explanation      blue bibcodes open ADS page with paths to full text
Author name code: reid
ADS astronomy entries on 2022-09-14
author:"Reid, Aaron" 

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Title: Constraining the magnetic vector in the quiet solar photosphere
    and the impact of instrumental degradation
Authors: Campbell, R. J.; Shelyag, S.; Quintero Noda, C.; Mathioudakis,
   M.; Keys, P. H.; Reid, A.
2021A&A...654A..11C    Altcode: 2021arXiv210701519C
  Context. With the advent of next generation high resolution telescopes,
  our understanding of how the magnetic field is organized in the
  internetwork (IN) photosphere is likely to advance significantly. <BR />
  Aims: We aim to evaluate the extent to which we can retrieve accurate
  information about the magnetic vector in the IN photosphere using
  inversion techniques. <BR /> Methods: We use a snapshot produced from
  high resolution three-dimensional magnetohydrodynamic (MHD) simulations
  and employ the Stokes Inversions based on Response functions (SIR) code
  to produce synthetic observables in the same near infrared spectral
  window as observed by the GREGOR Infrared Spectrograph (GRIS), which
  contains the highly magnetically sensitive photospheric Fe I line pair
  at 15 648.52 Å and 15 652.87 Å. We then use a parallelized wrapper to
  SIR to perform nearly 14 million inversions of the synthetic spectra to
  test how well the `true' MHD atmospheric parameters can be constrained
  statistically. Finally, we degrade the synthetic Stokes vector
  spectrally and spatially to GREGOR resolutions and examine how this
  influences real observations, considering the impact of stray light,
  spatial resolution and signal-to-noise (S/N) in particular. <BR />
  Results: We find that the depth-averaged parameters can be recovered
  by the inversions of the undegraded profiles, and by adding simple
  gradients to magnetic field strength, inclination, and line of sight
  velocity we show that an improvement in the χ<SUP>2</SUP> value
  is achieved. We also evaluate the extent to which we can constrain
  these parameters at various optical depths, with the kinematic and
  thermodynamic parameters sensitive deeper in the atmosphere than
  the magnetic parameters. We find the S/N and spatial resolution both
  play a significant role in determining how the degraded atmosphere
  appears. At the same time, we find that the magnetic and kinematic
  parameters are invariant upon inclusion of an unpolarized stray
  light. We compare our results to recent IN observations obtained
  by GREGOR. We studied a linear polarization feature which resembles
  those recently observed by GRIS in terms of appearing as `loop-like'
  structures and exhibiting very similar magnetic flux density. Thus,
  we demonstrate that realistic MHD simulations are capable of showing
  close agreement with real observations, and the symbiosis between them
  and observations continues to prove essential. We finally discuss the
  considerations that must be made for DKIST-era observations.

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Title: Flare-induced Sunquake Signatures in the Ultraviolet as
    Observed by the Atmospheric Imaging Assembly
Authors: Quinn, Sean; Mathioudakis, Mihalis; Nelson, Christopher J.;
   Milligan, Ryan O.; Reid, Aaron; Jess, David B.
2021ApJ...920...25Q    Altcode: 2021arXiv210505704Q
  Sunquakes (SQs) have been routinely observed in the solar photosphere,
  but it is only recently that signatures of these events have been
  detected in the chromosphere. We investigate whether signatures of
  SQs are common in ultraviolet (UV) continua that sample the solar
  plasma several hundred km above where SQs are typically detected. We
  analyze observations from the Solar Dynamics Observatory's Atmospheric
  Imaging Assembly (SDO/AIA) 1600 and 1700 Å passbands, for SQ signatures
  induced by the flares of Solar Cycle 24. We base our analysis on the
  62 SQs detected in the recent statistical study presented by Sharykin
  &amp; Kosovichev. We find that 9 out of 62 SQ candidates produced a
  response that is clearly detected in running-difference images from
  the AIA 1600 and 1700 Å channels. A binary frequency filter with a
  width of 2 mHz, centered on 6 mHz, was applied to the data. The first
  signature of each SQ was detected at distances between 5.2 and 25.7
  Mm from the associated flare ribbon. Time-distance and regression
  analysis allowed us to calculate the apparent transverse velocities
  of the SQs in the UV data sets and found maximum velocities as high
  as 41 km s<SUP>-1</SUP>, 87 Mm away from the SQ source. Our analysis
  shows that flare-induced SQ signatures can be detected in the SDO/AIA
  1600 and 1700 Å passbands, hinting at their presence in the lower
  chromosphere. There was no apparent correlation between GOES flare
  classification and the appearance of the SQ at these heights.

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Title: Temporal evolution of small-scale internetwork magnetic fields
    in the solar photosphere (Corrigendum)
Authors: Campbell, R. J.; Mathioudakis, M.; Collados, M.; Keys, P. H.;
   Asensio Ramos, A.; Nelson, C. J.; Kuridze, D.; Reid, A.
2021A&A...652C...2C    Altcode:
  No abstract at ADS

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Title: Flare-induced Photospheric Velocity Diagnostics
Authors: Monson, Aaron J.; Mathioudakis, Mihalis; Reid, Aaron;
   Milligan, Ryan; Kuridze, David
2021ApJ...915...16M    Altcode: 2021arXiv210502199M
  We present radiative-hydrodynamic simulations of solar flares generated
  by the RADYN and RH codes to study the perturbations induced in
  photospheric Fe I lines by electron beam heating. We investigate how
  variations in the beam parameters result in discernible differences
  in the induced photospheric velocities. Line synthesis revealed a
  significant chromospheric contribution to the line profiles resulting
  in an apparent red asymmetry by as much as 40 m s<SUP>-1</SUP> close
  to the time of maximum beam heating, which was not reflective of the
  upflow velocities that arose from the radiative-hydrodynamic simulations
  at those times. The apparent redshift to the overall line profile was
  produced by significant chromospheric emission that was blueshifted
  by as much as 400 m s<SUP>-1</SUP> and fills in the blue side of
  the near-stationary photospheric absorption profile. The velocity
  information that can be retrieved from photospheric line profiles during
  flares must therefore be treated with care to mitigate the effects of
  higher parts of the atmosphere providing an erroneous velocity signal.

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Title: Temporal evolution of small-scale internetwork magnetic fields
    in the solar photosphere
Authors: Campbell, R. J.; Mathioudakis, M.; Collados, M.; Keys, P. H.;
   Asensio Ramos, A.; Nelson, C. J.; Kuridze, D.; Reid, A.
2021A&A...647A.182C    Altcode: 2021arXiv210200942C
  Context. While the longitudinal field that dominates in photospheric
  network regions has been studied extensively, small-scale transverse
  fields have recently been found to be ubiquitous in the quiet
  internetwork photosphere and this merits further study. Furthermore,
  few observations have been able to capture how this field evolves. <BR
  /> Aims: We aim to statistically characterize the magnetic vector in
  a quiet Sun internetwork region and observe the temporal evolution of
  specific small-scale magnetic features. <BR /> Methods: We present
  two high spatio-temporal resolution observations that reveal the
  dynamics of two disk-centre internetwork regions taken by the new GREGOR
  Infrared Spectrograph Integral Field Unit with the highly magnetically
  sensitive photospheric Fe I line pair at 15648.52 Å and 15652.87
  Å. We record the full Stokes vector and apply inversions with the
  Stokes inversions based on response functions code to retrieve the
  parameters characterizing the atmosphere. We consider two inversion
  schemes: scheme 1 (S1), where a magnetic atmosphere is embedded in
  a field free medium, and scheme 2 (S2), with two magnetic models
  and a fixed 30% stray light component. <BR /> Results: The magnetic
  properties produced from S1 inversions returned a median magnetic
  field strength of 200 and 240 G for the two datasets, respectively. We
  consider the median transverse (horizontal) component, among pixels
  with Stokes Q or U, and the median unsigned longitudinal (vertical)
  component, among pixels with Stokes V, above a noise threshold. We
  determined the former to be 263 G and 267 G, and the latter to be 131
  G and 145 G, for the two datasets, respectively. Finally, we present
  three regions of interest, tracking the dynamics of small-scale magnetic
  features. We apply S1 and S2 inversions to specific profiles of interest
  and find that the latter produces better approximations when there is
  evidence of mixed polarities. We find patches of linear polarization
  with magnetic flux density of the order of 130−150 G and find that
  linear polarization appears preferentially at granule-intergranular
  lane boundaries. The weak magnetic field appears to be organized in
  terms of complex `loop-like' structures, with transverse fields often
  flanked by opposite polarity longitudinal fields.

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Title: Nonthermal electrons revealed by LOFAR
Authors: Zucca, Pietro; Pellizzoni, Alberto; Krankowski, Andrzej;
   Rothkaehl, Hanna; Mann, Gottfried; Vocks, Christian; Magdalenic,
   Jasmina; Marque, Christophe; Jackson, Bernard; Fallows, Richard;
   Tomasik, Lukasz; Hamish; Reid, A. S.; Gallagher, Peter; Vourlidas,
   Angelos; Bisi, Mario M.; Carley, Eoin; Matyjasiak, Barbara; Kozarev,
   Kamen; Dabrowski, Bartosz; Morosan, Diana; Tiburzi, Caterina; Chang,
   Peijin
2021cosp...43E1065Z    Altcode:
  During solar flares and CMEs, the corona is heated, plasma motion,
  waves and shocks are ignited, and particles are accelerated. The
  accelerated particles propagate through the solar corona causing a
  variety of plasma instabilities that lead to enhanced non-thermal
  radio emission, known as "radio bursts". By studying radio-bursts'
  characteristics we can gain insight into the properties of energetic
  particles and the ambient coronal plasma, and the properties of particle
  acceleration mechanisms, such as magnetic reconnection and/or shocks
  in the solar atmosphere. The Low Frequency aRray (LOFAR) can be used
  to study the fundamental plasma physics of solar radio bursts with
  unprecedented time resolution in dynamic spectra, as well as with
  both interferometric imaging and tied array imaging. In this talk, an
  overview of recent results obtained with the LOFAR telescope will be
  given, including observations of a different variety of radio bursts
  such as type II, III and IV. These observations were performed with
  simultaneous beam formed and interferometric imaging, resulting in
  unprecedented special resolution with baselines up to ~120 km. Finally,
  we will present the plan for future observations and the remaining
  challenges of solar-heliospheric low-frequency observations.

