration
of MeV electrons down to L=2.5 could be mostly explained by the fast
inward radial transport mechanism.

---------------------------------------------------------
Title: Energetic Particle Modulation by ULF waves in the inner
magnetosphere
Authors: Zong, Q.; Fritz, T.; Baker, D.; Fu, S.; Xie, L.; Daly, P.;
Balogh, A.; Reme, H.
2005AGUFMSM41D..05Z Altcode:
One of most important questions in the Earth's radiation belt is
to determine the dominant processes which accelerate magnetospheric
several keV electrons to MeV energies. In particular recent studies
have emphasized the question of the relative dominance of ULF and VLF
wave acceleration processes across the outer belt. Energetic electron
and ion flux and spectra variations associated with ULF waves in the
inner magnetosphere have been examined by using Cluster spacecraft
data. The quasi-periodic particle flux (electron 30 keV to 500 keV,
proton 30 keV to 1.5 MeV) modulations are observed in the the region
of L=5.3 to 11.7 at MLT=8. The relative phase of energetic electron
and ion are different in the different location, also, depend on the
energy of the particles. The particle fluxes were found to be either
90 or 270 out of phase with the magnetic variations. For the phase
difference between the ion density and the magnetic variation, this
argues that the time-average Poynting flux of the Pc5 wave along the
ambient magnetic field is approximately zero, this indicates that Pc5
waves are standing waves along the field line. In-situ ULF measurements
from inside geosynchros orbit are not commonly available. Multi-point
measurements of the ULF wave electric and magnetic field morphology,
as well as radiation belt particle flux, are made in this paper to
examine the efficiency of the ULF process in the outer belt. Cluster
constellation allow to determine wave coherence length and mode
structure, which are critical parameters for determining the efficiency
of the ULF wave drift-resonance interaction.

---------------------------------------------------------
Title: Radial Diffusion as a Potential Source and Loss Mechanism of
Relativistic Electrons in the Outer Radiation Belt
Authors: Shprits, Y. Y.; Thorne, R.; Friedel, R.; Reeves, G. D.;
Fennel, J. F.; Baker, D.; Shrikanth, K.; Horne, R.
2005AGUFMSM51D..06S Altcode:
The loss mechanisms responsible for the sudden depletions of the outer
electron radiation belt are examined based on observations and radial
diffusion modeling. SAMPEX data for October-December 2003, indicates
that depletions are correlated with increases in geomagnetic activity
and also correlated with sudden increases in the solar wind dynamic
pressure. Multi-channel HEO observations show that depletions are seen
at energies as low as a few hundred keV. For the same events high energy
proton channels also show decrease in fluxes at higher L-values. These
observations are consistent with outward radial diffusion driven by the
loss to magnetopause. We further examine the viability of the outward
radial diffusion loss by comparing CRRES observations with a radial
diffusion model simulations. Model-data comparison shows that flux
variation near geosynchronous orbit can be effectively propagated by the
outward radial diffusion to lower L-values and can account for the main
phase storm depletions. The presence of the outward radial diffusion
rises an important question: What is the origin of the relativistic
electrons at geosynchronous orbit plasma sheet or radiation belts?

---------------------------------------------------------
Title: Plasmaspheric Influence on Radiation Belts During Major
Geomagnetic Storms
Authors: Goldstein, J.; Baker, D.; Sandel, B. R.; Burch, J. L.;
Fennell, J. F.
2005AGUSMSM31A..01G Altcode:
We investigate a possible causal relationship between erosion of
the plasmasphere and enhancement of the radiation belts during major
geomagnetic storms. The Earth's plasmasphere was observed by the IMAGE
EUV imager to be drastically reduced in size by the 2003 Halloween
geomagnetic storm event. Before the storm the plasmapause was seen
at roughly 4 Earth radii (RE) geocentric distance; after the storm,
the plasmapause had moved inside 2 RE. This dramatic erosion of the
plasmasphere apparently had a profound effect on the global distribution
of the Van Allen radiation belts. Wave-particle interactions inside the
plasmasphere normally act to remove the radiation belt electrons inside
the slot region; however, in the days following the 2003 Halloween
storm's drastic plasmasphere erosion, SAMPEX witnessed the formation
of an extremely intense new radiation belt in what was formerly
the slot region. This chain of events suggests that the plasmasphere
configuration can have a primary influence on the global radiation belt
distribution. We present preliminary results of the investigation of
this possible relationship for three major geomagnetic storms, using
global images of the plasmasphere side-by-side with in situ energetic
particle data. We discuss likely mechanisms for quickly accelerating
electrons to the high levels observed in the slot that normally is
devoid of such relativistic electrons.

---------------------------------------------------------
Title: The correlation between the inner edge of outer radiation
belt electrons and the location of plasmapause
Authors: Li, X.; Barker, A.; Gannon, J.; Baker, D.; Kanekal, S.;
Selesnick, R.
2005AGUSMSM23C..02L Altcode:
During the period of enhanced geomagnetic activity, both the outer
radiation belt electrons and plasmapause move toward the Earth. Are
these just a natural consequence of enhanced solar wind interaction
with the magnetosphere or are they intrinsically related? Recent
studies indicate that the location of the plasmapause may determine
the location of the peak in the outer belt electron intensity. Our
study of long term satellite measurements shows that the inner edge
of the outer belt electrons correlates well with the location of
plasmapause. Combining data from SAMPEX, CRRES, Polar, IMAGE, ACE and
ground magnetometers and modeling efforts, we will address the role
of the plasmasphere in radiation belt acceleration and loss processes.

---------------------------------------------------------
Title: Energetic particle acceleration during a major magnetic storm
Authors: Kerttula, R.; Mursula, K.; Asikainen, T.; Friedel, R.; Baker,
D.; Søraas, F.; Fennell, J. F.; Blake, J. B.; Grande, M.
2005AdSpR..36.1835K Altcode:
We study the global properties of energetic (&gt;30 keV) particles
during the main and early recovery phase of a major magnetic storm
of March 31, 2001, using data of the NOAA 15 and 16 and the CLUSTER
satellites. During the storm main phase the ring current energetic
electron and ion fluxes were increased by nearly two orders of
magnitude, and the flux maxima were shifted to below L = 3. The
maximum ion fluxes were observed at about 07 UT, coinciding with the
minimum Dst. However, the highest fluxes of energetic electrons were
observed only at about 16-18 UT, indicating significant differences in
the acceleration of energetic electrons and ions during the storm. We
suggest that the ion maximum at about 07 UT was due to field-aligned
acceleration of ions from the ionosphere whereas the electron maximum
at 16-18 UT was due to a large injection from the nightside.

---------------------------------------------------------
Title: First results — Lunar X-ray mapping spectrometer on smart-1
Authors: Grande, Manuel; Kellett, B.; Howe, C.; Perry, C. H.;
Swinyard, B.; Dunkin, S.; Huovenin, J.; Thomas, N.; Mall, U.; Hughes,
D.; Alleyne, H.; Russell, S.; Grady, M.; Lundin, R.; Barabash, S.;
Baker, D.; Murray, C. D.; Guest, J. E.; Crawford, I.; Casanova, I.;
Maurice, S.; Gasnault, O.; Foing, B.; Lawrence, D.; Fernandez, V.
2005CIBu..163...18G Altcode: 2005SpReT.163...18G
No abstract at ADS

---------------------------------------------------------
Title: Hemispheric Differences and Evolution of the Cold Summer
Mesopause Observed by the SABER Experiment on the TIMED Satellite
Authors: Russell, J. M.; Mlynczak, M. G.; Mertens, C. J.; Gordley,
L. L.; Picard, R. H.; Winick, J.; Wintersteiner, P.; Garcia, R.;
Siskind, D. E.; Lopez-Puertas, M.; Remsberg, E. E.; Baker, D.
2004AGUFMSA33B..02R Altcode:
The Sounding of the Atmosphere using Broadband Emission Radiometry
(SABER) experiment was launched on December 7, 2001 into a 74.1
degree inclined, 625 km orbit onboard the TIMED satellite. The primary
science goal of SABER is to achieve major advances in understanding the
structure, energetics, chemistry, and dynamics in the atmospheric region
extending from 60 to 180 km altitude. SABER has been operating almost
continuously since activation using the space flight proven experiment
approach of spectral broadband limb emission radiometry applied in
10 selected infrared spectral bands ranging from 1.27 micrometers
to 17 micrometers wavelength. Observed limb emission profiles are
being processed on the ground to provide vertical profiles with 2 km
altitude resolution of key constituents, energetics parameters and
temperature. Measurements are made both night and day over the latitude
range from 52 degrees to 83 degrees with alternating hemisphere coverage
every 60 days. During the time SABER has been operating, there have been
two major solar storms in April 2002 and October 2003. The temporal
and geographic coverage provided by SABER has provided path finding
observations on the atmospheric effects of these events. In addition,
the battery of measurements made by SABER has yielded new information
on atmospheric energetics effects including radiative cooling due to
the 15 micrometer band of CO2 and the persistence of heating due to
exothermic chemical reactions. SABER observations have also provided
new information on the mesopause latitudinal structure and evolution
and have revealed the presence of a two-day wave in the mesopause
region that previously was known only through modeling. Further,
the data have shed light on the global distribution of the effects
of nitric oxide vertical descent into the upper stratosphere and on
the variability of atomic oxygen. This paper summarizes the major
scientific results from SABER up to now using illustrative examples.

