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Author name code: carlyle
ADS astronomy entries on 2022-09-14
author:"Carlyle, Jack"
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Title: Coordination within the remote sensing payload on the Solar
Orbiter mission
Authors: Auchère, F.; Andretta, V.; Antonucci, E.; Bach, N.;
Battaglia, M.; Bemporad, A.; Berghmans, D.; Buchlin, E.; Caminade,
S.; Carlsson, M.; Carlyle, J.; Cerullo, J. J.; Chamberlin, P. C.;
Colaninno, R. C.; Davila, J. M.; De Groof, A.; Etesi, L.; Fahmy,
S.; Fineschi, S.; Fludra, A.; Gilbert, H. R.; Giunta, A.; Grundy,
T.; Haberreiter, M.; Harra, L. K.; Hassler, D. M.; Hirzberger, J.;
Howard, R. A.; Hurford, G.; Kleint, L.; Kolleck, M.; Krucker, S.;
Lagg, A.; Landini, F.; Long, D. M.; Lefort, J.; Lodiot, S.; Mampaey,
B.; Maloney, S.; Marliani, F.; Martinez-Pillet, V.; McMullin, D. R.;
Müller, D.; Nicolini, G.; Orozco Suarez, D.; Pacros, A.; Pancrazzi,
M.; Parenti, S.; Peter, H.; Philippon, A.; Plunkett, S.; Rich, N.;
Rochus, P.; Rouillard, A.; Romoli, M.; Sanchez, L.; Schühle, U.;
Sidher, S.; Solanki, S. K.; Spadaro, D.; St Cyr, O. C.; Straus, T.;
Tanco, I.; Teriaca, L.; Thompson, W. T.; del Toro Iniesta, J. C.;
Verbeeck, C.; Vourlidas, A.; Watson, C.; Wiegelmann, T.; Williams,
D.; Woch, J.; Zhukov, A. N.; Zouganelis, I.
2020A&A...642A...6A Altcode:
Context. To meet the scientific objectives of the mission, the Solar
Orbiter spacecraft carries a suite of in-situ (IS) and remote sensing
(RS) instruments designed for joint operations with inter-instrument
communication capabilities. Indeed, previous missions have shown that
the Sun (imaged by the RS instruments) and the heliosphere (mainly
sampled by the IS instruments) should be considered as an integrated
system rather than separate entities. Many of the advances expected
from Solar Orbiter rely on this synergistic approach between IS and
RS measurements. <BR /> Aims: Many aspects of hardware development,
integration, testing, and operations are common to two or more
RS instruments. In this paper, we describe the coordination effort
initiated from the early mission phases by the Remote Sensing Working
Group. We review the scientific goals and challenges, and give an
overview of the technical solutions devised to successfully operate
these instruments together. <BR /> Methods: A major constraint for the
RS instruments is the limited telemetry (TM) bandwidth of the Solar
Orbiter deep-space mission compared to missions in Earth orbit. Hence,
many of the strategies developed to maximise the scientific return from
these instruments revolve around the optimisation of TM usage, relying
for example on onboard autonomy for data processing, compression,
and selection for downlink. The planning process itself has been
optimised to alleviate the dynamic nature of the targets, and an
inter-instrument communication scheme has been implemented which can
be used to autonomously alter the observing modes. We also outline the
plans for in-flight cross-calibration, which will be essential to the
joint data reduction and analysis. <BR /> Results: The RS instrument
package on Solar Orbiter will carry out comprehensive measurements
from the solar interior to the inner heliosphere. Thanks to the close
coordination between the instrument teams and the European Space
Agency, several challenges specific to the RS suite were identified
and addressed in a timely manner.