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Title: Results from the LOFAR coordination with PSP
Authors: Zucca, Pietro; Pellizzoni, Alberto; Krankowski, Andrzej;
   Rothkaehl, Hanna; Mann, Gottfried; Vocks, Christian; Magdalenic,
   Jasmina; Marque, Christophe; Jackson, Bernard; Fallows, Richard;
   Tomasik, Lukasz; Miteva, Rositsa; Hamish; Reid, A. S.; Gallagher,
   Peter; Vourlidas, Angelos; Bisi, Mario M.; Carley, Eoin; Matyjasiak,
   Barbara; Kozarev, Kamen; Dabrowski, Bartosz; Morosan, Diana; Tiburzi,
   Caterina; Zhabngm, Peijin
2021cosp...43E.945Z    Altcode:
  Understanding and modelling the complex state of the Sun-solar
  wind-magnetosphere-ionosphere-thermosphere system, requires a
  comprehensive set of multiwavelength observations. LOFAR has unique
  capabilities in the radio domain. Some examples of these include: a)
  the ability to take high-resolution solar dynamic spectra and radio
  images of the Sun; b) observing the scintillation (interplanetary
  scintillation - IPS) of distant, compact, astronomical radio sources
  to determine the density, velocity and turbulence structure of the
  solar wind; and c) the use of Faraday rotation as a tool to probe
  the interplanetary magnetic-field strength and direction. However, to
  better understand and predict how the Sun, its atmosphere, and more
  in general the Heliosphere works and impacts Earth, the combination
  of in-situ spacecraft measurements and ground-based remote-sensing
  observations of coronal and heliospheric plasma parameters is extremely
  useful. Ground-based observations can be used to infer a global
  picture of the inner heliosphere, providing the essential context into
  which in-situ measurements from spacecraft can be placed. Conversely,
  remote-sensing observations usually contain information from extended
  lines of sight, with some deconvolution and modelling necessary to build
  up a three-dimensional (3-D) picture. Precise spacecraft measurements,
  when calibrated, can provide ground truth to constrain these models. The
  PSP mission is observing the solar corona and near-Sun interplanetary
  space. It has a highly-elliptical orbit taking the spacecraft as close
  as nearly 36 solar radii from the Sun centre on its first perihelion
  passage, and subsequent passages ultimately reaching as close as 9.8
  solar radii. Four instruments are on the spacecraft's payload: FIELDS
  measuring the radio emission, electric and magnetic fields, Poynting
  flux, and plasma waves as well as the electron density and temperature;
  ISOIS measuring energetic electrons, protons, and heavy ions in the
  energy range 10 keV-100 MeV; SWEAP measuring the density, temperature,
  and flow speed of electrons, protons, and alphas in the solar wind;
  and finally, WISPR imaging coronal streamers, coronal mass ejections
  (CMEs), their associated shocks, and other solar wind structures in the
  corona and near-Sun interplanetary space, and provide context for the
  other three in-situ instruments. In this talk, several results of the
  joint LOFAR/PSP campaign will be presented, including fine structures
  of radio bursts, localization and kinematics of propagating radio
  sources in the heliosphere, and the challenges and plans for future
  observing campaigns including PSP and Solar Orbiter.

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Title: Non-LTE inversions of a confined X2.2 flare. I. The vector
    magnetic field in the photosphere and chromosphere
Authors: Vissers, G. J. M.; Danilovic, S.; de la Cruz Rodríguez,
   J.; Leenaarts, J.; Morosin, R.; Díaz Baso, C. J.; Reid, A.; Pomoell,
   J.; Price, D. J.; Inoue, S.
2021A&A...645A...1V    Altcode: 2020arXiv200901537V
  Context. Obtaining an accurate measurement of magnetic field vector
  in the solar atmosphere is essential for studying changes in field
  topology during flares and reliably modelling space weather. <BR />
  Aims: We tackle this problem by applying various inversion methods to a
  confined X2.2 flare that occurred in NOAA AR 12673 on 6 September 2017
  and comparing the photospheric and chromospheric magnetic field vector
  with the results of two numerical models of this event. <BR /> Methods:
  We obtained the photospheric magnetic field from Milne-Eddington
  and (non-)local thermal equilibrium (non-LTE) inversions of Hinode
  SOT/SP Fe I 6301.5 Å and 6302.5 Å. The chromospheric field was
  obtained from a spatially regularised weak-field approximation (WFA)
  and non-LTE inversions of Ca II 8542 Å observed with CRISP at the
  Swedish 1 m Solar Telescope. We investigated the field strengths
  and photosphere-to-chromosphere shear in the field vector. <BR />
  Results: The LTE- and non-LTE-inferred photospheric magnetic field
  components are strongly correlated across several optical depths in
  the atmosphere, with a tendency towards a stronger field and higher
  temperatures in the non-LTE inversions. For the chromospheric field,
  the non-LTE inversions correlate well with the spatially regularised
  WFA, especially in terms of the line-of-sight field strength and field
  vector orientation. The photosphere exhibits coherent strong-field
  patches of over 4.5 kG, co-located with similar concentrations
  exceeding 3 kG in the chromosphere. The obtained field strengths
  are up to two to three times higher than in the numerical models,
  while the photosphere-to-chromosphere shear close to the polarity
  inversion line is more concentrated and structured. <BR /> Conclusions:
  In the photosphere, the assumption of LTE for Fe I line formation
  does not yield significantly different magnetic field results in
  comparison to the non-LTE case, while Milne-Eddington inversions
  fail to reproduce the magnetic field vector orientation where Fe
  I is in emission. In the chromosphere, the non-LTE-inferred field
  is excellently approximated by the spatially regularised WFA. Our
  inversions confirm the locations of flux rope footpoints that have
  been predicted by numerical models. However, pre-processing and lower
  spatial resolution lead to weaker and smoother field in the models than
  what our data indicate. This highlights the need for higher spatial
  resolution in the models to better constrain pre-eruptive flux ropes.

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Title: An Introduction to Photospheric Flare Line Diagnostics
Authors: Monson, A.; Mathioudakis, M.; Milligan, R.; Reid, A.;
   Kuridze, D.
2020AGUFMSH057..04M    Altcode:
  In preparation for solar cycle 25, we present radiative hydrodynamic
  flare models from the F-CHROMA archive constructed using the RADYN and
  RH codes. We simulate potential observable perturbations seen in the
  line-of-sight velocity and heating induced in the photosphere during
  a flare. Many works have focused on the recreation of chromospheric
  spectral line profiles as the atmosphere rapidly heats and expands
  due to the injection of energy from magnetic reconnection. This
  extreme heating mechanism can permeate through the upper atmosphere
  and affect the lowest levels of the solar atmosphere. This results
  in an observable brightening and Doppler shifting of spectral lines
  formed in the deepest regions, though the extent of this photospheric
  reaction is still not fully characterised. We investigate how variations
  in the properties of a solar flare-accelerated electron beam result in
  discernible asymmetries in the flaring profiles of several deep forming
  Fe I spectral lines. Through analysis of the contribution functions
  and response functions of these lines during a flare, we have found
  an unprecedented level of high velocity chromospheric contribution
  which significantly alters the emergent profile of these lines. This
  comparatively weak, high velocity surplus contributing region of
  the chromosphere can result in false red shifts and/or significantly
  adds to the flaring Doppler shifted profile, resulting in a greater
  blue shift of the line core, which had previously been assumed as a
  purely photospheric velocity diagnostic. Based on this evidence, it
  is concluded that any future work using these photospheric lines to
  diagnose properties of the photosphere in a flaring atmosphere must
  be carefully analysed to mitigate effect of higher forming regions
  providing a surplus velocity signal.

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Title: Chromospheric Bubbles in Solar Flares
Authors: Reid, A.; Zhigulin, B.; Carlsson, M.; Mathioudakis, M.
2020ApJ...894L..21R    Altcode: 2020arXiv200510586R
  We analyze a grid of radiative hydrodynamic simulations of solar flares
  to study the energy balance and response of the atmosphere to nonthermal
  electron beam heating. The appearance of chromospheric bubbles is one
  of the most notable features that we find in the simulations. These
  pockets of chromospheric plasma get trapped between the transition
  region and the lower atmosphere as it is superheated by the particle
  beam. The chromospheric bubbles are seen in the synthetic spectra,
  appearing as an additional component to Balmer line profiles with high
  Doppler velocities as high as 200 km s<SUP>-1</SUP>. Their signatures
  are also visible in the wings of Ca II 8542 Å line profiles. These
  bubbles of chromospheric plasma are driven upward by a wave front that
  is induced by the shock of energy deposition, and require a specific
  heating rate and atmospheric location to manifest.

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Title: Internal consistency of neutron coherent scattering length
    measurements from neutron interferometry and from neutron gravity
    reflectometry
Authors: Snow, W. M.; Apanavicius, J.; Dickerson, K. A.; Devaney,
   J. S.; Drabek, H.; Reid, A.; Shen, B.; Woo, J.; Haddock, C.; Alexeev,
   E.; Peters, M.
2020PhRvD.101f2004S    Altcode: 2019arXiv191014271S
  Many theories beyond the Standard Model postulate short-range
  modifications to gravity which produce deviations of Newton's
  gravitational potential from a strict 1 /r dependence. It is common to
  analyze experiments searching for these modifications using a potential
  of the form V<SUP>'</SUP>(r )=-G/M m r [1 +α exp (-r /λ ) ] . The best
  present constraints on α for λ &lt;100 nm come from neutron scattering
  and often employ comparisons of different measurements of the coherent
  neutron scattering amplitudes b . We analyze the internal consistency
  of existing data from two different types of measurements of low-energy
  neutron scattering amplitudes: neutron interferometry, which involves
  squared momentum transfers q<SUP>2</SUP>=0 , and neutron gravity
  reflectometry, which involves squared momentum transfers q<SUP>2</SUP>=8
  m V<SUB>opt</SUB> where m is the neutron mass and V<SUB>opt</SUB>
  is the neutron optical potential of the medium. We show that the
  fractional difference Δ/b |b | averaged over the seven elements where
  high precision data exist on the same material from both measurement
  methods is [2.2 ±1.4 ]×10<SUP>-4</SUP>. We also show that Δ/b |b |
  for these data is insensitive both to exotic Yukawa interactions and
  also to the electromagnetic neutron-atom interactions proportional to
  the neutron-electron scattering length b<SUB>n e</SUB> and the neutron
  polarizability scattering amplitude b<SUB>pol</SUB>. This result will
  be useful in any future global analyses of neutron scattering data
  to determine b<SUB>n e</SUB> and bound α and λ . We also discuss
  how various neutron interferometric and scattering techniques with
  cold and ultracold neutrons can be used to improve the precision of
  b measurements and make some specific proposals.