---------------------------------------------------------
Title: Cluster Observations of Earthward Flowing Plasmoid in the Tail
Authors: Zong, Q.; Fritz, T.; Fu, S.; Pu, Z.; Baker, D.; Zhang, H.;
Lui, A.; Glassmeier, K.; Korth, A.; Daly, P.; Balogh, A.; Reme, H.
2004AGUFMSM31A1216Z Altcode:
The energetic electrons and ions embedded in Earthward-moving plasmoid
structures have been observed. These plasmoids are associated with a
rotational local Bz component (bi-polar) signature. Energetic
electrons are found to be confined in a smaller spatial region than ions
inside the plasmoid. Energetic ions and electrons seem to be a good
indicator for the structure boundary. The fleet of Cluster spacecraft
cross the plasmoid structure in a "first entry, last out" order (Note:
when spacecraft cross a planar discontinuity, e.g. magnetopause, they
will be in "first entry, first out" order). This documents the fact that
the plasmoid has a non-planar nested structure. The large separation
distance (around 1 RE) of the Cluster satellites in October
2002 is an advantage to provide constraints on the size and shape of the
plasmoid structure of interest. In addition, the plasmoid (with closed
field lines) should preserve the ion composition information where it is
formed. The ion composition observed in the plasmoid shows significantly
lower O and He than in the ambient plasma. This implies few heavy
ions are involved in the reconnection process where the plasmoid is
formed. Multiple flux ropes/plasmoids observation presented in this
paper can be interpreted as strong evidence for multiple X-lines.

---------------------------------------------------------
Title: Sensitivity Tests of the Temerin-Li Dst Model
Authors: Halford, A. J.; Weigel, R.; Baker, D.
2004AGUFMSM43A1146H Altcode:
The Dst historically has been used as a measure of the disturbance
of the magnetosphere and an indicator of when a geomagnetic storm is
occuring. The Temerin-Li [2002] (TL02) model is a semi-empirical Dst
model which was trained on five years (1995 - 1999) of data. The TL02
model is the most successful Dst predictor in terms of prediction
efficiency, with a reported prediction efficiency of greater then
.90. The inputs into this model are the solar wind parameters,
solar wind velocity, interplanetary magnetic field, and solar wind
density. This model is based on the Burton et al. model, but has
many parameters whose physical relavance are not well understood. To
better understand the physical relevance of the empirical parameters,
we use parameter sensitivity, impulse response, and driver sensitivity
analysis. These techniques are used along with seasonal and diurnal
analysis of the prediction error to extract a physical understanding
of the most influential components of the model. By holding the input
parameters constant and comparing this output and the output from
sending pulses of delta t = 1 hour at regular intervals over a period
of a year to the actual Dst, we can observe the diurnal and seasonal
variations due to the individual parameters.

---------------------------------------------------------
Title: CISM Metrics Plan and Initial Model Validation Results
Authors: Spence, H. E.; Baker, D.; Burns, A.; Guild, T.; Huang, C.;
Siscoe, G.; Weigel, R.
2004AGUSMSM54A..03S Altcode:
Metrics and model validation represent two key elements upon which
the success of the Center for Integrated Spaceweather Modeling (CISM)
hinges. The routine calculation of important operationally- and
scientifically-motivated metrics permits us to objectively measure
and track the ability of coupled CISM models to predict essential
space weather quantities. The rationale for CISM metrics selection is
developed and the list of 29 metrics, along with the baseline models,
first-generation physics models, and the data sets needed to compute
skill scores, are outlined. While metrics provide a means for the
objective assessment of long-term model improvement, model validation -
the comprehensive, systematic quantitative comparison of model output
with observations - is required for identifying and documenting model
strengths and weaknesses. Two representative examples of initial
validation efforts are summarized. The first uses case study analysis
techniques and comparison with in situ observations during real events
to explore the range of validity of the Lyon-Fedder-Mobarry (LFM)
MHD simulation during magnetic storms. The second uses a statistical
approach to compare the climatology of plasma sheet bulk properties
(density, temperature, magnetic field, flows) deduced from both
spacecraft observation and modeled by the LFM code.

---------------------------------------------------------
Title: Lunar Elemental Composition and Ivestigations with D-CIXS
X-Ray Mapping Spectrometer on SMART-1
Authors: Grande, M.; Dunkin, S.; Howe, C.; Browning, R.; Kellett,
B.; Perry, C. H.; Swinyard, B.; Waltham, N.; Kent, B.; Huovenin, J.;
Thomas, N.; Mal, U.; Hughes, D.; Alleyne, H.; Russell, S.; Grady,
M.; Lundin, R.; Barabash, S.; Baker, D.; Murray, C. D.; Guest, J.;
Casanova, I.; Maurice, S.; Foing, B.
2004LPI....35.1519G Altcode:
The D-CIXS Compact X-ray Spectrometer on ESA SMART-1 successfully
launched in Sept 2003 can derive 45 km resolution images of the
Moon with a spectral resolution of 185 eV, providing the first
high-resolution global map of rock forming element abundances.

---------------------------------------------------------
Title: An Overview Of The SABER Experiment And Science Results
Authors: Gordley, L. L.; Russell, J. M.; Mlynczak, M. G.;
Mertens, C. J.; Remsberg, E. E.; Picard, R. H.; Lopez-Puertas, M.;
Wintersteiner, P.; Winick, J.; Siskind, D. E.; Baker, D.; Garcia, R.
2003AGUFMSA32B..01G Altcode:
The Sounding of the Atmosphere using Broadband Emission Radiometry
(SABER) experiment was launched on December 7, 2001 into a 74.1o
inclined, 625 km orbit onboard the TIMED satellite. The primary
science goal of SABER is to achieve major advances in understanding
the structure, energetics, chemistry, and dynamics in the atmospheric
region extending from 60 to 180 km altitude. SABER has been operating
almost continuously since activation using the space flight proven
experiment approach of spectral broadband limb emission radiometry. The
instrument scans the earth limb in 10 selected spectral bands ranging
from 1.27 mm to 17 mm wavelength. The observed limb emission profiles
are being processed on the ground to provide vertical profiles with 2
km altitude resolution of the following: temperature, O3, H2O, and CO2
mixing ratios; volume emission rates due to O2 (1D), OH (u=3,4,5), OH
(u=7,8,9), and NO; key atmospheric cooling rates, solar heating rates,
chemical heating rates, and airglow losses; atomic oxygen, atomic
hydrogen and geostrophic winds. Measurements are made both night
and day over the latitude range from 54oS to 87oN with alternating
hemisphere coverage every 60 days. SABER has provided new information
on energetics of the TIMED core region, observed atmospheric effects
of major solar storms and made measurements in both northern and
southern polar summers. This paper provides an experiment overview,
orbital performance, comparisons with correlative observations and an
overview of science results.