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Title: Models and data analysis tools for the Solar Orbiter mission
Authors: Rouillard, A. P.; Pinto, R. F.; Vourlidas, A.; De Groof, A.;
Thompson, W. T.; Bemporad, A.; Dolei, S.; Indurain, M.; Buchlin, E.;
Sasso, C.; Spadaro, D.; Dalmasse, K.; Hirzberger, J.; Zouganelis, I.;
Strugarek, A.; Brun, A. S.; Alexandre, M.; Berghmans, D.; Raouafi,
N. E.; Wiegelmann, T.; Pagano, P.; Arge, C. N.; Nieves-Chinchilla,
T.; Lavarra, M.; Poirier, N.; Amari, T.; Aran, A.; Andretta, V.;
Antonucci, E.; Anastasiadis, A.; Auchère, F.; Bellot Rubio, L.;
Nicula, B.; Bonnin, X.; Bouchemit, M.; Budnik, E.; Caminade, S.;
Cecconi, B.; Carlyle, J.; Cernuda, I.; Davila, J. M.; Etesi, L.;
Espinosa Lara, F.; Fedorov, A.; Fineschi, S.; Fludra, A.; Génot,
V.; Georgoulis, M. K.; Gilbert, H. R.; Giunta, A.; Gomez-Herrero, R.;
Guest, S.; Haberreiter, M.; Hassler, D.; Henney, C. J.; Howard, R. A.;
Horbury, T. S.; Janvier, M.; Jones, S. I.; Kozarev, K.; Kraaikamp,
E.; Kouloumvakos, A.; Krucker, S.; Lagg, A.; Linker, J.; Lavraud,
B.; Louarn, P.; Maksimovic, M.; Maloney, S.; Mann, G.; Masson, A.;
Müller, D.; Önel, H.; Osuna, P.; Orozco Suarez, D.; Owen, C. J.;
Papaioannou, A.; Pérez-Suárez, D.; Rodriguez-Pacheco, J.; Parenti,
S.; Pariat, E.; Peter, H.; Plunkett, S.; Pomoell, J.; Raines, J. M.;
Riethmüller, T. L.; Rich, N.; Rodriguez, L.; Romoli, M.; Sanchez,
L.; Solanki, S. K.; St Cyr, O. C.; Straus, T.; Susino, R.; Teriaca,
L.; del Toro Iniesta, J. C.; Ventura, R.; Verbeeck, C.; Vilmer, N.;
Warmuth, A.; Walsh, A. P.; Watson, C.; Williams, D.; Wu, Y.; Zhukov,
A. N.
2020A&A...642A...2R Altcode:
Context. The Solar Orbiter spacecraft will be equipped with a wide
range of remote-sensing (RS) and in situ (IS) instruments to record
novel and unprecedented measurements of the solar atmosphere and
the inner heliosphere. To take full advantage of these new datasets,
tools and techniques must be developed to ease multi-instrument and
multi-spacecraft studies. In particular the currently inaccessible
low solar corona below two solar radii can only be observed
remotely. Furthermore techniques must be used to retrieve coronal
plasma properties in time and in three dimensional (3D) space. Solar
Orbiter will run complex observation campaigns that provide interesting
opportunities to maximise the likelihood of linking IS data to their
source region near the Sun. Several RS instruments can be directed
to specific targets situated on the solar disk just days before
data acquisition. To compare IS and RS, data we must improve our
understanding of how heliospheric probes magnetically connect to the
solar disk. <BR /> Aims: The aim of the present paper is to briefly
review how the current modelling of the Sun and its atmosphere
can support Solar Orbiter science. We describe the results of a
community-led effort by European Space Agency's Modelling and Data
Analysis Working Group (MADAWG) to develop different models, tools,
and techniques deemed necessary to test different theories for the
physical processes that may occur in the solar plasma. The focus here
is on the large scales and little is described with regards to kinetic
processes. To exploit future IS and RS data fully, many techniques have
been adapted to model the evolving 3D solar magneto-plasma from the
solar interior to the solar wind. A particular focus in the paper is
placed on techniques that can estimate how Solar Orbiter will connect
magnetically through the complex coronal magnetic fields to various
photospheric and coronal features in support of spacecraft operations
and future scientific studies. <BR /> Methods: Recent missions such as
STEREO, provided great opportunities for RS, IS, and multi-spacecraft
studies. We summarise the achievements and highlight the challenges
faced during these investigations, many of which motivated the Solar
Orbiter mission. We present the new tools and techniques developed
by the MADAWG to support the science operations and the analysis of
the data from the many instruments on Solar Orbiter. <BR /> Results:
This article reviews current modelling and tool developments that ease
the comparison of model results with RS and IS data made available
by current and upcoming missions. It also describes the modelling
strategy to support the science operations and subsequent exploitation
of Solar Orbiter data in order to maximise the scientific output
of the mission. <BR /> Conclusions: The on-going community effort
presented in this paper has provided new models and tools necessary
to support mission operations as well as the science exploitation of
the Solar Orbiter data. The tools and techniques will no doubt evolve
significantly as we refine our procedure and methodology during the
first year of operations of this highly promising mission.