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Title: High-resolution spectropolarimetric observations of the
    temporal evolution of magnetic fields in photospheric bright points
Authors: Keys, P. H.; Reid, A.; Mathioudakis, M.; Shelyag, S.;
   Henriques, V. M. J.; Hewitt, R. L.; Del Moro, D.; Jafarzadeh, S.;
   Jess, D. B.; Stangalini, M.
2020A&A...633A..60K    Altcode: 2019arXiv191108436K
  Context. Magnetic bright points (MBPs) are dynamic, small-scale
  magnetic elements often found with field strengths of the order of a
  kilogauss within intergranular lanes in the photosphere. <BR /> Aims:
  Here we study the evolution of various physical properties inferred from
  inverting high-resolution full Stokes spectropolarimetry data obtained
  from ground-based observations of the quiet Sun at disc centre. <BR
  /> Methods: Using automated feature-tracking algorithms, we studied
  300 MBPs and analysed their temporal evolution as they evolved to
  kilogauss field strengths. These properties were inferred using
  both the NICOLE and SIR Stokes inversion codes. We employ similar
  techniques to study radiative magnetohydrodynamical simulations
  for comparison with our observations. <BR /> Results: Evidence was
  found for fast (∼30-100 s) amplification of magnetic field strength
  (by a factor of 2 on average) in MBPs during their evolution in our
  observations. Similar evidence for the amplification of fields is seen
  in our simulated data. <BR /> Conclusions: Several reasons for the
  amplifications were established, namely, strong downflows preceding
  the amplification (convective collapse), compression due to granular
  expansion and mergers with neighbouring MBPs. Similar amplification of
  the fields and interpretations were found in our simulations, as well
  as amplification due to vorticity. Such a fast amplification will have
  implications for a wide array of topics related to small-scale fields
  in the lower atmosphere, particularly with regard to propagating wave
  phenomena in MBPs.

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Title: Hydrogen Emission in Type II White-light Solar Flares
Authors: Procházka, Ondřej; Reid, Aaron; Mathioudakis, Mihalis
2019ApJ...882...97P    Altcode: 2019arXiv190710888P
  Type II white-light flares (WLFs) have weak Balmer line emission
  and no Balmer jump. We carried out a set of radiative hydrodynamic
  simulations to understand how the hydrogen radiative losses vary with
  the electron-beam parameters and more specifically with the low-energy
  cutoff. Our results have revealed that for low-energy beams, the excess
  flare Lyman emission diminishes with increasing low-energy cutoff as
  the energy deposited into the top chromosphere is low compared to the
  energy deposited into the deeper layers. Some Balmer excess emission is
  always present and is driven primarily by direct heating from the beam
  with a minor contribution from Lyman continuum backwarming. The absence
  of Lyman excess emission in electron-beam driven models with high
  low-energy cutoff is a prominent spectral signature of type II WLFs.

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Title: The magnetic properties of photospheric magnetic bright points
    with high-resolution spectropolarimetry
Authors: Keys, Peter H.; Reid, Aaron; Mathioudakis, Mihalis; Shelyag,
   Sergiy; Henriques, Vasco M. J.; Hewitt, Rebecca L.; Del Moro, Dario;
   Jafarzadeh, Shahin; Jess, David B.; Stangalini, Marco
2019MNRAS.488L..53K    Altcode: 2019MNRAS.tmpL..98K; 2019MNRAS.tmpL..95K; 2019arXiv190607687K
  Magnetic bright points (MBPs) are small-scale magnetic elements
  ubiquitous across the solar disc, with the prevailing theory suggesting
  that they form due to the process of convective collapse. Employing a
  unique full Stokes spectropolarimetric data set of a quiet Sun region
  close to disc centre obtained with the Swedish Solar Telescope, we look
  at general trends in the properties of magnetic bright points. In total
  we track 300 MBPs in the data set and we employ NICOLE inversions to
  ascertain various parameters for the bright points such as line-of-sight
  magnetic field strength and line-of-sight velocity, for comparison. We
  observe a bimodal distribution in terms of maximum magnetic field
  strength in the bright points with peaks at ∼480 G and ∼1700 G,
  although we cannot attribute the kilogauss fields in this distribution
  solely to the process of convective collapse. Analysis of MURAM
  simulations does not return the same bimodal distribution. However,
  the simulations provide strong evidence that the emergence of new flux
  and diffusion of this new flux play a significant role in generating
  the weak bright point distribution seen in our observations.

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Title: The Chromospheric Response to the Sunquake Generated by the
    X9.3 Flare of NOAA 12673
Authors: Quinn, Sean; Reid, Aaron; Mathioudakis, Mihalis; Nelson,
   Christoper; Krishna Prasad, S.; Zharkov, Sergei
2019ApJ...881...82Q    Altcode: 2019arXiv190608545Q
  Active region NOAA 12673 was extremely volatile in 2017 September,
  producing many solar flares, including the largest of solar cycle 24,
  an X9.3 flare of 2017 September 06. It has been reported that this flare
  produced a number of sunquakes along the flare ribbon. We have used
  cotemporal and cospatial Helioseismic and Magnetic Imager (HMI) line of
  sight (LOS) and Swedish 1 m Solar Telescope (SST) observations to show
  evidence of the chromospheric response to these sunquakes. Analysis
  of the Ca II 8542 Å line profiles of the wavefronts revealed that
  the crests produced a strong blue asymmetry, whereas the troughs
  produced at most a very slight red asymmetry. We used the combined
  HMI, SST data sets to create time-distance diagrams and derive the
  apparent transverse velocity and acceleration of the response. These
  velocities ranged from 4.5 to 29.5 km s<SUP>-1</SUP> with a constant
  acceleration of 8.6 × 10<SUP>-3</SUP> km s<SUP>-2</SUP>. We employed
  NICOLE inversions, in addition to the center-of-gravity method to
  derive LOS velocities ranging from 2.4 km s<SUP>-1</SUP>-3.2 km
  s<SUP>-1</SUP>. Both techniques show that the crests are created by
  upflows. We believe that this is the first chromospheric signature of
  a flare induced sunquake.

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Title: Mapping the Magnetic Field of Flare Coronal Loops
Authors: Kuridze, D.; Mathioudakis, M.; Morgan, H.; Oliver, R.; Kleint,
   L.; Zaqarashvili, T. V.; Reid, A.; Koza, J.; Löfdahl, M. G.; Hillberg,
   T.; Kukhianidze, V.; Hanslmeier, A.
2019ApJ...874..126K    Altcode: 2019arXiv190207514K
  Here, we report on the unique observation of flaring coronal loops at
  the solar limb using high-resolution imaging spectropolarimetry from
  the Swedish 1 m Solar Telescope. The vantage position, orientation,
  and nature of the chromospheric material that filled the flare loops
  allowed us to determine their magnetic field with unprecedented accuracy
  using the weak-field approximation method. Our analysis reveals coronal
  magnetic field strengths as high as 350 G at heights up to 25 Mm above
  the solar limb. These measurements are substantially higher than a
  number of previous estimates and may have considerable implications
  for our current understanding of the extended solar atmosphere.

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Title: Coronal and chromospheric observations of pre- and post-flare
    plasma evolution
Authors: Long, David; Reid, Aaron; Harra, Louise; Mathioudakis, Mihalis
2018csc..confE..16L    Altcode:
  Solar flares are among the most energetic and spectacular events
  occurring in our solar system, produced by the release of stored
  magnetic energy in the solar atmosphere through the reconnection
  of twisted magnetic fields. Although the magnetic field itself is
  difficult to observe in the solar atmosphere, we can gain vital
  insights into the reconnection process by studying the evolution
  of solar plasma prior to and following the flare. Here we present
  contemporaneous spectroscopic and imaging observations of an X9.3 solar
  flare from 2017-September-6. This was the largest flare of the current
  solar cycle to date, and was well observed in the corona by SDO/AIA
  and Hinode/EIS as well as in the chromosphere by instruments at the
  ground-based Swedish Solar Telescope. This combination of observations
  provides spectroscopic information throughout the solar atmosphere,
  giving a unique insight into the evolution of plasma in the lead-up
  to and following the flare.

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Title: Signatures of quiet Sun reconnection events in Ca II, Hα,
    and Fe I
Authors: Shetye, J.; Shelyag, S.; Reid, A. L.; Scullion, E.; Doyle,
   J. G.; Arber, T. D.
2018MNRAS.479.3274S    Altcode: 2018MNRAS.tmp.1509S; 2017arXiv170310968S
  We use observations of quiet Sun (QS) regions in the Hα 6563 Å, Ca II
  8542 Å, and Fe I 6302 Å lines. We observe brightenings in the wings
  of the Hα and Ca II combined with observations of the interacting
  magnetic concentrations observed in the Stokes signals of Fe I. These
  brightenings are similar to Ellerman bombs (EBs), i.e. impulsive
  bursts in the wings of the Balmer lines that leave the line cores
  unaffected. Such enhancements suggest that these events have similar
  formation mechanisms to the classical EBs found in active regions,
  with the reduced intensity enhancements found in the QS regions due to
  a weaker feeding magnetic flux. The observations also show that the
  quiet Sun Ellerman bombs are formed at a higher height in the upper
  photosphere than the photospheric continuum level. Using simulations,
  we investigate the formation mechanism associated with the events and
  suggest that these events are driven by the interaction of magnetic
  field lines in the upper photospheric regions. The results of the
  simulation are in agreement with observations when comparing the light
  curves, and in most cases, we found that the peak in the Ca II 8542
  Å wing occurred before the peak in Hα wing. Moreover, in some cases,
  the line profiles observed in Ca II are asymmetrical with a raised core
  profile. The source of heating in these events is shown by the MURaM
  simulations and is suggested to occur 430 km above the photosphere.

---------------------------------------------------------
Title: Reproducing Type II White-light Solar Flare Observations with
    Electron and Proton Beam Simulations
Authors: Procházka, Ondřej; Reid, Aaron; Milligan, Ryan O.; Simões,
   Paulo J. A.; Allred, Joel C.; Mathioudakis, Mihalis
2018ApJ...862...76P    Altcode: 2018arXiv180600249P
  We investigate the cause of the suppressed Balmer series and the origin
  of the white-light continuum emission in the X1.0 class solar flare on
  2014 June 11. We use radiative hydrodynamic simulations to model the
  response of the flaring atmosphere to both electron and proton beams,
  which are energetically constrained using Ramaty High Energy Solar
  Spectroscopic Imager and Fermi observations. A comparison of synthetic
  spectra with the observations allows us to narrow the range of beam
  fluxes and low energy cutoff that may be applicable to this event. We
  conclude that the electron and proton beams that can reproduce the
  observed spectral features are those that have relatively low fluxes
  and high values for the low energy cutoff. While electron beams shift
  the upper chromosphere and transition region to greater geometrical
  heights, proton beams with a similar flux leave these areas of the
  atmosphere relatively undisturbed. It is easier for proton beams to
  penetrate to the deeper layers and not deposit their energy in the
  upper chromosphere where the Balmer lines are formed. The relatively
  weak particle beams that are applicable to this flare do not cause
  a significant shift of the τ = 1 surface and the observed excess WL
  emission is optically thin.