---------------------------------------------------------
Title: Replication As An Alternative Approach For Large Segmented
Telescopes
Authors: Farber, M.; Ulmer, M. P.; Graham, M. E.; Vaynman, S.; Varlese,
S.; Baker, D.; Echt, J.
2003AAS...203.3819F Altcode: 2003BAAS...35.1263F
The next generation of optical/IR telescopes will require large
numbers of co-phased mirror segments. Therefore, some form of
replication technology is desirable to reduce costs. Eletroforming
has the advantage that it is a commercially developed technology
for replication, and the technology has been widely used for making
X-ray mirrors (e.g. XMM-Newton). Composite materials are appealing,
since a great deal of development work has been done with composites
as well. There are 3 areas that need to be addressed: replication with
minimal stress so as to produce a high quality figure; attachment of
support of the mirror segment so as to maintain the figure quality;
thermal control requirements. Here we present a discussion of the
requirements that lead us to select replication as the fabrication
technology and the advantages of replication. We report on our first
results of making a concave and flat mirrors. This work was
funded by a NASA Space Grant to Illinois, Ball Aerospace, Northwestern
University, NASA Contract NAS1-03007, an AFOSR Contract F4620-C-0073,
and a NASA Grant NAG5-03069.

---------------------------------------------------------
Title: Coordinated Energetic Particle Measurements Using Chandra,
Cluster, and Polar
Authors: Mueller-Mellin, R.; Blake, J. B.; Baker, D.
2003AGUFMSM51E..02M Altcode:
It is not well known in the magnetospheric physics community that
the Chandra spacecraft carries a multi-element energetic particle
telescope called EPHIN (Electron Proton Helium Instrument) fielded
by the University of Kiel. For present purposes we are interested
in electrons that are measured from greater than 30 keV to greater
than 10 MeV. Chandra is in a highly elliptical orbit with a perigee
of 16000 km, and apogee of 133,000 km and an inclination of 28
degrees. Fortuitously the line of apsides is relatively close to that
of the Cluster constellation. A first use of the Chandra data has been
a further examination of a substorm onset that occurred = 0408 UT on 27
August 2001, discussed in a publication by Baker et al. (2002). At that
time the s/c coordinates in GSM were Chandra (-6.64, 16.15, 12.82);
Cluster 3 (-19.15, -1.40, 1.54); Polar (-7.71, -4.50, 3.32). It can
be seen that whereas Cluster and Polar were a bit post midnight and
roughly radially aligned, Chandra was well pre-midnight at around 20
hrs. Yet the onset time of energetic electrons at Chandra was very close
to that observed at Cluster and Polar. Furthermore, some pre-substorm
bursts were also seen to be closely time coincident at Chandra and the
other spacecraft. These observations give additional evidence about the
scale size of the phenomena and will be discussed in detail along with
other coordinated measurements. Baker et al. GRL 29, no. 24, 2190, 2002

---------------------------------------------------------
Title: Branch Prediction and Speculative Execution in Magnetospheric
Forecasting
Authors: Doxas, I.; Horton, W.; Baker, D.; McPherron, R.; Weigel,
R.; Wiltberger, M.
2003AGUFMSM51B0522D Altcode:
Recent advances in the development of integrated models of the Sun-Earth
environment are placing increasing emphasis on data assimilation schemes
that can maximize the intelligence extracted from our sparse sampling of
upwind conditions. One of the schemes proposed is Branch Prediction and
Speculative Execution, which consists of making probabilistic estimates
of current upstream conditions, and distribute among available machines
simulations that assume each of the probabilistically estimated states
as initial conditions. As the near-Earth space evolves and near-Earth
satellite data are compared with the models, some of the speculatively
executed simulations will be proved wrong. At that point the machines
that were executing them will be reassigned either to new lines of
speculative simulation, or to increase the processing power devoted to
more promising simulations already executing. The scheme is particularly
suited to Space Weather since our upwind early warning sentries can
provide only sparse sampling of the incoming solar wind, while the
bulk of our monitors, which can provide significantly better coverage,
are located close to Earth and provide much shorter lead times. By
the time the data come in from the near-Earth monitors, the forecasts
of the speculative simulations are already in hand. CALCHAS is a 3D
visualization package that integrates models and data, and is used in
the above data assimilation scheme. The package is written in Java 3D,
and has a modular design, so that different models and datasets, both
real-time and historical, can be seamlessly compared using a variety of
goodness-of-fit measures. The scheme gives good results when used with
particle simulations and WINDMI, a low-dimensional dynamical model of
the coupled Magnetosphere-Ionosphere system (Doxas and Horton, Using
Branch Prediction and Speculative Execution to Forecast Space Weather,
Geospace Environment Modeling meeting, Telluride, CO, 2002). Numerical
perturbation studies of global MHD models will also be presented.

---------------------------------------------------------
Title: The D-CIXS X-ray mapping spectrometer on SMART-1
Authors: Grande, M.; Browning, R.; Waltham, N.; Parker, D.; Dunkin,
S. K.; Kent, B.; Kellett, B.; Perry, C. H.; Swinyard, B.; Perry, A.;
Feraday, J.; Howe, C.; McBride, G.; Phillips, K.; Huovelin, J.; Muhli,
P.; Hakala, P. J.; Vilhu, O.; Laukkanen, J.; Thomas, N.; Hughes, D.;
Alleyne, H.; Grady, M.; Lundin, R.; Barabash, S.; Baker, D.; Clark,
P. E.; Murray, C. D.; Guest, J.; Casanova, I.; d'Uston, L. C.; Maurice,
S.; Foing, B.; Heather, D. J.; Fernandes, V.; Muinonen, K.; Russell,
S. S.; Christou, A.; Owen, C.; Charles, P.; Koskinen, H.; Kato, M.;
Sipila, K.; Nenonen, S.; Holmstrom, M.; Bhandari, N.; Elphic, R.;
Lawrence, D.
2003P&SS...51..427G Altcode:
The D-CIXS Compact X-ray Spectrometer will provide high quality
spectroscopic mapping of the Moon, the primary science target
of the ESA SMART-1 mission. D-CIXS consists of a high throughput
spectrometer, which will perform spatially localised X-ray fluorescence
spectroscopy. It will also carry a solar monitor, to provide the direct
calibration needed to produce a global map of absolute lunar elemental
abundances, the first time this has been done. Thus it will achieve
ground breaking science within a resource envelope far smaller than
previously thought possible for this type of instrument, by exploiting
two new technologies, swept charge devices and micro-structure
collimators. The new technology does not require cold running, with
its associated overheads to the spacecraft. At the same time it will
demonstrate a radically novel approach to building a type of instrument
essential for the BepiColombo mission and potential future planetary
science targets.

---------------------------------------------------------
Title: Scientific rationale for the D-CIXS X-ray spectrometer on
board ESA's SMART-1 mission to the Moon
Authors: Dunkin, S. K.; Grande, M.; Casanova, I.; Fernandes, V.;
Heather, D. J.; Kellett, B.; Muinonen, K.; Russell, S. S.; Browning,
R.; Waltham, N.; Parker, D.; Kent, B.; Perry, C. H.; Swinyard, B.;
Perry, A.; Feraday, J.; Howe, C.; Phillips, K.; McBride, G.; Huovelin,
J.; Muhli, P.; Hakala, P. J.; Vilhu, O.; Thomas, N.; Hughes, D.;
Alleyne, H.; Grady, M.; Lundin, R.; Barabash, S.; Baker, D.; Clark,
P. E.; Murray, C. D.; Guest, J.; d'Uston, L. C.; Maurice, S.; Foing,
B.; Christou, A.; Owen, C.; Charles, P.; Laukkanen, J.; Koskinen,
H.; Kato, M.; Sipila, K.; Nenonen, S.; Holmstrom, M.; Bhandari, N.;
Elphic, R.; Lawrence, D.
2003P&SS...51..435D Altcode:
The D-CIXS X-ray spectrometer on ESA's SMART-1 mission will provide
the first global coverage of the lunar surface in X-rays, providing
absolute measurements of elemental abundances. The instrument will
be able to detect elemental Fe, Mg, Al and Si under normal solar
conditions and several other elements during solar flare events. These
data will allow for advances in several areas of lunar science,
including an improved estimate of the bulk composition of the Moon,
detailed observations of the lateral and vertical nature of the crust,
chemical observations of the maria, investigations into the lunar
regolith, and mapping of potential lunar resources. In combination with
information to be obtained by the other instruments on SMART-1 and the
data already provided by the Clementine and Lunar Prospector missions,
this information will allow for a more detailed look at some of the
fundamental questions that remain regarding the origin and evolution
of the Moon.