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Title: Understanding the Role of Mass-Unloading in a Filament Eruption
Authors: Jenkins, Jack; Long, David; van Driel-Gesztelyi, Lidia;
Carlyle, Jack; Hopwood, Matthew
2018csc..confE..17J Altcode:
We combine observations of a partial filament eruption on 11
December 2011 with a simple line-current model to demonstrate
that including mass is an important next step for understanding
solar eruptions. Observations from the Solar Terrestrial Relations
Observatory-Behind (STEREO-B) and the Solar Dynamics Observatory (SDO)
spacecraft were used to remove line-of-sight projection effects in
filament motion and correlate the effect of plasma dynamics with
the evolution of the filament height. The two viewpoints enable
the amount of mass drained to be estimated, and an investigation of
the subsequent radial expansion and eruption of the filament. We use
these observational measurements to constrain a line-current model and
quantitatively demonstrate the important role that the presence and
draining of mass has in the lead-up to solar eruptions. Specifically,
we show that the balance of magnetic and gravitational forces acting
on the line-current is increasingly sensitive to mass perturbations
as it approaches its loss-of-equilibrium. Finally, we conclude that
the eruption of the observed filament was restrained until 70% of the
mass had drained from the structure.
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Title: Understanding the Role of Mass-Unloading in a Filament Eruption
Authors: Jenkins, Jack Michael; Long, David; van Driel-Gesztelyi,
Lidia; Carlyle, Jack
2018tess.conf10907J Altcode:
Solar filaments are persistent features on the solar surface,
lasting from days to months before either successfully erupting into
the heliosphere as part of a CME, or collapsing and returning the
suspended plasma to the chromosphere. To date, the consensus has
been that the plasma comprising the filament plays no significant
role in the global evolution of the host flux rope. As a result,
little effort has been made to quantify the impact that mass has on
the evolution of magnetic structures in the solar atmosphere. Here we
present observations and analysis that suggest that the inclusion of
mass is an important next step to fully understand solar eruptions. A
partial filament eruption that occurred on 11 December 2011 was
observed by both the Solar Terrestrial Relations Observatory-Behind
(STEREO-B) and the Solar Dynamics Observatory (SDO) spacecraft. The
combination of multiple perspectives from different locations within
the heliosphere allowed the removal of line-of-sight projection
effects, and the correlation of plasma dynamics to the evolution in
filament height. Our results show that 70\% of the measurable filament
mass drained shortly \textit{prior} to a change in the height--time
expansion profile of the remaining filament material from a shallow
to steeper exponential. A proxy was then formulated to test whether
the observed mass-unloading was responsible for this observed change
in behaviour. This proxy is defined as the ratio between the upward
force supplied to the host flux rope due to this mass-unloading and
the restraining force caused by the tension of the overlying magnetic
field. A ratio range of between 1.8 and 4.1 was found, indicating that
the upward force as a result of the the mass-unloading dominated the
evolution. We conclude that the unloading of filament mass from the
host flux rope was likely responsible for the accelerated expansion.