---------------------------------------------------------
Title: Penumbral Waves Driving Solar Fan-shaped Chromospheric Jets
Authors: Reid, A.; Henriques, V. M. J.; Mathioudakis, M.; Samanta, T.
2018ApJ...855L..19R    Altcode:
  We use Hα imaging spectroscopy taken via the Swedish 1 m Solar
  Telescope to investigate the occurrence of fan-shaped jets at the solar
  limb. We show evidence for near-simultaneous photospheric reconnection
  at a sunspot edge leading to the jets appearance, with upward velocities
  of 30 km s<SUP>-1</SUP>, and extensions up to 8 Mm. The brightening at
  the base of the jets appears recurrent, with a periodicity matching that
  of the nearby sunspot penumbra, implying running penumbral waves could
  be the driver of the jets. The jets’ constant extension velocity
  implies that a driver counteracting solar gravity exists, possibly
  as a result of the recurrent reconnection erupting material into the
  chromosphere. These jets also show signatures in higher temperature
  lines captured from the Solar Dynamics Observatory, indicating a very
  hot jet front, leaving behind optically thick cool plasma in its wake.

---------------------------------------------------------
Title: Penumbral Waves driving Solar chromospheric fan-shaped jets
Authors: Reid, A.; Henriques, V. M. J.; Mathioudakis, M.; Samanta, T.
2018arXiv180207537R    Altcode:
  We use H$\alpha$ imaging spectroscopy taken via the Swedish 1-m Solar
  Telescope (SST) to investigate the occurrence of fan-shaped jets at
  the solar limb. We show evidence for near-simultaneous photospheric
  reconnection at a sunspot edge leading to the jets appearance, with
  upward velocities of 30\ks, and extensions up to 8~Mm. The brightening
  at the base of the jets appears recurrent, with a periodicity matching
  that of the nearby sunspot penumbra, implying running penumbral waves
  could be the driver of the jets. The jets' constant extension velocity
  implies that a driver counteracting solar gravity exists, possibly
  as a result of the recurrent reconnection erupting material into the
  chromosphere. These jets also show signatures in higher temperature
  lines captured from the Solar Dynamics Observatory (SDO), indicating
  a very hot jet front, leaving behind optically thick cool plasma in
  its wake.

---------------------------------------------------------
Title: Modelling of Electron and Proton Beams in a White-light
    Solar Flare
Authors: Procházka, O.; Reid, A.; Milligan, R. O.; Allred, J. C.;
   Mathioudakis, M.
2017AGUFMSH41A2756P    Altcode: 2017AGUFMSH41A2756M
  Observations of an X1 class WL solar flare on 2014 June 11 showed a
  surprisingly weak emission in both higher order Balmer and Lyman
  lines and continua. The flare was observed by RHESSI but low
  energy cut-off of non-thermal component was indeterminable due to
  the unusually hard electron spectrum (delta = 3). An estimate of
  power in non-thermal electron beams together with an area of WL
  emission observed by HMI yielded to an upper and lower estimate of
  flux 1E9 and 3E10 erg/cm2/s, respectively. We performed a grid of
  models using a radiative hydrodynamic code RADYN in order to compare
  synthetic spectra with observations. For low energy cut-off we chose
  a range from 20 to 120 keV with a step of 20 keV and delta parameter
  equal to 3. Electron beam-driven models show that higher low energy
  cut-off is more likely to produce an absorption Balmer line profile,
  if the total energy flux remains relatively low. On the other hand a
  detectable rise of HMI continuum (617 nm) lays a lower limit on the
  beam flux. Proton beam-driven models with equivalent fluxes indicate a
  greater penetration depth, while the Balmer lines reveal significantly
  weaker emission. Atmospheric temperature profiles show that for higher
  values of low energy cut-off the energy of the beam is deposited lower
  in chromosphere or even in temperature minimum region. This finding
  suggests, that suppressed hydrogen emission can indicate a formation
  of white-light continuum below chromosphere.

---------------------------------------------------------
Title: IRIS Burst Spectra Co-spatial to a Quiet-Sun Ellerman-like
    Brightening
Authors: Nelson, C. J.; Freij, N.; Reid, A.; Oliver, R.; Mathioudakis,
   M.; Erdélyi, R.
2017ApJ...845...16N    Altcode: 2017arXiv170705080N
  Ellerman bombs (EBs) have been widely studied over the past two
  decades; however, only recently have the counterparts of these events
  been observed in the quiet-Sun. The aim of this article is to further
  understand small-scale quiet-Sun Ellerman-like brightenings (QSEBs)
  through research into their spectral signatures, including investigating
  whether the hot signatures associated with some EBs are also visible
  co-spatial to any QSEBs. We combine Hα and Ca II 8542 Å line scans at
  the solar limb with spectral and imaging data sampled by the Interface
  Region Imaging Spectrograph (IRIS). Twenty-one QSEBs were identified
  with average lifetimes, lengths, and widths measured to be around 120 s,
  0.″63, and 0.″35, respectively. Three of these QSEBs displayed clear
  repetitive flaring through their lifetimes, comparable to the behavior
  of EBs in active regions. Two QSEBs in this sample occurred co-spatial
  to increased emission in SDO/AIA 1600 Å and IRIS slit-jaw imager 1400
  Å data; however, these intensity increases were smaller than those
  reported co-spatially with EBs. One QSEB was also sampled by the IRIS
  slit during its lifetime, displaying increases in intensity in the
  Si IV 1393 Å and Si IV 1403 Å cores, as well as the C II and Mg II
  line wings, analogous to IRIS bursts (IBs). Using RADYN simulations,
  we are unable to reproduce the observed QSEB Hα and Ca II 8542 Å
  line profiles, leaving the question of the temperature stratification
  of QSEBs open. Our results imply that some QSEBs could be heated to
  transition region temperatures, suggesting that IB profiles should be
  observed throughout the quiet-Sun.

---------------------------------------------------------
Title: Chromospheric Inversions of a Micro-flaring Region
Authors: Reid, A.; Henriques, V.; Mathioudakis, M.; Doyle, J. G.;
   Ray, T.
2017ApJ...845..100R    Altcode: 2017arXiv170700029R
  We use spectropolarimetric observations of the Ca II 8542 Å line, taken
  from the Swedish 1 m Solar Telescope, in an attempt to recover dynamic
  activity in a micro-flaring region near a sunspot via inversions. These
  inversions show localized mean temperature enhancements of ∼1000
  K in the chromosphere and upper photosphere, along with co-spatial
  bi-directional Doppler shifting of 5-10 km s<SUP>-1</SUP>. This heating
  also extends along a nearby chromospheric fibril, which is co-spatial
  to 10-15 km s<SUP>-1</SUP> downflows. Strong magnetic flux cancellation
  is also apparent in one of the footpoints, and is concentrated in the
  chromosphere. This event more closely resembles that of an Ellerman
  Bomb, though placed slightly higher in the atmosphere than what is
  typically observed.

---------------------------------------------------------
Title: Solar Ellerman Bombs in 1D Radiative Hydrodynamics
Authors: Reid, A.; Mathioudakis, M.; Kowalski, A.; Doyle, J. G.;
   Allred, J. C.
2017ApJ...835L..37R    Altcode: 2017arXiv170104213R
  Recent observations from the Interface Region Imaging Spectrograph
  appear to show impulsive brightenings in high temperature lines,
  which when combined with simultaneous ground-based observations in
  Hα, appear co-spatial to Ellerman Bombs (EBs). We use the RADYN
  one-dimensional radiative transfer code in an attempt to try and
  reproduce the observed line profiles and simulate the atmospheric
  conditions of these events. Combined with the MULTI/RH line synthesis
  codes, we compute the Hα, Ca II 8542 Å, and Mg II h and k lines for
  these simulated events and compare them to previous observations. Our
  findings hint that the presence of superheated regions in the
  photosphere (&gt;10,000 K) is not a plausible explanation for the
  production of EB signatures. While we are able to recreate EB-like
  line profiles in Hα, Ca II 8542 Å, and Mg II h and k, we cannot
  achieve agreement with all of these simultaneously.

---------------------------------------------------------
Title: Ellerman bombs in 1-D radiative hydrodynamics
Authors: Reid, Aaron
2017psio.confE..44R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Magnetic Flux Cancellation in Ellerman Bombs
Authors: Reid, A.; Mathioudakis, M.; Doyle, J. G.; Scullion, E.;
   Nelson, C. J.; Henriques, V.; Ray, T.
2016ApJ...823..110R    Altcode: 2016arXiv160307100R
  Ellerman Bombs (EBs) are often found to be co-spatial with bipolar
  photospheric magnetic fields. We use Hα imaging spectroscopy along with
  Fe I 6302.5 Å spectropolarimetry from the Swedish 1 m Solar Telescope
  (SST), combined with data from the Solar Dynamic Observatory, to study
  EBs and the evolution of the local magnetic fields at EB locations. EBs
  are found via an EB detection and tracking algorithm. Using NICOLE
  inversions of the spectropolarimetric data, we find that, on average,
  (3.43 ± 0.49) × 10<SUP>24</SUP> erg of stored magnetic energy
  disappears from the bipolar region during EB burning. The inversions
  also show flux cancellation rates of 10<SUP>14</SUP>-10<SUP>15</SUP>
  Mx s<SUP>-1</SUP> and temperature enhancements of 200 K at the detection
  footpoints. We investigate the near-simultaneous flaring of EBs due to
  co-temporal flux emergence from a sunspot, which shows a decrease in
  transverse velocity when interacting with an existing, stationary area
  of opposite polarity magnetic flux, resulting in the formation of the
  EBs. We also show that these EBs can be fueled further by additional,
  faster moving, negative magnetic flux regions.

---------------------------------------------------------
Title: Ellerman Bombs with Jets: Cause and Effect
Authors: Reid, A.; Mathioudakis, M.; Scullion, E.; Doyle, J. G.;
   Shelyag, S.; Gallagher, P.
2015ApJ...805...64R    Altcode: 2015arXiv150305359R
  Ellerman Bombs (EBs) are thought to arise as a result of photospheric
  magnetic reconnection. We use data from the Swedish 1 m Solar
  Telescope to study EB events on the solar disk and at the limb. Both
  data sets show that EBs are connected to the foot points of forming
  chromospheric jets. The limb observations show that a bright structure
  in the Hα blue wing connects to the EB initially fueling it, leading
  to the ejection of material upwards. The material moves along a loop
  structure where a newly formed jet is subsequently observed in the
  red wing of Hα. In the disk data set, an EB initiates a jet which
  propagates away from the apparent reconnection site within the EB
  flame. The EB then splits into two, with associated brightenings in
  the inter-granular lanes. Micro-jets are then observed, extending
  to 500 km with a lifetime of a few minutes. Observed velocities of
  the micro-jets are approximately 5-10 km s<SUP>-1</SUP>, while their
  chromospheric counterparts range from 50 to 80 km s<SUP>-1</SUP>. MURaM
  simulations of quiet Sun reconnection show that micro-jets with
  properties similar to those of the observations follow the line of
  reconnection in the photosphere, with associated Hα brightening at
  the location of increased temperature.