---------------------------------------------------------
Title: The Substorm at 05:45 on October 13, 2001 Observed From the
Ground, and the LANL, GOES, Polar, and Cluster Satellites
Authors: Peterson, W.; Baker, D.; Su, Y.; Eriksson, S.; Li, X.;
Sigwarth, J.; Scudder, J.; Donovan, E.; Korth, A.; Trattner, K.;
Slavin, J.; Reme, H.; Dunlop, M.; Andre, M.; Singer, H.; Friedel,
R.; Lu, G.; McPherron, R.; Russell, C.
2002AGUFMSM71A0580P Altcode:
The substorm at ~05:45 was not the first, last, or most intense of
those observed during the first half of October 13, 2001. However
the configuration of platforms noted in the title was excellent for
obtaining a comprehensive view of the initiation and evolution of a
substorm. The combination of Canopus ground magnetograms and Polar
VIS images identified onset at 05:45:02 +/- 00:00:22 west and south
of Ft. Churchill, Canada. The closest satellite, Polar, was located
near geosynchronous altitude at 23:00 MLT. Polar was sampling magnetic
fields and plasmas characteristic of the outer plasma sheet before
05:45 UT and characteristic of the central plasma sheet after 05:45
UT. Polar magnetometer data from below the magnetic equator and GOES 12
magnetometer data from above the magnetic equator suggest that the main
currents were flowing tailward of near-geosynchronous altitude. The
Cluster satellites were located at ~19 Re and ~21:00 MLT on the dusk
side of the magnetotail. A coherent dispersion feature in the plasma
at several of the Cluster spacecraft was observed at ~05:36 UT, when
the Bz (GSM) component on all four spacecraft began decreasing. The
Bz component was negative on all four Cluster spacecraft from ~05:42
to ~05:55 UT. We will present these observations and a time line of
events derived from them. We will discuss how these observations agree
and disagree with current ideas of the initiation and global evolution
of substorms.

---------------------------------------------------------
Title: Atmospheric models, GPS and InSAR measurements of the
tropospheric water vapour field over Mount Etna
Authors: Wadge, G.; Webley, P. W.; James, I. N.; Bingley, R.; Dodson,
A.; Waugh, S.; Veneboer, T.; Puglisi, G.; Mattia, M.; Baker, D.;
Edwards, S. C.; Edwards, S. J.; Clarke, P. J.
2002GeoRL..29.1905W Altcode: 2002GeoRL..29s..11W
Dynamic models of atmospheric movement over the Mount Etna volcano are
used to calculate the path delays affecting radar caused by variable
water vapour in the troposphere. We compare these model results with the
equivalent differential radar interferogram generated by two ERS-2 SAR
images taken 35 days apart and the water vapour delay retrievals from
a network of fourteen GPS stations distributed over the volcano. The
atmospheric model delay field agrees well with the long-wavelength
spatial differences measured by InSAR and those measured by GPS.

---------------------------------------------------------
Title: The SABER Experiment on the TIMED Mission: Overview and
Preliminary Science Results
Authors: Russell, J. M.; Mlynczak, M. G.; Gordley, L. L.; Mertens,
C. J.; Picard, R. H.; Lopez-Puertas, M.; Wintersteiner, P.; Winick,
J.; Siskind, D. E.; Baker, D.; Ulwick, J.; Remsberg, E. E.; Garcia,
R.; Espy, P. J.; Roble, R. G.; Solomon, S.
2002AGUSMSA51A..04R Altcode:
The Sounding of the Atmosphere using Broadband Emission Radiometry
(SABER) experiment was launched onboard the TIMED satellite at
7:07:35 am PST on December 7, 2001 from the Western Test Range. The
satellite was placed in a 74.1o inclined, 625 km orbit by a Delta II
rocket. The primary science goal of SABER is to achieve major advances
in understanding the structure, energetics, chemistry, and dynamics in
the atmospheric region extending from 60 to 180 km altitude. This will
be accomplished using the space flight proven experiment approach of
spectral broadband limb emission radiometry. The SABER instrument scans
the earth limb in 10 selected spectral bands ranging from 1.27 mm to 17
mm wavelength. The observed limb emission profiles are being processed
on the ground to provide vertical profiles with 2 km altitude resolution
the following: temperature, O3, H2O, and CO2 mixing ratios; volume
emission rates due to O2 (1D), OH (u=3,4,5), OH (u=7,8,9), and NO; key
atmospheric cooling rates, solar heating rates, chemical heating rates,
and airglow losses; atomic oxygen, atomic hydrogen and geostrophic
winds. Measurements are made both night and day over the latitude
range from 54oS to 87oN with alternating hemisphere coverage every 60
days. SABER measurements taken just after activation include data on
the cold summer mesopause in the southern hemisphere and observations of
the dynamically active northern hemisphere winter. This paper provides
an experiment overview, orbital performance, example data products,
and preliminary comparisons with correlative observations. Science
implications of the data will be discussed.

---------------------------------------------------------
Title: Self-Organized Criticality and Intermittent Turbulence in
the Plasma Sheet
Authors: Klimas, A.; Uritsky, V.; Vassiliadis, D.; Weigel, R.;
Baker, D.
2002AGUSMSM31B..06K Altcode:
Our recent analysis of Polar UVI image data has now made the evidence
for self-organized criticality (SOC) in the magnetospheric dynamics
difficult to interpret in any other way. The results support our
earlier suggestion that this SOC component of the dynamics is centered
in the plasma sheet and that it is related to the flow bursts and
associated localized reconnections that have been observed there. It is
necessary now to develop an interpretation of SOC in a plasma physical
context. Numerical simulations of a 2-D plasma sheet model that may
evolve into SOC will be discussed. Chang has suggested that intermittent
turbulence may be associated with SOC in the plasma sheet. Angelopolous
et al. [Phys. Plasmas, 1999], taking advantage of a rare conjunction
of the Geotail and Wind spacecraft in the plasma sheet, have shown
that relative cross-tail plasma velocities at the spatially separated
spacecraft positions exhibit a Castaing distribution, indicative of
intermittent turbulence. It will be shown that relative velocities in
the numerical solutions of the 2-D plasma sheet model also exhibit
this type of distribution when the model appears to be evolving in
the neighborhood of the SOC limit. Based on the model behavior, the
relationship between intermittent turbulence and SOC will be discussed.

---------------------------------------------------------
Title: The D-CIXS X-ray spectrometer, and its capabilities for
lunar science
Authors: Grande, M.; Dunkin, S.; Heather, D.; Kellett, B.; Perry,
C. H.; Browning, R.; Waltham, N.; Parker, D.; Kent, B.; Swinyard,
B.; Fereday, J.; Howe, C.; Huovelin, J.; Muhli, P.; Hakala, P. J.;
Vilhu, O.; Thomas, N.; Hughes, D.; Alleyne, H.; Grady, M.; Russell,
S.; Lundin, R.; Barabash, S.; Baker, D.; Clark, P. E.; Murray, C. D.;
Christou, A.; Guest, J.; Casanova, I.; d'Uston, L. C.; Maurice, S.;
Foing, B.; Kato, M.
2002AdSpR..30.1901G Altcode:
The purpose of the D-CIXS (Demonstration of a Compact Imaging X-ray
Spectrometer) instrument on the ESA SMART-1 mission is to provide high
quality spectroscopic mapping of the Moon by imaging fluorescence
X-rays emitted from the lunar surface. In order to obtain adequate
statistics for what can be very weak sources, it is essential to have
a large effective area, while maintaining a low mass. The solution is
to make a thin, low profile detector, essentially a modern version of
"X-ray detecting paper". D-CIXS will achieve a spatial resolution on
the ground of 42km from a spacecraft at 300 km altitude, with a spectral
resolution of 200 eV or better. The instrument is based around the use
of advanced dual microstructure collimator and Swept Charge Device
X-ray detector technologies. Swept Charge Device X-ray detectors,
a novel architecture based on proven CCD technology, have the virtue
of providing superior X-ray detection and spectroscopic measurement
capabilities, while also operating at room temperature. Thus we avoid
the need for the large passive cooling radiator that was previously
required to cool large X-ray focal plane CCDs. The advanced low profile
microstructure collimation and filter design builds on expertise
developed in solid state and microwave technology to enable us to
dramatically reduce the instrument mass. The total mass of D-CIXS,
including an X-ray solar monitor is ∼4.6 kg. D-CIXS will provide the
first global map of the Moon in X-rays. During normal solar conditions,
it will be able to detect absolute elemental abundances of Fe, Mg, Al
and Si on the lunar surface, using the on-board solar monitor to obtain
a continuous measurement of the input solar spectrum. During solar flare
events, it will also be possible to detect other elements such as Ca,
Ti, V, Cr, Mn, Co, K, P and Na. The global mapping of Mg, Al and Si,
and in particular deriving Mg#, the magnesium number (MgO/[MgO+FeO]),
represents the prime goal of the D-CIXS experiment.