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Title: Understanding the Role of Mass-Unloading in a Filament Eruption
Authors: Jenkins, J. M.; Long, D. M.; van Driel-Gesztelyi, L.;
Carlyle, J.
2018SoPh..293....7J Altcode: 2017arXiv171102565J
We describe a partial filament eruption on 11 December 2011 that
demonstrates that the inclusion of mass is an important next step for
understanding solar eruptions. Observations from the Solar Terrestrial
Relations Observatory-Behind (STEREO-B) and the Solar Dynamics
Observatory (SDO) spacecraft were used to remove line-of-sight
projection effects in filament motion and correlate the effect
of plasma dynamics with the evolution of the filament height. Flux
cancellation and nearby flux emergence are shown to have played a role
in increasing the height of the filament prior to eruption. The two
viewpoints allow the quantitative estimation of a large mass-unloading,
the subsequent radial expansion, and the eruption of the filament to be
investigated. A 1.8 to 4.1 lower-limit ratio between gravitational and
magnetic-tension forces was found. We therefore conclude that following
the loss-of-equilibrium of the flux-rope, the radial expansion of
the flux-rope was restrained by the filamentary material until 70%
of the mass had evacuated the structure through mass-unloading.
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Title: The non-linear growth of the magnetic Rayleigh-Taylor
instability
Authors: Carlyle, Jack; Hillier, Andrew
2017A&A...605A.101C Altcode: 2017arXiv170707987C
This work examines the effect of the embedded magnetic field strength on
the non-linear development of the magnetic Rayleigh-Taylor instability
(RTI) (with a field-aligned interface) in an ideal gas close to the
incompressible limit in three dimensions. Numerical experiments are
conducted in a domain sufficiently large so as to allow the predicted
critical modes to develop in a physically realistic manner. The ratio
between gravity, which drives the instability in this case (as well
as in several of the corresponding observations), and magnetic field
strength is taken up to a ratio which accurately reflects that of
observed astrophysical plasma, in order to allow comparison between the
results of the simulations and the observational data which served as
inspiration for this work. This study finds reduced non-linear growth
of the rising bubbles of the RTI for stronger magnetic fields, and that
this is directly due to the change in magnetic field strength, rather
than the indirect effect of altering characteristic length scales with
respect to domain size. By examining the growth of the falling spikes,
the growth rate appears to be enhanced for the strongest magnetic field
strengths, suggesting that rather than affecting the development of the
system as a whole, increased magnetic field strengths in fact introduce
an asymmetry to the system. Further investigation of this effect
also revealed that the greater this asymmetry, the less efficiently
the gravitational energy is released. By better understanding the
under-studied regime of such a major phenomenon in astrophysics,
deeper explanations for observations may be sought, and this work
illustrates that the strength of magnetic fields in astrophysical
plasmas influences observed RTI in subtle and complex ways.
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Title: The 2015 St Patrick's Day Storm: Origins
Authors: Carlyle, Jack; van Driel-Gesztelyi, Lidia; Zuccarello,
Francesco; James, Alexander; Williams, David
2017SPD....4840402C Altcode:
The magnetic storm experienced at Earth on St. Patrick's Day 2015 had
been the strongest of cycle 24 (at that time) with a measured DST of
-223 nT, though it was not expected to cause much of a disturbance. In
this work we study the solar source region of several peculiar
eruptions, leading to the formation and destruction of various
structures, in the week leading up to the storm, and determine the
true sequence of events. The evolution of the magnetic flux at the
solar surface is examined in order to place suspected flux-ropes
into context, and the evolution of the magnetic connectivities
is described alongside a PFSS model of the surrounding region. The
balance between positive and negative flux directly before two key
eruptions is investigated in detail, in order to ascertain whether
particular trigger mechanisms are feasible explanations. As well as
these magnetic investigations, the column density of plasma involved
is calculated from extreme ultraviolet images, and this is used to
estimate the total mass of one filament, as well as select other
features relevant to the eruptions. This information is then used to
comment on the energy budgets and requirements of several processes in
order to best understand the underlying drivers of this event.Previous
studies on the St. Patrick's Day Storm are also incorporated into this
work, and an attempt is made to reconcile the disparate conclusions
drawn by the scientific community as to why this storm was not only
so effective, but also a major forecasting failure.