---------------------------------------------------------
Title: Chromospheric Diagnostics from IRIS and DST
Authors: Cauzzi, Gianna; Reardon, Kevin P.; Jaeggli, Sarah A.;
   Reid, Aaron
2014AAS...22430201C    Altcode:
  Using data obtained during a coordinated observing campaign in
  September 2013, we compare the spectral and imaging diagnostics from
  IRIS and the instruments at the Dunn Solar Telescope (DST). We focus
  on a small active region observed for approximately one hour with IRIS
  (NUV, FUV, and SJI) in conjunction with IBIS, FIRS, and ROSA from the
  DST.In particular, we examine the line widths and intensities in the
  different chromospheric lines (H-alpha, Ca II 8542, Mg II) and the
  temporal evolution of these different diagnostics. This allows us to
  better relate the views from new window provided by IRIS to previous
  studies of the chromosphere.

---------------------------------------------------------
Title: Radio and X-ray Diagnostics of Electron Beams in Solar Flares
Authors: Vilmer, Nicole; Kontar, Eduard; Hamish; Reid, A. S.;
   Maksimovic, Milan
2014cosp...40E3526V    Altcode:
  Solar flares are associated with efficient production of energetic
  particles at all energies. While energetic electrons and ions
  interacting with the solar atmosphere produce high energy X-rays
  and gamma-rays, the energetic electrons escaping to the corona and
  interplanetary medium produce coherent radio emissions (in particular
  type III bursts) and may be directly detected by experiments aboard
  spacecraft. We shall present the results of two statistical studies
  combining X-ray observations from RHESSI and of type III bursts observed
  in the decimeter/meter range and imaged by the Nançay Radioheliograph
  We shall show how the combination of X-ray and radio observations
  allows for some events to deduce the characteristics of the electron
  beam acceleration sites (height and size). We shall also present the
  results of a recent study on the percentage of decimetric/metric
  type III bursts observed with Nançay which have a counterpart at
  lower frequencies (namely in the range 14 to 1 MHz ) observed with
  Wind/Waves. This study is based on a list of events for which X-ray
  emission (by RHESSI) is also observed in connection with the type III
  bursts. We shall discuss the different reasons which could explain
  the extent or not of the metric type III burst to the hectometric range.

---------------------------------------------------------
Title: Alfvén Waves in Simulations of Solar Photospheric Vortices
Authors: Shelyag, S.; Cally, P. S.; Reid, A.; Mathioudakis, M.
2013ApJ...776L...4S    Altcode: 2013arXiv1309.2019S
  Using advanced numerical magneto-hydrodynamic simulations of the
  magnetized solar photosphere, including non-gray radiative transport and
  a non-ideal equation of state, we analyze plasma motions in photospheric
  magnetic vortices. We demonstrate that apparent vortex-like motions in
  photospheric magnetic field concentrations do not exhibit "tornado"-like
  behavior or a "bath-tub" effect. While at each time instance the
  velocity field lines in the upper layers of the solar photosphere show
  swirls, the test particles moving with the time-dependent velocity
  field do not demonstrate such structures. Instead, they move in a
  wave-like fashion with rapidly changing and oscillating velocity field,
  determined mainly by magnetic tension in the magnetized intergranular
  downflows. Using time-distance diagrams, we identify horizontal
  motions in the magnetic flux tubes as torsional Alfvén perturbations
  propagating along the nearly vertical magnetic field lines with local
  Alfvén speed.

---------------------------------------------------------
Title: Proterozoic rejuvenation of the Archean Crust tracked by U
    Pb and Hf-isotopes in Detrital Zircon
Authors: Belousova, E. A.; Reid, A. J.; Griffin, W. L.; O'Reilly, S. Y.
2006GeCAS..70R..44B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Petrography and Geochemistry of Upper Eocene Spherules from
    709C (Indian Ocean) and DSDP 612 (NW Atlantic)
Authors: Rajmon, D.; Reid, A. M.; Copeland, P.
2006LPI....37.2201R    Altcode:
  Spherules from ODP 709c (Indian ocean) diplay petrographic and
  geochemical characteristics similar to spherules from ODP 216 and 292
  (SE Asia). The data, however, neither strongly support nor reject the
  hypothesis of a third Upper Eocene ejecta layer in SE Asia.

---------------------------------------------------------
Title: Argon isotopic analysis of breccia veins from the Roter Kamm
    crater, Namibia, and implications for their thermal history
Authors: Rajmon, D.; Copeland, P.; Reid, A. M.
2005M&PS...40..841R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Potential of Radar Imaging and Sounding Methods in Mapping
Heavily Eroded Impact Craters: Mapping Some Structural Elements of
    the Hico Crater, TX
Authors: Heggy, E.; Horz, F.; Reid, A. M.; Hall, S. A.; Chan, C.
2004LPI....35.1462H    Altcode:
  SRTM data combined with a GPR field survey of the area north Hico
  central Texas, suggest that the Hico disturbed area is an impact
  structure with a minimum diameter around 5 km, and that its concentric
  rings are structurally controlled by faults.

---------------------------------------------------------
Title: Magnetic Investigations of Breccia Veins and Basement Rocks
    from Roter Kamm Crater and Surrounding Region, Namibia
Authors: Rajmon, D.; Hall, S. A.; Reid, A. M.; McG. Miller, R.;
   Robertson, D. J.
2004LPI....35.1867R    Altcode:
  The target rocks from Roter Kamm crater retained NRM components related
  to the Kalahari APWP for ~1.1 0.9, ~0.7 0.6 and ~0.5 Ga. There is no
  evidence for re-magnetization of the Roter Kamm samples at ~300 Ma or
  during the impact at 3.7 Ma.

---------------------------------------------------------
Title: “Pseudotachylytes” that Never Melted: A Thermal Story from
    Roter Kamm Crater, Namibia
Authors: Rajmon, D.; Copeland, P.; Reid, A. M.
2002LPI....33.1944R    Altcode:
  The rim rocks of the 2.5 km Roter Kamm crater in southwest
  Namibia are cut by breccia veins that macroscopically resemble
  pseudotachylytes. <SUB>40</SUB>Ar/<SUB>39</SUB>Ar data, coupled to
  other published data, show that these veins never approached melting
  temperatures and only attained temperatures of 250-330 °C.

---------------------------------------------------------
Title: Metamorphosed Antarctic LL Chondrites: Pyroxene Thermometry
Authors: Reid, A. M.; Dussaud, E. A.
2000LPI....31.1751R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Radio study of X-ray clusters. (Thesis abstract).
Authors: Reid, A. D.
2000PASA...17..285R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Geology and Stratigraphy of Mare Tranquillitatis
Authors: Rajmon, D.; Reid, A. M.; Spudis, P.
1999M&PSA..34R..96R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Temperature and Formation of Pseudotachylytic Impact Breccias,
    Roter Kamm Crater, Southwestern Namibia
Authors: Rajmon, D.; Copeland, P.; Reid, A. M.; Lavigne, J. -F.
1999M&PSA..34...95R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Heterogeneity of Silicates in Antarctic LL4 Chondrites
Authors: Aoyama, H.; Reid, A. M.
1999LPI....30.1791A    Altcode:
  LL4 Antarctic chondrites contain a mix of relict primary and metamorphic
  secondary characteristics. The metamorphic effects probably relate to
  short-lived high temperature impact events rather than to prolonged
  burial metamorphism.

---------------------------------------------------------
Title: Radio study of X-ray clusters of galaxies -- II. A1300:
    a post-merger cluster at z=0.31 containing a halo and a relic
Authors: Reid, A. D.; Hunstead, R. W.; Lemonon, L.; Pierre, M. M.
1999MNRAS.302..571R    Altcode:
  As part of an extensive radio--IR--optical--X-ray study of ROSAT
  clusters of galaxies in the Hydra region we have observed the Abell
  cluster A1300, one of the most distant (z~= 0.31) and X-ray luminous
  (L_X~ 1.7 x 10^45 erg s^-1 cm^-2, 0.1--2.4 keV) clusters in the
  sample, with the Molonglo Observatory Synthesis Telescope at 843 MHz
  and the Australia Telescope Compact Array at 1.34, 2.4, 4.8 and 8.6
  GHz. Previous results in the X-ray and optical have suggested that
  A1300 is in a post-merging phase. We present further evidence of this
  with the discovery of two diffuse radio sources projected within the
  extended X-ray emission of A1300. These may be among the most distant
  radio halo and relic sources yet found. We argue that the halo source,
  which is seen in projection near the centre of the cluster and coincides
  with an extension in the X-ray surface brightness distribution, is
  the result of a cluster-wide process related to the merger.

---------------------------------------------------------
Title: Memorial for Elbert Aubrey King, Jr.
Authors: Reid, A.
1999M&PS...34..677R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: ASCA/ROSAT observations of the radio source MRC 0625-536
Authors: Otani, C.; Brinkmann, W.; Boehringer, H.; Reid, A.;
   Siebert, J.
1998A&A...339..693O    Altcode:
  We present the results of ROSAT/ASCA observations of the bright
  southern radio source MRC 0625-536. The majority of the X-ray emission
  originates from the surrounding cluster Abell 3391. The best fit
  temperature for the cluster gas is kT = 5.8(+0.4}_{-0.3) keV with
  an abundance of 0.36+/- 0.10 times the solar value. We determined
  the radial mass profile and extrapolating the data out to 3 Mpc, and
  we find that the total mass of the cluster is (0.4 - 1.6) x 10(15)
  M_sun. Up to about 10% of the X-ray flux could originate from the
  central dumbbell galaxy. A comparison of the X-ray contours with the
  complex 13cm radio structure reveals strong interactions between the
  radio jets and the surrounding matter. MRC 0625-536 is thus another
  object where the interaction between the otherwise invisible matter
  of the cluster and the activity of the central radio galaxy can be
  studied by combining data from the radio and the X-ray regimes.