---------------------------------------------------------
Title: New results on the structure and dynamics of the radiation
belts
Authors: Vassiliadis, D.; Weigel, R.; Klimas, A.; Fung, S.; Kanekal,
S.; Mewaldt, R.; Baker, D.; Rigler, E.
2002cosp...34E2936V Altcode: 2002cosp.meetE2936V
Earlier solar wind-magnetosphere coupling studies tell us that the
MeV electron pop- ulation in the outer zone responds to the solar
wind speed V_SW, IMF B_z, and B_tot. The most geoeffective profiles
of these quantities are associated with high- speed streams and
magnetic clouds. What is less known is that different L shell re-
gions of the inner magnetosphere respond to very different, sometimes
diametrically so, interplanetary conditions. Using the response to
the solar wind driving we iden- tify four regions: L=1-2, 2-3 (slot),
3-4 (P0, responding to shock- and cloud-like solar wind), 4-7 (P1,
responding to high-speed stream conditions), and 7-15 (P2, responding
to dV_SW/dt&lt;0 and IMF B_z&gt;0). We find that a) omnidirectional
fluxes in a given L shell are strongly correlated with fluxes in the
same region, but much less so with fluxes in other regions, giving
further support to the hypothesis of magnetospheric coherence. b)
The boundaries between regions (especially between P1 and P2 which
determines overall trapping capacity) vary with the solar cycle and
season. c) The re- sponse in each region increases with activity level,
but each region has a different rate of increase. d) The P2 region
is characterized by lower fluxes (typically &gt;2 orders of magnitude
below P1) organized in a fine structure of long-lived (days-weeks-long),
narrow (DeltaL=0.1-0.3) regions with generally different dynamics than
P0 or P1. The most prominent of these regions are located at L=9.4
and 7.5. These effects were stud- ied with SAMPEX and EXOS-C (OHZORA)
particle fluxes and the OMNIweb solar wind database.

---------------------------------------------------------
Title: Solar wind driven radiation belt response functions at 100-min
time scales using SAMPEX orbit-averaged electron fluxes
Authors: Baker, D.; Rigler, J.; Vassiliadis, D.
2002cosp...34E2198B Altcode: 2002cosp.meetE2198B
Characterizations of radiation belt dynamics using linear prediction
filters (LPFs) were first published by Nagai (1988) and Baker et
al. (1990). These studies focused primarily on short-term predictions
of daily-averaged radiation fluxes at geostationary orbit using global
magnetospheric indices and the speed of the so la r wind impinging on
the Earth's magnetosphere. Using solar wind data from the NSSDC OMNI
database and SAMPEX 2 6MeV omn idirectional electron fluxes at- various
magnetic L-shells, new analyses have combined linear response functions
to provide a three dimensional view (relative time, L-shell, and impulse
response) describing the linear response of relativistic radiation
belt electrons to solar wind input. Several physical interpretations
and implications are gleaned by applying this novel data analysis
technique. This includes the demonstration of strong seasonal and solar
cycle-dependent variatio ns in the global response function, as well
as the existence of a quasi-adiabatic peak in the response functions
just outside of the slot region. Our analyses have demonstrated the
ability of autoregressive(AR) filters to remove the diurnal variation
observed in radiation belt data sets. This paper extends prior work
by removing diurnal variations in SAMPEX orbit-averaged electron data
and analyzing the linear prediction filters at the 100-min time scales
of the SAMPEX orbit.

---------------------------------------------------------
Title: Cluster Observations of Magnetospheric Substorm Behavior In
The Near- and Mid-tail Regions
Authors: Baker, D.; Blake, J.; Burch, J. L.; Daly, P.; Dunlop, M.;
Ergun, R.; Friedel, R.; Fritz, T.
2002EGSGA..27.6639B Altcode:
The Cluster constellation of spacecraft have returned a wealth of new
data on particle and field variations in the near- and mid-magnetotail
regions of Earth's magnetosphere. Using the Research with Adaptive
Particle Imaging Detectors (RAPID) systems onboard the four Cluster
vehicles, we have identified substorm- related energetic (E &gt; 20 keV)
electron enhancement events during the period March 2001 through October
2001 in the geocentric radial range of 4 to 19 Earth radii. We have
used concurrent data from other Cluster instruments as well as from
the IMAGE, FAST, OPS, and geostationary orbit spacecraft in order to
understand particle injection and transport phenomena throughout this
key region of the magnetotail. One particularly striking event during
a major geomagnetic storm on 31 March 2001 showed a dispersionless
electron injection event in as close to the Earth as 4 Re. More normal
electron enhancements in the plasma sheet at intermediate radial
distances are also studied in a global substorm context.

---------------------------------------------------------
Title: Cluster observations of geomagnetic storms and of
magnetospheric substorm behavior in the near- and mid-tail regions
Authors: Baker, D.
2002cosp...34E.234B Altcode: 2002cosp.meetE.234B
The Cluster constellation of spacecraft have returned a wealth of new
data on particle and field variations in the near- and mid-magnetotail
regions of Earth's magnetosphere. Using the Research with Adaptive
Particle Imaging Detectors (RAPID) systems onboard the four Cluster
vehicles, we have identified substorm- related energetic (E &gt; 20 keV)
electron enhancement events during the period March 2001 through October
2001 in the geocentric radial range of 4 to 19 Earth radii. We have
used concurrent data from other Cluster instruments as well as from
the IMAGE, FAST, GPS, and geostationary orbit spacecraft in order to
understand particle injection and transport phenomena throughout this
key region of the magnetotail. One particularly striking event during
a major geomagnetic storm on 31 March 2001 showed a dispersionless
electron injection event in as close to the Earth as 4 Re. More normal
electron enhancements in the plasma sheet at intermediate radial
distances are also studied in a global substorm context. A particularly
well- observed substorm case occurred on August 27, 2001 when CLUSTER
was almost exactly in the midnight meridian and complementary data were
available from IMAGE, POLAR, GOES-8, and the LANL satellites. We find
evidence that CLUSTER was very near the near-Earth substorm neutral
line and that magnetic reconnection began some seven minutes prior to
the substorm auroral brightening of the expansive phase onset.

---------------------------------------------------------
Title: Energetic particle boundaries and injections during the main
phase of a major magnetic storm
Authors: Kerttula, R.; Mursula, K.; Asikainen, T.; Friedel, R.; Baker,
D.; Soeraas, F.; Daly, P.; Fritz, T.; Blake, J.; Carter, M.
2002cosp...34E2702K Altcode: 2002cosp.meetE2702K
We study energetic particle observations during the main phase of the
March 31, 2001, storm using the low-altitude NOAA satellites and the
four Cluster satellites. The NOAA satellites are used to monitor the
change of the global magnetospheric configuration. At the start of the
main phase, the polar cap boundaries extend equatorwards and energetic
particle densities in the polar cap region are reduced. The boundaries
return polewards soon after the end of the main phase. Strong injections
of energetic particles are observed during and soon after the main phase
whose development is followed by the NOAA satellite observations. Also
during the main phase, an intense population of energetic electrons is
established at very low altitudes in the equatorial region. During one
of the most intense injections at about 0640 UT, when Cluster is close
to its perigee in the post-midnight sector, the energetic particle
fluxes of the Rapid instruments are increased in two steps separated
by about 3 minutes. Using Cluster observations we will examine whether
the increases are due to spatial gradients formed after one major
injection or whether they correspond to two separate injections,
and determine the motion of the injection boundary.