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Title: Mass Diagnostics of Eruptive Filament Material
Authors: Carlyle, Jack
2016usc..confE..19C Altcode:
Filament eruptions are not only breathtakingly beautiful, but also key
to our understanding of the variable environment which is the solar
atmosphere. From the distribution of the material and internal density
structure, it is possible to learn about the associated magnetic field
which drives the transient activity in the corona, and knowledge of the
total mass can answer questions regarding the kinetic energy of coronal
mass ejections (CMEs). My research centers around the development
of a technique which uses multi-wavelength EUV images from SDO/AIA
to determine the mass of any plasma which appears in absorption, as
filaments and associated eruptions frequently do. This method is being
continuously developed to not only increase the accuracy of results,
but also to widen its applicability to a broader spectrum of data
(figuratively and literally). I show how I have successfully examined
several events using this technique, particularly focusing on partially
failed eruptions. I also demonstrate how is possible to use these
results to further analyse the material, for example, by constraining
numerical experiments which aim to recreate observed plasma instability.
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Title: Mass and magnetic field of eruptive solar filaments
Authors: Carlyle, Jack
2016PhDT.......335C Altcode:
No abstract at ADS
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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 (10<SUP>10</SUP> cm<SUP>-3</SUP>) 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.
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Title: Investigating the Dynamics and Density Evolution of Returning
Plasma Blobs from the 2011 June 7 Eruption
Authors: Carlyle, Jack; Williams, David R.; van Driel-Gesztelyi,
Lidia; Innes, Davina; Hillier, Andrew; Matthews, Sarah
2014ApJ...782...87C Altcode: 2014arXiv1401.4824C
This work examines in-falling matter following an enormous coronal mass
ejection on 2011 June 7. The material formed discrete concentrations,
or blobs, in the corona and fell back to the surface, appearing as dark
clouds against the bright corona. In this work we examined the density
and dynamic evolution of these blobs in order to formally assess the
intriguing morphology displayed throughout their descent. The blobs
were studied in five wavelengths (94, 131, 171, 193, and 211 Å)
using the Solar Dynamics Observatory Atmospheric Imaging Assembly,
comparing background emission to attenuated emission as a function
of wavelength to calculate column densities across the descent of
four separate blobs. We found the material to have a column density of
hydrogen of approximately 2 × 10<SUP>19</SUP> cm<SUP>-2</SUP>, which is
comparable with typical pre-eruption filament column densities. Repeated
splitting of the returning material is seen in a manner consistent
with the Rayleigh-Taylor instability. Furthermore, the observed
distribution of density and its evolution is also a signature of this
instability. By approximating the three-dimensional geometry (with data
from STEREO-A), volumetric densities were found to be approximately 2
× 10<SUP>-14</SUP> g cm<SUP>-3</SUP>, and this, along with observed
dominant length scales of the instability, was used to infer a magnetic
field of the order 1 G associated with the descending blobs.
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Title: Density evolution of in-falling prominence material from the
7th June 2011 CME
Authors: Carlyle, Jack; Williams, David; van Driel-Gesztelyi, Lidia;
Innes, Davina
2014IAUS..300..401C Altcode:
This work investigates the density of in-falling prominence material
following the 7 <SUP>th</SUP> June 2011 eruption. Both the evolution
and the distribution of the density is analysed in five discreet
“blobs” of material. The density appears to be remarkably uniform,
both spatially within the blobs, and temporally over the course of the
descent of each, although a slight concentration of material towards
the leading edge is noted in some cases. Online material is available
at bit.ly/jackblob
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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.
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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.
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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.