---------------------------------------------------------
Title: Lewis Cliff 88701: A Partly Equilibrated LL4 Chondrite
Authors: Reid, A. M.; Ayoyama, H.
1998M&PSA..33Q.128R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Time-dependent structure in ultraviolet absorption lines of
    the rapid rotators HD 64760 (B0Ib) and HD 93521 (O9.5V)
Authors: Howarth, Ian D.; Townsend, R. H. D.; Clayton, M. J.;
   Fullerton, A. W.; Gies, D. R.; Massa, D.; Prinja, R. K.; Reid, A. H. N.
1998MNRAS.296..949H    Altcode:
  Cross-correlation provides an effective line-averaging function
  for spectra containing many line features, a result which can
  be exploited in order to perform time-series and spatial-domain
  analyses of absorption-line variability in data of (relatively) poor
  quality. We apply this method to high-resolution IUE spectra. For
  the known non-radial pulsator HD 93521 (O9.5V), time-series analysis
  of the cross-correlation function recovers two periods that are
  confirmed in independent optical data (P_1=1.77 h, P_2=2.90 h); there
  is no statistically significant excess power at these frequencies
  in lines formed in the stellar wind. By comparing phase information
  from the time-series analysis with results from pulsation models we
  estimate l~=10+/-1 and 6+/-1 as the harmonic degrees for P_1 and P_2,
  respectively, with l+m&lt;~2 for each mode (where m is the azimuthal
  order of the mode). We also present evidence for absorption-line
  variability in HD 64760 (HR3090 B0.5 Ib), finding marginally significant
  signals with P_1=8.9 h (or, possibly, 14.2 h) and P_2=29 h. The longer
  period is present, with a strong signal, in wind-formed lines. We
  consider possible circumstellar and (quasi-)photospheric origins for
  P_2, and conclude that this signal probably does not arise through
  rotational modulation (with the corollary that the stellar-wind signal
  also does not arise in corotating structures, contrary to previous
  suggestions). The phase behaviour of the signals is consistent with
  non-radial pulsation models characterized by l=5+/-1 (P_1) and 2+/-1
  (P_2), with l+m&lt;=1, supporting a previous suggestion by Baade that
  both low- and higher-order modes are present; the wind modulation at P_2
  may then result from leakage of pulsation energy into the supersonic
  outflow. The lack of significant photometric variability is a serious
  difficulty for this model (any sinusoidal photometric variability at P_2
  has semiamplitude &lt;2 mmag at lambda_eff=1575Angstroms, with 95 per
  cent confidence), but this may itself be a consequence of wave leakage.

---------------------------------------------------------
Title: Radio study of X-ray clusters of galaxies - I. A3528: a
    pre-merging cluster in the core of the Shapley Supercluster
Authors: Reid, A. D.; Hunstead, R. W.; Pierre, M. M.
1998MNRAS.296..531R    Altcode: 1997astro.ph.11330R
  As part of an extensive radio-IR-optical-X-ray study of ROSAT
  clusters of galaxies in the Hydra region we have observed the bimodal
  Abell cluster A3528, located in the core of the Shapley Supercluster
  (z~=0.053), with the Molonglo Observatory Synthesis Telescope at 843MHz
  and the Australia Telescope Compact Array at 1.4 and 2.4GHz. This is
  part I in a series of papers which looks at the relationship between
  the radio and X-ray emission in samples of ROSAT selected clusters. The
  radio source characteristics - tailed morphologies and steep spectra -
  are consistent with the effects of a dense intracluster medium and
  the pre-merging environment of A3528. In particular, we present
  evidence that the minor member of the radio-loud dumbbell galaxy
  located at the centre of the northern component of A3528 is on a
  plunging orbit. We speculate that this orbit may have been induced by
  the tidal interactions between the merging components of A3528. In
  addition, the radio source associated with the dominant member of
  the dumbbell galaxy exhibits many of the characteristics of compact
  steep spectrum sources. We argue that the radio emission from this
  source was triggered ~10^6 yr ago by tidal interactions between the
  two members of the dumbbell galaxy, strengthening the argument that
  compact steep spectrum (CSS) sources are young. Re-analysis of archive
  pointed Position Sensitive Proportional Counter (PSPC) data using
  multiresolution filtering suggests the presence of an AGN and/or a
  cooling flow in the southern component of A3528.

---------------------------------------------------------
Title: Characterization of Experimental Shock Effects in Calcite
    and Dolomite by X-Ray Diffraction
Authors: Bell, M. S.; Horz, F.; Reid, A.
1998LPI....29.1422B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: LL Chondrites and Prior's Rules
Authors: Komatsu, M.; Reid, A. M.
1998LPI....29.1224K    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: VizieR Online Data Catalog: Probing the LHS Catalog (Gizis+
    1997)
Authors: Gizis, J. E.; Reid; I. N.
1997yCat..61090849G    Altcode:
  We present moderate resolution spectroscopy of 111 cool dwarf stars
  to supplement the observations we have already presented in the
  Palomar/MSU Nearby-Star Spectroscopic Survey. The sample consists of
  71 suspected nearby stars added to the Preliminary Third Catalog of
  Nearby Stars since 1991 as well as 40 faint red stars selected from
  the LHS catalog. The study was aimed at identifying interesting red
  dwarfs, particularly new nearby, ultracool dwarfs, and very metal-poor
  stars. <P />The observations were made using the Palomar 60-inch,
  the Hale 200-inch and the Las Campanas 100-inch telescopes between
  June 1995 and January 1996. The spectral resolution is approximately
  3 Angstroms per pixel with wavelength coverage from 6200 to 7500
  Angstroms. Table 2 contains bandstrengths for TiO, CaH, and CaOH
  indices. <P />(4 data files).

---------------------------------------------------------
Title: X-ray/optical analysis of the cluster of galaxies Abell 1300:
    indications of a post-merger at z=0.31.
Authors: Lemonon, L.; Pierre, M.; Hunstead, R.; Reid, A.; Mellier,
   Y.; Boehringer, H.
1997A&A...326...34L    Altcode: 1997astro.ph..4065L
  We present ROSAT PSPC and HRI observations of the distant cluster
  A 1300 (z=0.3071) in conjunction with optical data, to investigate
  the physics of the intra-cluster medium and the dynamical state
  of the cluster. By means of a multi-resolution wavelet analysis,
  we find evidence for structures in the X-ray emission of this very
  luminous (L_X_~1.7x10^45^erg/s in the 0.1-2.4keV band) and massive
  (M_tot_~1.3x10^15^M<SUB>sun</SUB>_ at a radius ~2.2Mpc) cluster. This
  cluster is significant as we appear to be witnessing the end of a
  merger which occurred at an early epoch.

---------------------------------------------------------
Title: Petrology of Allende dark inclusions
Authors: Buchanan, P. C.; Zolensky, M. E.; Reid, A. M.
1997GeCoA..61.1733B    Altcode:
  Bulk compositions acquired by neutron activation analysis are reported
  for eight Allende dark inclusions (DIs) and compared with compositions
  of five DIs previously reported in the literature. Enrichments of
  the elements Na, K, Br, Ba, Au, and As are generally correlated with
  increased proportions of porous aggregates predominantly composed
  of fine-grained, platy to fibrous olivine. These aggregates have
  been interpreted by some workers as chondrules and inclusions that
  first were exposed to aqueous alteration, converting anhydrous
  silicates to phyllosilicates, and later were dehydrated by thermal
  metamorphism, converting phyllosilicates to olivine. Our data support
  this interpretation and suggest that the aqueous alteration was open
  system in character. Feldspathoid grains intergrown with platy to
  fibrous olivines in porous, olivine-rich aggregates and inclusions of
  sodalite, nepheline, pentlandite, ilmenite, and spinel in these olivines
  suggest that phyllosilicates produced during aqueous alteration could
  accommodate Na, K, Ni, S, etc and are most consistent with a mixture
  of both saponite and serpentine. Dehydration of saponite would require
  that the temperature of thermal metamorphism was higher than previously
  suggested and may have been as high as 800°-900°C. Nonporous rims
  containing Ca-rich minerals (andradite, hedenbergite) surrounding dark
  inclusions containing highest proportions of porous, olivine-rich
  aggregates and slight to moderate depletions of these clasts in Ca
  relative to bulk Allende suggest that these rims were also the result
  of redistribution of some elements during dehydration of these clasts
  caused by thermal metamorphism.

---------------------------------------------------------
Title: Petrography and Mineral Chemistry of the Pipliya Eucrite
Authors: Buchanan, P. C.; Goetzee, S. H.; Reimold, W. U.; Reid, A. M.
1997LPI....28..167B    Altcode:
  The texture and mineralogy of the Pipliya meteorite are reported. The
  meteorite is a brecciated eucrite and is distinctive because of its
  high proportion of lithic clasts compared to the amount of brecciate
  matrix and because lithology A (fine-grained and containing pyroxenes
  similar in composition to those in 'main group' eucrites) and lithology
  B (similar to A in mineralogy but medium-grained) are similar in
  pyroxene mineralogy but different in texture and grain size. The
  texture of the matrix material suggests that the breccia may have
  undergone late stage metamorphism.

---------------------------------------------------------
Title: Olivine and Pyroxene Compositions in LL6 Chondrites from
    Antarctica
Authors: Reid, A.
1997LPI....28.1155R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Antarctic LL Chondrites
Authors: Reid, A. M.
1997pbnm.work...50R    Altcode: 1997LPITR9702...50R
  No abstract at ADS

---------------------------------------------------------
Title: A first glimpse into ISM/ICM connections at z=0.2 with ISOCAM.
Authors: Pierre, M.; Aussel, H.; Altieri, B.; Bernard, J. P.; Biviano,
   A.; Boulade, O.; Cesarsky, C.; Cesarsky, D.; Elbaz, D.; Hunstead,
   R.; Lemonon, L.; Reid, A.; Vigroux, L.
1996A&A...315L.297P    Altcode:
  Although it is well established that the cluster environment affects
  the gas content and massive star formation in galaxies, the mechanisms
  have not yet been unambiguously identified. In order to elucidate
  some of the processes responsible, an ISO Core Programme - DEEPXSRC -
  is dedicated to deep observations of medium redshift rich clusters
  of galaxies. We present here the first results from this programme,
  obtained by correlating our ISOCAM observations ( at 7.5 and 15μm)
  of the cluster A1732 with radio, optical and X-ray images. Some 10
  distant IR galaxies are detected in an 8'x8' field and are the faintest
  extragalactic sources detected by ISO so far.

---------------------------------------------------------
Title: Optical time-series spectroscopy of the O4 supergiant ζ
    Puppis.
Authors: Reid, A. H. N.; Howarth, I. D.
1996A&A...311..616R    Altcode:
  We present time-resolved echelle spectroscopy of the O4 I(n)f supergiant
  ζ Puppis. Variations are observed in all absorption-line profiles,
  with typical peak-to-peak amplitudes of ~2% of the continuum intensity
  (~4% in He II λ5411A). All observed absorption lines (He I, He II,
  N IV, and C IV) show the same gross characteristics, with `bumps' and
  `dips' moving blue-to-red through the profiles, with no detectable
  line-to-line velocity shifts in the variability pattern (&lt;15km/s)
  although there are differences in the relative amplitudes across the
  lines. The time dependence of the variability is investigated by using
  a 2-D clean power-spectrum analysis. Significant power is found at a
  period of ~8.54hr; the underlying signal is marginally consistent with
  sectorial, prograde non-radial pulsations with l=-m=2, although this
  does not account for all the observed variability. The blue emission
  wing of Hα was included in the echellograms, and, in contrast to the
  absorption lines, shows features moving red-to-blue with a period of
  8.5hr (the absorption-line period). The Hα data also show features
  at a period of 19.6hr (the recurrence time of the `discrete absorption
  features' observed in UV P-Cygni resonance lines), moving blue-to-red
  at velocities more positive than -280km/s and red-to-blue at more
  negative velocities. The temporal behaviour of Hα provides the first
  direct evidence for a dynamical response of a radiation-driven wind
  to basal velocity fields.