---------------------------------------------------------
Title: Status of Project GRAND's Proportional Wire Chamber Array
Authors: Poirier, J.; Baker, D.; Barchie, J.; D'Andrea, C.; Dunford,
M.; Green, M.; Gress, J.; Lin, T.; Race, D.; Skibba, R.; VanLaecke,
G.; Wysocki, M.
2001astro.ph..9489P Altcode:
Project GRAND is an extensive air shower array of proportional wire
chambers. It has 64 stations in a 100m x 100m area; each station has
eight planes of proportional wire chambers with a 50 mm steel absorber
plate above the bottom two planes. This arrangement of planes, each
1.25 square meters of area, allow an angular measurement for each
track to 0.25 degrees in each of two projections. The steel absorber
plate allows a measurement of the identity of each muon track to 96%
accuracy. Two data-taking triggers allow data to be simultaneously
taken for a) extensive air showers (multiple coincidence station hits)
at about 1 Hz and b) single muons (single tracks of identified muons)
at 2000 Hz. Eight on-line computers pre-analyze the single track
data and store the results on magnetic tape in compacted form with a
minimum of computer dead-time. One additional computer reads data from
the shower triggers and records this raw data on a separate magnetic
tape with no pre-analysis.

---------------------------------------------------------
Title: Project GRAND's status: an array of proportional wire chambers
Authors: Poirier, J.; Baker, D.; Barchie, J.; D'Andrea, C.; Dunford,
M.; Green, M.; Gress, J.; Lin, T.; Race, D.; Skibba, R.; Vanlaecke,
G.; Wysocki, J.
2001ICRC....2..602P Altcode: 2001ICRC...27..602P
Project GRAND is an extensive air shower array of proportional wire
chambers. It has 64 stations in a 100 m x 100 m area; each station has
eight planes of proportional wire chambers with a 50 mm steel absorber
plate above the bottom two planes. This arrangement of planes, each 1.25
square meters of area, allow an angular measurement for each track to
0.25° in each of two projections. The steel absorber plate allows a
measurement of the identity of each muon track to 96% accuracy. Two
data-taking triggers allow data to be simultaneously taken for a)
extensive air showers (multiple coincidence station hits) at about 1
Hz and b) single muons (single tracks of identified muons) at 2000
Hz. Eight on-line computers pre-analyze the single track data and
store the results on magnetic tape in compacted form with a minimum
of computer dead-time. One additional computer reads data from the
shower triggers and records this raw data on a separate magnetic tape
with no pre-analysis.

---------------------------------------------------------
Title: Solar-Terrestrial Connection: Coupling Between Solar Wind,
Magnetosphere, Ionosphere, and Neutral Atmosphere
Authors: Baker, D.
2000eaa..bookE2239B Altcode:
The particle flux from the Sun and the magnetosphere represents a
large source of energy and ionization for the lower thermosphere and
ionosphere. The energy flux, which ranges from &lt;10-3 J m-2 s-1 to
over 0.1 J m-2 s-1, is deposited by particles with energies that range
from hundreds of eV to several hundred MeV. The intensity, spectrum,
and localization of the precipitation are functions of sol...

---------------------------------------------------------
Title: The D-CIXS X-Ray Spectrometer on ESA's SMART-1 Mission to
the Moon
Authors: Grande, M.; Browning, R.; Dunkin, S.; Parker, D.; Kent, B.;
Kellett, B.; Perry, H. C.; Swinyard, B.; Phillips, K.; Huovenin, J.;
Thomas, N.; Hughes, D.; Alleyne, H.; Grady, M.; Lundin, R.; Barabash,
S.; Baker, D.; Murray, D. C.; Guest, J.; Casanova, I.; D'Uston, C. L.;
Maurice, S.; Foing, B.; Heather, D.; Clark, E. P.; Kato, M.
2000ESASP.462...97G Altcode: 2000eum..conf...97G
No abstract at ADS

---------------------------------------------------------
Title: Lunar Elemental Composition and Investigations with D-CIXS
X-Ray Mapping Spectrometer on Smart-1
Authors: Grande, M.; Browning, R.; Waltham, N.; Kent, B.; Kellett,
B.; Perry, C. H.; Phillips, B. Swinyard K.; Huovenin, J.; Thomas,
N.; Livi, S.; Mal, U.; Hughes, D.; Alleyne, H.; Lundin, M. Grady R.;
Barabash, S.; Baker, D.; Murray, C. D.; Guest, J.; Dunkin, S. K.;
Maurice, I. Casanova S.; Foing, B.
2000LPI....31.1442G Altcode:
No abstract at ADS

---------------------------------------------------------
Title: A Multi-Spacecraft Synthesis of Relativistic Electrons in
the Inner Magnetosphere using LANL, GOES, GPS, SAMPEX, HEO and POLAR
Authors: Friedel, R. H. W.; Reeves, G.; Belian, D.; Cayton, T.;
Mouikis, C.; Korth, A.; Blake, B.; Fennell, J.; Selesnick, R.; Baker,
D.; Onsager, T.; Kanekal, S.
2000AdSpR..26...93F Altcode:
One of the Brussels Radiation Belt Workshop recommendations was the
establishment of a near-real-time data driven model of the inner
magnetospheric energetic particle population (L &lt; 8). Although the
“ideal” missions and data sets for such a model do not exist at
present, more spacecraft than ever before are currently sampling
the inner magnetosphere. We attempt here in a case study of the
January 10, 1997 magnetic cloud event to construct such a model with
the energetic electron data available from 5 geosynchronous and 5
elliptically orbiting satellites. We examine the constraints and
difficulties of putting together a large number of datasets which
are measured near-simultaneously at very different locations in the
inner magnetosphere. First results indicate that we can achieve a
time resolution of about 3 hours for a given “snapshot” of the inner
magnetosphere, and that large azimuthal asymmetries of the energetic
electron population can be observed during large storms

---------------------------------------------------------
Title: D-CIXS: Lunar investigation using the Compact X-Ray
Spectrometer on SMART-1
Authors: Grande, M.; Browning, R.; Waltham, N.; Kent, B.; Kellett,
B.; Perry, C. H.; Swinyard, B.; Phillips, K.; Huovenin, J.; Thomas,
N.; Livi, S.; Wilken, B.; Hughes, D.; Alleyne, H.; Grady, M.; Lundin,
R.; Barabash, S.; Baker, D.; Murray, C. D.; Guest, J.; Dunkin, S.
1999DPS....31.0808G Altcode:
The D-CIXS Compact X-ray Spectrometer will provide high quality
spectroscopic mapping of the Moon, the primary science target of the
SMART-1 mission. At the same time it will demonstrate a radically novel
approach to building a type of instrument essential for the Mercury
cornerstone mission. It will achieve ground breaking science within
a resource envelope far smaller than previously thought possible for
this type of instrument, using new technology which does not require
cold running, with its associated overheads to the spacecraft, and
which is radiation tolerant, essential to many potential and future
science targets. It consists of a high throughput spectrometer, which
will perform spatially localised X-ray fluorescence spectroscopy,
and a solar monitor to provide the calibration of the illumination
necessary to produce global map of absolute Lunar elemental abundances.

---------------------------------------------------------
Title: D-CIXS: lunar investigation using the compact X-Ray
spectrometer on SMART-1.
Authors: Grande, M.; Browning, R.; Waltham, N.; Kent, B.; Kellett,
B.; Perry, C. H.; Swinyard, B. M.; Phillips, K.; Huovenin, J.; Thomas,
N.; Livi, S.; Wilken, B.; Hughes, D.; Alleyne, H.; Grady, M.; Lundin,
R.; Barabash, S.; Baker, D.; Murray, C. D.; Guest, J. E.; Dunkin, S.
1999BAAS...31R1083G Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Solar-terrestrial symposium examines coupling processes
Authors: Daglis, I.; Baker, D.; Sarris, E.; Wilken, B.
1998EOSTr..79..139D Altcode:
Exploration of the space environment has revealed a dynamic and
complex system of interacting plasmas, magnetic fields, and electrical
currents. Plasma physics determines the behavior of matter in space
on spatial and temporal scales vastly different from those that
can be duplicated in Earth-based laboratories. The near-Earth space
environment has traditionally been studied as a system of independent
component parts in the interplanetary region, the magnetosphere, the
ionosphere, and the upper atmosphere. From such early explorations,
it was known that “geospace” is a complex system composed of highly
interactive parts. While previous programs advanced the understanding of
these geospace components individually, an understanding of geospace
as a whole required a planned program of simultaneous space and
ground-based observations and theoretical studies keyed to a global
assessment of the production, transfer, storage, and dissipation of
energy throughout the solar-terrestrial system. Prior understanding
of the various geospace components plus the availability of advanced
instrumentation has allowed, for the first time, a comprehensive,
quantitative study of the solar-terrestrial energy chain to be planned:
the International Solar Terrestrial Physics (ISTP) Program.