---------------------------------------------------------
Title: Breccias resembling melt bombs from the Roter Kamm Crater
Authors: Degenhardt, J. J.; Miller, R. McG.; Reimold, W. U.; Reid,
   A. M.
1996M&PS...31..413D    Altcode:
  Irregular, dark green to black, glassy-looking boulders are locally
  common in the northwest portion of the rim of the Roter Kamm impact
  crater in southern Namibia. Their smooth surfaces, flow-like textures,
  presence of folds, and their similarity to melt bombs have led to
  the interpretation that these are molten impact ejecta. However, the
  samples we have examined are all fine-grained breccias composed of
  angular fragments that show no evidence of melting. Meltlike surface
  textures of these rim breccias are largely a consequence of surface
  wind polishing of fine-grained rocks in a desert environment. These
  mono-mict breccias were produced by impact-related brecciation of
  Gariep sediments (carbonaceous, siliceous shales) previously modified
  by low-grade Damaran metamorphism. Secondary quartz within the breccias
  is attributed to fluid activity that postdates the impact.

---------------------------------------------------------
Title: Analysis of Dark Inclusions from Allende
Authors: Buchanan, P. C.; Zolensky, M. E.; Wentworth, S. J.; Reid,
   A. M.
1996LPI....27..177B    Altcode:
  Fruland et al. described dark inclusions found in the meteorite Allende
  as "black to light gray lithic inclusions (xenoliths) that have been
  found to be different from the bulk meteorite, both petrographically
  and chemically." Similar dark inclusions have been described from
  other CV3 meteorites (e.g., Leoville and Vigarano). Most authors
  have concluded that these clasts are petrogenetically related to the
  meteorites in which they occur, even though textures can be strikingly
  different. These inclusions apparently represent materials that have
  been affected by different processes from those that affected typical
  CV3 meteorites, or by the same processes either in a different sequence
  or to different degrees. This abstract reports and interprets new
  geochemical and mineralogical data for several of these clasts.

---------------------------------------------------------
Title: Non-Chondritic Inclusions in the LL Chondrite DOM85505
Authors: Peterson, K. C. A.; Reid, A. M.; Mittlefehldt, D. W.
1996LPI....27.1027P    Altcode:
  DOM85505 is a 31g LL Antarctic chondrite that was noted in the
  preliminary description to contain inclusions lacking chondritic
  texture. Angular inclusions in the host chondrite (LL5, S4) do
  not resemble any of the common achondrites in texture or mineral
  composition. The non-chondritic inclusions have similar bulk
  compositions and the same mineral compositions as the host chondrite
  and appear to be have formed as cumulates from an LL chondrite
  melt. Texturally similar non-chondritic inclusions in the L6 Yamato
  meteorites 75097 and 793241 derive from an H chondrite source but are
  also cumulates that have reacted with the host chondrite following
  incorporation.

---------------------------------------------------------
Title: Petrology of Allende Dark Inclusions
Authors: Buchanan, P. C.; Zolensky, M. E.; Reid, A. M.
1996M&PSA..31Q..23B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Petrology of the polymict eucrite Petersburg
Authors: Buchanan, P. C.; Reid, A. M.
1996GeCoA..60..135B    Altcode:
  The polymict eucrite Petersburg contains eucritic and diogenitic
  materials which span a broad range of compositions. The present
  study focuses on four eucritic clasts for which bulk compositions and
  mineralogical data were acquired; the broad compositional range of
  these clasts documents the diversity of the parent regolith. Clast
  A is REE-rich (~26 × chondrite) and magnesian (Mg# = 48.7);
  composition of this clast can best be explained by partial melting of
  a source region distinctly different from that of other noncumulate
  eucrites. Composition of eucritic clast B is similar to compositions
  of cumulate eucrites in REE and Sr abundances, but it has a much
  lower Mg# than Moore County. Clasts C and D are similar in texture,
  mineralogy, and composition to main group eucrites. The presence of
  anomalous clast A in the same polymict breccia as typical eucrite
  clasts C and D emphasizes the variability of source materials from
  which eucritic melts were derived on the HED parent body(ies). After
  final accretion, this breccia apparently was exposed to a minor episode
  of thermal metamorphism causing ~30 μm wide alteration rims around
  larger pyroxene fragments and causing alteration of pyroxenes at the
  edges of eucritic clasts. This metamorphism completely altered the Mg#
  of smaller matrix pyroxenes, less than 40-60 μm in size, to values
  closer to the bulk Mg# of the meteorite.

---------------------------------------------------------
Title: Multi-Wavelength Study of ROSAT Clusters of Galaxies
Authors: Reid, A. D.; Hunstead, R. W.; Pierre, M. M.
1996IAUS..175..353R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Recovery of three ordinary chondrites, Rooikop 001-003,
    from the Namib Desert in Western Namibia
Authors: Reid, A. M.; Jakes, O.; Zolensky, M. E.; Miller, R. Mcg.
1995Metic..30..781R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Features Resembling Pseudotachylyte at Enchanted Rock
    Batholith, Texas
Authors: Buchanan, P. C.; Degenhardt, J. J., Jr.; Reid, A. M.
1995Metic..30R.492B    Altcode:
  Enchanted Rock batholith in central Texas is a granitic pluton of ~250
  km^2 area [1]. The batholith intrudes Precambrian metamorphic rocks and
  is dated by Rb-Sr at 1,048+/-34 m.y. [2]. Plutonic rocks are exposed in
  a series of exfoliation domes located along the southeastern edge of the
  batholith. Numerous subvertical fractures occur along the outer margins
  of the intrusion and, in a few cases, between exfoliation domes. A
  number of these fractures contain veins described as pseudotachylytes
  by Barnes [3]. In hand specimen, the veins resemble pseudotachylytes,
  forming a branching network and containing angular fragments of local
  country rock in a fine-grained matrix that locally exhibits an apparent
  flow texture. Some smaller veins appear to have been injected into
  host rock. The veins range in width up to ~30 cm with boundaries which
  are sharp and smooth with undulating surfaces. Thin (~4-5 cm) aplite
  dikes cut the granite and generally show small amounts of displacement
  where intersected by the fracture veins (maximum measured apparent
  displacement ~75 cm). Matrix material in veins includes fragments of
  quartz, feldspar, biotite, and opaques. Matrix biotite is generally
  associated with opaques and occurs as numerous, tiny, oriented flakes
  between fragments of feldspar and quartz in areas which are darker
  than surrounding matrix. The flow-like textures of matrix materials
  are defined by these darker areas which are elongated subparallel
  to fracture direction. The finer-grained matrix biotite apparently
  derives from comminution of larger grains from host rock. Larger clasts
  include rock fragments and fragments of alkali feldspar and quartz,
  with a tendency for the larger fragments to concentrate in the centers
  of veins. Clasts are irregular in shape and are commonly angular and
  rarely contorted. Rock fragments are derived from host rock and also
  include "breccia within breccia" fragments. Single-mineral fragments
  display evidence of strain; quartz commonly shows undulatory extinction,
  mosaic texture, and multiple fractures. Feldspar twins commonly are
  deformed. None of the samples show PDF's in quartz or any evidence
  for the former presence of glass or quenched melt which might have
  formed by frictional melting. Fracture vein materials from Enchanted
  Rock pluton are not pseudotachylytes sensu stricto, in that there is
  no evidence of frictional melting. The presence of small, comminuted
  flakes of apparently unaltered biotite in these veins suggests that
  temperatures did not exceed ~400 degrees-800 degrees C for appreciable
  periods of time [4, 5, 6] and limits the amount of frictional heating
  which could have affected these breccias. However, some characteristic
  features of these rocks are similar to those of pseudotachylytes,
  including narrow vein-like form, flow-like texture, very fine-grained
  brecciated nature, extensive deformation of constituent minerals, and
  localized derivation. These veins represent narrow zones of moderately
  intense deformation related to the latter stages of emplacement of the
  pluton or to later tectonic activity. The deformation is not related
  to impact processes or to fault zones involving any significant
  displacement. References: [1] Hutchison R. M. (1956) Bull. GSA, 67,
  763-806. [2] Garrison J. R. Jr. et al. (1979) Contrib. Mineral. Petrol.,
  69, 361-374. [3] Barnes V. E. (1940) Texas Univ. Publ. 3945,
  645-656. [4] Vedder W. and Wilkins R. W. T. (1969) Am. Mineral., 54,
  482-509. [5] Sanz J. et al. (1983) Phys. Chem. Mineral., 9, 14-18. [6]
  Spray J. G. (1992) Tectonophys., 204, 205-221.

---------------------------------------------------------
Title: High resolution radio maps of quasars from the Jodrell Bank
    966MHz survey.
Authors: Reid, A.; Shone, D. L.; Akujor, C. E.; Browne, I. W. A.;
   Murphy, D. W.; Pedelty, J.; Rudnick, L.; Walsh, D.
1995A&AS..110..213R    Altcode:
  Radio maps are presented of quasars from the Jodrell Bank 966MHz
  survey. The maps are made from observations at 408MHz with MERLIN,
  1464/1666MHz with the VLA/MERLIN and at 5GHz with the VLA. The core
  radio spectra at the three frequencies are shown for nearly all the
  sources, showing that although a majority of core spectra are flat,
  some sources have steep-spectrum cores.