---------------------------------------------------------
Title: RAPID - The Imaging Energetic Particle Spectrometer on Cluster
Authors: Wilken, B.; Axford, W. I.; Daglis, I.; Daly, P.; Guttler, W.;
Ip, W. H.; Korth, A.; Kremser, G.; Livi, S.; Vasyliunas, V. M.; Woch,
J.; Baker, D.; Belian, R. D.; Blake, J. B.; Fennell, J. F.; Lyons,
L. R.; Borg, H.; Fritz, T. A.; Gliem, F.; Rathje, R.; Grande, M.; Hall,
D.; Kecsuemety, K.; McKenna-Lawlor, S.; Mursula, K.; Tanskanen, P.;
Pu, Z.; Sandahl, I.; Sarris, E. T.; Scholer, M.; Schulz, M.; Sorass,
F.; Ullaland, S.
1997SSRv...79..399W Altcode:
No abstract at ADS

---------------------------------------------------------
Title: The Clementine mission - initial results from Lunar mapping.
Authors: Spudis, P. D.; Shoemaker, E.; Davies, M.; Acton, C.; Burratti,
B.; Duxbury, T.; Eliason, E.; McEwen, A.; Baker, D.; Smith, D.; Lucey,
P.; Blamont, J.; Pieters, C.
1994ESASP1170...91S Altcode: 1994luna.work...91S
No abstract at ADS

---------------------------------------------------------
Title: The Clementine Mission: Initial Results from lunar mapping
Authors: Spudis, P. D.; Shoemaker, E.; Acton, C.; Burratti, B.;
Duxbury, T.; Baker, D.; Smith, D.; Blamont, J.; Davies, M.; Eliason, E.
1994STIN...9524994S Altcode:
Clementine was a mission designed to test the space-worthiness of
a variety of advanced sensors for use on military surveillance
satellites while, at the same time, gathering useful scientific
information on the composition and structure of the Moon and a
near-Earth asteroid. Conducted jointly by the Ballistic Missile
Defense Organization (BMDO, formerly the Strategic Defense Initiative
Organization) of the US Department of Defense and NASA, Clementine was
dispatched for an extended stay in the vicinity of Earth's moon on 25
January 1994 and arrived at the Moon on 20 February 1994. The spacecraft
started systematic mapping on 26 February, completed mapping on 22
April, and left lunar orbit on 3 May. The entire Clementine project,
from conception through end-of-mission, lasted approximately 3 years.

---------------------------------------------------------
Title: One Small Step for Mankind
Authors: Baker, D.
1989NewSc.123...52B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Earth-based Radio Observations of the Planet Mercury
Authors: Ledlow, M. J.; Burns, J. O.; Zhao, J. H.; Gisler, G.; Zeilik,
M.; Baker, D.
1989LPI....20..564L Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Observation of OH Meinel (7,4) P(N”=13) transitions in the
night airglow
Authors: Pendleton, W., Jr.; Espy, P.; Baker, D.; Steed, A.; Fetrow,
M.; Henriksen, K.
1989JGR....94..505P Altcode:
Improved spectral measurements of the OH Meinel Δv=3 night airglow
emissions have revealed unexpectedly intense transitions from high
rotational levels. The example selected for this communication
involves the previously unreported P(N”=13) transitions in the OH M
(7,4) band. Under the extant conditions, the column emission rates
associated with these new features exceeded by factors ~104
those expected on the basis of the assumption of rotational-kinetic
equilibrium for the v=7 rotational manifold. We present the key
observations and discuss some of the implications.

---------------------------------------------------------
Title: Book-Review - the History of Manned Space Flight
Authors: Baker, D.; Fraknoi, A.
1983Mercu..12T..91B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Book-Review - the History of Manned Space Flight
Authors: Baker, D.; Michaud, M. A. G.
1983S&T....66...30B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Astronomia.
Authors: Baker, D.
1980astr.book.....B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Book-Review - the Rocket
Authors: Baker, D.; Watts, R. N., Jr.
1980S&T....60..141B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Book-Review - Space Shuttle
Authors: Baker, D.; Michaud, M. A. G.
1980S&T....59..150B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Book-Review - Space Shuttle
Authors: Baker, D.
1980Sci...208..394B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Der Kosmos-Sternführer. Planeten, Sterne, Galaxien.
Authors: Baker, D.; Hardy, D. A.
1979dkps.book.....B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Space Shuttle.
Authors: Baker, D.
1979spsh.book.....B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: The rocket_- the history and development of rocket and
missile technology.
Authors: Baker, D.
1978rhdr.book.....B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: The Hamlyn guide to astronomy.
Authors: Baker, D.
1978hgta.book.....B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Behind the Viking scene. 4, 5.
Authors: Baker, D.
1977SpFl...19..166B Altcode:
Engineering problems encountered early in the mission of Viking Lander
1 are discussed. These include the refusal of the seismometer to
uncage itself, failure of the low-gain No. 1 receiver, and trouble in
retracting the surface-sampler boom. The way in which the boom problem
was overcome is described in detail. It is noted that the seismometer
was rendered virtually inoperable and that the low-gain receiver could
not be coaxed back into operation.

---------------------------------------------------------
Title: Near-infrared spectrum of an aurora
Authors: Baker, D.; Pendleton, W., Jr.; Steed, A.; Huppi, R.; Stair,
A. T., Jr.
1977JGR....82.1601B Altcode:
The spectrum of an aurora has been obtained at moderately high
resolution by using a wide-field interferometer-spectrometer. The
free spectral range was from 0.83 to 1.67 µm at a midrange resolving
power of about 1800. The principal auroral features observed during
an IBC III+ breakup on the night of April 19, 1974, at
Chatanika, Alaska, were the N2+ Meinel bands,
the N2 first positive bands, and certain atomic O and
N emission lines. Comparisons of the auroral spectra are made with
both high-latitude airglow and laboratory spectra taken by the same
instrument.

---------------------------------------------------------
Title: Behind the Viking scene. 1 - 3.
Authors: Baker, D.
1977SpFl...19...75B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Viking: lander science equipment - 2.
Authors: Baker, D.
1976SpFl...18..241B Altcode:
The soil collector carried aboard the Viking Mars Lander and the
instruments and procedures that will be used to investigate samples
of the surface soil of Mars are described. The collector, stored
in a collapsed, coiled configuration during flight, deploys to form
a rigid arm capable of collecting materials from 90 cm to 3 m from
the Lander itself within an azimuth arc of 120 deg. Screens limit
the passage of particles larger than 1 mm. Soil samples delivered to
the bio-lab will be subjected to pyrolytic release, labelled release,
and gas exchange tests to detect the presence of metabolic products or
of organic compounds indicative of the present or past existence of
life. The GCMS, which is capable of performing six organic tests and
up to 60 atmospheric analyses, will be used to search for compounds
in the surface soil. Inorganic chemical analyses will be performed by
an X-ray fluorescence spectrometer.

---------------------------------------------------------
Title: Viking: Orbiter science equipment.
Authors: Baker, D.
1976SpFl...18..124B Altcode:
The instrumentation aboard the Viking orbiter for obtaining a
photographic record of geological changes, high resolution imagery
of selected areas of the Martian surface, information on the
distribution of water vapor, and details on the thermal environment
is described. The spacecraft will carry two TV cameras incorporating
38 mm selenium vidicon tube, and catadioptric Cassegrain lenses. An
infrared spectrometer will detect water vapor at 1.38 micrometers. A
four-channel infrared radiometer operating at wavelengths of 6-8,
8-9.5, 9.5-13, and 18-24 microns will be used to determine surface
temperature profiles, measure atmospheric temperature, and detect
frost or condensation levels. Additional spectral bands at 0.3-3
and 16 microns will measure atmospheric temperature and planetary
albedo. Bimetallic thermocouples will measure infrared radiation in
the spectral gaps between filter settings. The aeroshell protecting the
Lander will contain a mass spectrometer, retarding potential analyzer,
and pressure and temperature sensors to measure gross characteristics
of the atmosphere of Mars.

---------------------------------------------------------
Title: Viking: lander science equipment - 1.
Authors: Baker, D.
1976SpFl...18..211B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Viking: the orbiter.
Authors: Baker, D.
1976SpFl...18...84B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Surveyor on the moon. 6.
Authors: Baker, D.
1976SpFl...18..228B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: The voyages of Viking - 3. Viking: the lander.
Authors: Baker, D.
1976SpFl...18..158B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Mariner-Venus-Mercury 1973 project history.
Authors: Baker, D.
1975SpFl...17..298B Altcode:
The significant advances made by the Mariner-Venus-Mercury 1973 project
include the gravity-assist fly-by of a second planet from the deflected
trajectory induced by a primary target, TV views of Venus, investigation
of Mercury, the planetary re-visit on a fly-by profile, and effective
manipulation of real-time planning (using solar-sailing to effect
attitude stabilization). The flight of Mariner 10 is described from
June 6, 1974, when the spacecraft had moved around the sun to superior
conjunction and the dual S-band and X-band radio signals from the
high-gain antenna passed within 1.67 deg of the solar surface as viewed
from earth, until the conclusion of the operational phase on March 24,
1975. The second and third Mercury encounters, allowed a full frontal
scan of the sunlit side plus slant-angle examination of the south pole
and transmitted images of 60% of the total surface area of Mercury.

---------------------------------------------------------
Title: Twilight transition spectra of atmospheric O2
Ir emissions
Authors: Baker, D.; Steed, A.; Huppi, R.; Baker, K.
1975GeoRL...2..235B Altcode:
Resolved spectra have been obtained from the ground of the
O2(a¹Δg) emissions from the upper atmosphere
utilizing a wide-field interferometer with a cryogenically cooled
germanium detector. The rotational structure of both the (0, 0) band at
1.27 µm and the (0, 1) band at 1.58 µm are clearly separable from the
hydroxyl airglow. The decay rate of the O2(a¹Δg)
during the twilight transition has been observed.

---------------------------------------------------------
Title: Mariner-Venus-Mercury 1973 project history. Part 2.
Authors: Baker, D.
1975SpFl...17..191B Altcode:
During December, 1973, as Mariner 10 continued on its course toward
Venus, recurrent problems were encountered with the feed system
of the spacecraft's steerable dish antenna. The final trajectory
correction maneuver, TCM-2, was accomplished on January 21, 1975, and
the spacecraft passed Venus at a distance of 3585 miles on February 5,
1974. After the TCM-3 burn on March 16, Mariner 10 passed within 460
miles of Mercury on March 29. The second Mercury encounter occurred
on September 21, 1974.

---------------------------------------------------------
Title: Mariner-Venus-Mercury 1973 project history. Part 1.
Authors: Baker, D.
1975SpFl...17..131B Altcode:
Mariner-Venus-Mercury 1973 (MVM 73) was officially endorsed by the
Space Science Board of the National Academy of Science in 1968. In
February 1970, the initial Program Authorization Document was signed
and a project office was set up. NASA plans for MVM-73 anticipated
a launch during the period from November 1 to December 15, 1973. The
actual launch took place on November 3, 1973. On November 28, Mariner
10 was 5.5 million miles from earth and 48.1 million miles from Venus.

---------------------------------------------------------
Title: A history of the Saturn I/IB launchers
Authors: Baker, D.
1975SpFl...17..146B Altcode:
Studies concerning the development of a liquid propellant booster using
a cluster of conventional rocket motors to produce a total thrust of 1.5
million pounds began in April 1957. By November 1958 four flight test
vehicles had been approved. On January 18, 1960, the Saturn project
was approved as a program of highest national priority. Attention
is given to handling problems concerning the various Saturn stages,
questions of payload capability, major changes to the Saturn C-1
program in connection with the Apollo program, the first C-1 launching
on October 27, 1961, and plans for Nova.

---------------------------------------------------------
Title: Report from Jupiter - 2.
Authors: Baker, D.
1975SpFl...17..102B Altcode:
The exploration of the planet Jupiter with the aid of the spacecraft
Pioneer 10 is discussed. Pioneer 10 had been launched on Mar. 2,
1972. The closest approach of the spacecraft to Jupiter came on Dec. 3,
1973, when Pioneer 10 passed within 81,000 miles of the cloud tops of
the gigantic planet. The journey of Pioneer 10 through the asteroid
belt is briefly reviewed and the various stages of the encounter of
the spacecraft with Jupiter are described. The characteristics of
the Jovian environment are considered along with details regarding
the Galilean satellites, the Jovian radiation belts, and the new
perspective on Jupiter obtained as a result of the Pioneer-10 data.

---------------------------------------------------------
Title: Skylab: the three month vigil. Part 3.
Authors: Baker, D.
1975SpFl...17...11B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: The Russian Venus probes.
Authors: Baker, D.
1975SpFl...17..446B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Ranger 7.
Authors: Baker, D.
1974SpFl...16..276B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Skylab: the three month vigil. II.
Authors: Baker, D.
1974SpFl...16..456B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Report from Jupiter. Part 1.
Authors: Baker, D.
1974SpFl...16..140B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: The large space telescope.
Authors: Baker, D.
1974SpFl...16....7B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Skylab: 59 days in space. Part four.
Authors: Baker, D.
1974SpFl...16..305B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Skylab: 59 days in space. Part three.
Authors: Baker, D.
1974SpFl...16..206B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Skylab: 59 days in space. Part 1, 2.
Authors: Baker, D.
1974SpFl...16...55B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Mariner 4.
Authors: Baker, D.
1974SpFl...16..418B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Skylab: the three month vigil.
Authors: Baker, D.
1974SpFl...16..412B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: The last Apollo - 1, 2, 3.
Authors: Baker, D.
1973SpFl...15...42B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Skylab - the diary of a rescue mission. Part 1.
Authors: Baker, D.
1973SpFl...15..334B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Skylab - The diary of a rescue mission. Part 2, 3.
Authors: Baker, D.
1973SpFl...15..377B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Negative Ion Composition of the D and E-Regions During a PCA
Authors: Narcisi, R. S.; Sherman, C.; Philbrick, C. R.; Thomas, D. M.;
Bailey, A. D.; Wlodyka, L. E.; Wlodyka, R. A.; Baker, D.; Federico, G.
1972spen.conf..411N Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Positive Ion Composition of the D and E-Regions During a PCA
Authors: Narcisi, R. S.; Philbrick, C. R.; Thomas, D. M.; Bailey,
A. D.; Wlodyka, L. E.; Baker, D.; Federico, G.; Wlodyka, R.; Gardner,
M. E.
1972spen.conf..421N Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Mission to Descartes - 1.
Authors: Baker, D.
1972SpFl...14..246B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Pioneers to Jupiter.
Authors: Baker, D.
1972SpFl...14..111B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Mission to Descartes - 2.
Authors: Baker, D.
1972SpFl...14..287B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Lunar roving vehicle: Design report.
Authors: Baker, D.
1971SpFl...13..234B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Space Station Situation Report - 2. The McDonnell-Douglas
proposal.
Authors: Baker, D.
1971SpFl...13..344B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Skylab.
Authors: Baker, D.
1971SpFl...13..335B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Expedition to Hadley-Apennine - 3.
Authors: Baker, D.
1971SpFl...13..468B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Apollo 14: A visit to Fra Mauro - 3.
Authors: Baker, D.
1971SpFl...13..373B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Orbitas bases. Space Station Situation Report - 1: The North
American Rockwell proposal.
Authors: Baker, D.
1971SpFl...13..318B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Apollo 14: A visit to Fra Mauro, 1, 2.
Authors: Baker, D.
1971SpFl...13..164B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: a Large Aperture, High-Resolution Field-Widened
Interferometer-Spectrometer for Airglow Studies
Authors: Despain, A.; Brown, F., Jr.; Steed, A.; Baker, D.
1971fosp.conf..293D Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Expedition to Hadley-Apennine - 1.
Authors: Baker, D.
1971SpFl...13..358B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Expedition to Hadley-Apennine - 2.
Authors: Baker, D.
1971SpFl...13..431B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: NASA explores the solar system.
Authors: Baker, D.
1971SpFl...13...42B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Apollo 11: A systems analysis.
Authors: Baker, D.
1970SpFl...12...35B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Lunar landing dust.
Authors: Baker, D.
1970SpFl...12..336B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: The Apollo spacecraft: Guidance and navigation.
Authors: Baker, D.
1969SpFl...11..386B Altcode:
No abstract at ADS