---------------------------------------------------------
Title: 'Melt' Breccias from the Roter Kamm Impact Crater, Namibia
Authors: Degenhardt, J. J., Jr.; Reid, A. M.; Buchanan, P. C.; Miller,
   R. Mcg.
1995LPI....26..323D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Recovering Parental Magma Compositions: A Single-Blind Test
    of the Method and an Analysis of a Kilauean Parental Magma
Authors: Woronow, A.; Reid, A. M.; Jones, J. H.
1995LPI....26.1521W    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Book Review: New perspectives on stellar pulsation and
    pulsating variable stars (IAU colloquium 139) / Cambridge U Press,
    1993
Authors: Reid, A.
1995Obs...115...44R    Altcode: 1995Obs...115...44N
  No abstract at ADS

---------------------------------------------------------
Title: Two Modes of Pulsation in the Rapidly Rotating O9.5 Dwarf,
    HD 93521
Authors: Reid, A. H. N.; Bohlender, D.; Bolton, C. T.; Fullerton,
   A. W.; Howarth, I. D.; Manz, C.; Smith, K. C.; Townsend, R. H. D.
1995ASPC...83..309R    Altcode: 1995aasp.conf..309R; 1995IAUCo.155..309R
  No abstract at ADS

---------------------------------------------------------
Title: Recovery of Three Ordinary Chondrites from the Namib Desert
    in Western Namibia
Authors: Reid, A. M.; Jakeš, P.; Zolensky, M. E.; McG. Miller, R.
1995mfch.work...57R    Altcode: 1995LPITR9502...57R
  No abstract at ADS

---------------------------------------------------------
Title: Locating New Meteorite Recovery Areas
Authors: Zolensky, M. E.; Schutt, J. W.; Reid, A. M.; Jakeš, P.;
   Martinez de Los Rios, E.; Miller, R. M.
1995mfch.work...78Z    Altcode: 1995LPITR9502...78Z
  No abstract at ADS

---------------------------------------------------------
Title: Multi-wavelength study of ROSAT clusters of galaxies.
Authors: Pierre, M.; Hunstead, R.; Reid, A.; Robertson, G.; Mellier,
   Y.; Soucail, G.; Böhringer, H.; Ebeling, H.; Voges, W.; Cesarsky,
   C.; Oukbir, J.; Sauvageot, J. -L.; Vigroux, L.
1994Msngr..78...24P    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Subsurface Character of the Marquez Impact Crater in Leon
    County, Texas, as Determined from Gravity and Well Log Data
Authors: Wong, A. M.; Reid, A. M.; Hall, S. A.; Sharpton, V. L.
1994Metic..29R.552W    Altcode:
  The Marquez Dome in northwest Leon County, Texas is a shallow buried
  complex impact crater. Exposure of Cretaceous sediments in a 1.2
  km diameter disturbed zone, surrounded by shallow dipping Tertiary
  sediments, led early investigators to interpret the structure as the
  uplift overlying a salt dome. Subsequent drilling and seismic reflection
  data within the area have ruled out a salt diapiric origin. Gibson and
  Sharpton [1], and Sharpton and Gibson [2] reinterpreted the disturbed
  zone as the central uplift of a complex crater, based on the absence
  of salt above 5000 m below sea level, from well log information, on
  the presence, from seismic reflection data, of continuous flat-lying
  reflectors beneath the structure, and on examination of the rocks from
  the central uplift. Shatter cones were found associated with the uplift
  and planar deformation features occur in quartz grains collected at
  the Marquez Dome [2]. Sharpton and Gibson [2] estimated the age of
  the structure at 58 m.y., and that age has recently been confirmed
  by apatite fission track dating [3]. In an attempt to understand the
  geometry of the Marquez Dome, which is only exposed within the region
  of the central uplift, we have combined limited surface mapping with
  available geophysical well logs, and with gravity data that combines
  a new detailed survey with earlier regional gravity data. Structure
  maps were constructed by well log correlation for five stratigraphic
  horizons that were disrupted by the impact. The extent of the crater was
  estimated by mapping the small negative gravity anomaly that surrounds
  the central uplift. Depths to the breccia lens surrounding the uplift
  were estimated using empirical scaling laws. The revised model for the
  Marquez Structure yields a diameter estimate of 12.7 km with an uplift
  of at least 1120 m at the center of the structure. Subsurface structure
  maps show decreasing deformation with depth, consistent with an impact
  origin. From the well log and gravity data we have constructed a three
  dimensional model of the central uplift to a depth of around 2000 m,
  where there is no further evidence of deformation associated with
  the central uplift. The predictions of this model, at least for the
  shallow horizons, will be tested with the completion of two shallow
  drill holes, sited just off the central uplift and midway to the
  proposed crater rim. Core will be recovered selectively from both these
  holes. References: [1] Gibson J. W. Jr. and Sharpton V. L. (1989) EOS,
  70-15, 383. [2] Sharpton V. L. and Gibson J. W. Jr. (1990) LPS XXI,
  1136-1137. [3] McHone J. F. and Sorkhabi R. B. (1994) LPS XXV, 881-882.

---------------------------------------------------------
Title: Lithic Clasts in the Polymict Eucrite Petersburg
Authors: Buchanan, P. C.; Reid, A. M.
1994Metic..29S.450B    Altcode:
  The polymict eucrite Petersburg is a regolith breccia containing
  significant proportions of matrix pyroxenes with compositions
  interrnediate between those found in diogenites and noncumulate
  eucrites. Possible sources of these intennediate composition pyroxenes
  include cumulate eucrites, noncumulate eucrites more magnesian than
  "main group" eucrites, cores of zoned pyroxenes from unequilibrated
  eucntes, and eucritic materials affected by metamorphic redistribution
  of Fe/Mg. Abundant eucritic clasts in Petersburg allow examination of
  materials from which matrix minerals were derived. The majority of
  Petersburg lithic clasts represent Fe-rich, equilibrated eucrites
  similar to Juvinas. Clast pyroxenes within 20-30 micrometers of
  clast edges have significantly higher Mg# than interior pyroxenes;
  this is apparently the result of subsolidus alteration after clast
  formation. Fe-rich alteration rims of similar thickness are present
  on matrix pyroxenes of diogenitic composition. Fe/Mg exchange
  during lithification of howardites and polymict eucrites has been
  reported previously [l,2]. Based on matrix textures, Hewins [3,4]
  has inferred thermal metamorphism of the Petersburg breccia under a
  hot breccia blanket or lava flow. The uniform width and ubiquity of
  Petersburg alteration rims suggests formation during a single thermal
  event after final breccia accumulation. Less common among Petersburg
  eucrite clasts are more magnesian compositions. Mittlefehldt [5]
  reported data from Petersburg clast RC03 with bulk Mg# of 46 and
  REE abundances of ~13x chondrite. We have analyzed Petersburg clast
  A, a medium-grained (average grain size ~l mm), subophitic clast
  predominantly composed of lath-shaped plagioclase (44%) and elongate
  to equant pyroxene (44%) with mesostasis (10%) and minor opaques
  (2%). Pyroxenes are unzoned with respect to Mg/Fe and are dominantly
  composed of low-Ca clinopyroxene with fine (&lt;1 micrometer thick)
  augite exsolution lamellae that causes electron microprobe analyses
  to range in apparent composition from Wo(sub)2.0En(sub)46.5 to
  Wo(sub)32.7En(sub)33 7. These compositions are distinctly more
  magnesian than pyroxene in "main group" eucrites [6]. Plagioclase
  composition ranges from An77.4 to An88.7. REE abundances are
  ~26x chondrite with a signifilcant negative Eu anomaly. Electron
  microprobe analyses of fused beads indicate that bulk Mg# of this
  clast is ~49. Given the narrow width of alteration rims on Petersburg
  eucrite clasts, the large size of clast A (&gt;0.6 g), and the fact
  that INAA and fused bead samples were obtained from the interior of
  clast A, bulk clast compositions were unaffected by the metamorphic
  redistribution of Fe/Mg described above. Stolper [7] suggested that
  eucrites Stannern and Sioux County represented increasing degrees
  of partial melting of similar source areas; other eucrites (e.g.,
  Nuevo Laredo) represented fractionation of Sioux County-like liquids
  (Fig. l). Later studies demonstrated the presence of eucritic materials
  that could not easily be explained by this interpretation. Clast RC03
  from Petersburg [5] and clast CF3 from Kapoeta [8] were interpreted
  as derived from different source regions than other noncumulate
  eucrites, based on major and trace element compositions. Hewins [4]
  came to a similar conclusion for eucritic clasts in Petersburg based
  on anomalously high Ni/Co ratio of clast metal. Warren et al.[9],
  however, interpreted the REE-rich -21x chondrite), but magnesian
  (Mg# ~45) eucrite Pomozdino as a partial cumulate, a mixture of
  Stannern-like melt and cumulate material. Such an interpretation is
  difficult to reconcile with data for clast A from Petersburg, since
  bulk composition is more REE rich and yet more magnesian than that of
  Pomozdino. Assuming Binda-like cumulate material, modeling of this
  composition requires mixture with liquid that is more REE rich than
  any eucritic matenal yet analyzed. Clast A may represent a very low
  proportion partial melt of a source that has chondritic REE abundances,
  but is significantly more magnesian than the source from which the
  "main group" eucrites were derived. Intermediate-composition matrix
  pyroxenes in Petersburg are derived at least in part from materials
  that have trace element compositions similar to Stannern, but are more
  magnesian. Some smaller (&lt;60 micrometers) matrix pyroxene grains
  probably have compositions that are largely the result of redistribution
  of Fe/Mg during metamorphism after breccia accumulation. There is
  no evidence that any of the intermediate-composition pyroxenes in
  the matrix of Petersburg were derived from zoned pyroxenes similar
  to those in Pasamonte. References: [l] Labotka T. C. and Papike
  J. J. (1980) Proc. LPSC 11th, 1103-1130. [2] Fuhrman M. and Papike
  J. J. (1981) Proc. LPSC 12th, 1257-1279. [3] Hewins R. H. (1979)
  LPS X, 543-545. [4] Hewins R. H. (1979) GCA, 43, 1663-1673. [5]
  Mittlefehldt D. W. (1979) GCA, 43, 1917-1935. [6] BVSP (1981)
  Basaltic Volcanism on the Terrestrial Planets, Pergamon. [7]
  Stolper E. (1977) GCA, 41, 587-611. [8] Smith M. R. (1982) Ph.D
  dissertation, Oregon State University. [9] Warren P. H. et al. (1990)
  Proc. LPSC 20th, 281-297. [10] Christophe Michel-Levy M. et al. (1987)
  Bull. Mineral., 110, 449-458. [11] Hamet J. et al. (1978) Proc. LPSC,
  9th, 1115-1136. [12] Jerome D. Y. (1970) Ph.D. dissertation, University
  of Oregon. [13] McCarthy T. S. et al. (1973) EPSL, 18, 433-442. [14]
  Palme H. et al. (1978) Proc. LPSC, 9th, 25-57. [15] Wanke H. et
  al. (1974) Proc. LSC, 3rd, 1251-1268. [16] Warren P. H. and Jerde
  E. A. (1987) GCA, 51, 713-725.

---------------------------------------------------------
Title: Parental Magma Compositions of Basalts Using an Artificial
Neural Network: Theory
Authors: Woronow, A.; Reid, A. M.; Jones, J. H.; Pingitore, N. E., Jr.
1994LPI....25.1513W    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Time-series analysis of the O4 supergiant Zeta Puppis
Authors: Reid, A.
1994IAUS..162..112R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Carbonaceous Chondrite Clasts in the Howardites Bholghati
    and EET87513
Authors: Buchanan, P. C.; Zolensky, M. E.; Reid, A. M.
1993Metic..28..659B    Altcode:
  Twenty-two carbonaceous chondrite clasts from the two howardites
  Bholghati and EET87513 were analyzed. Clast N from EET87513 is a
  fragment classified as CM2 material on the basis of texture, bulk
  composition, mineralogy, and bulk O isotopic composition. Carbonaceous
  chondrite clasts from Bholghati, for which less data are available
  because of their small size, can be divided into two petrologic
  types: C1 and C2. C1 clasts are composed of opaque matrix with
  rare coarse-grained silicates as individual mineral fragments;
  textures resemble CI meteorites and some dark inclusions from CR
  meteorites. Opaque matrix is predominantly composed of flaky saponite;
  unlike typical CI and CR meteorites, serpentine is absent in the samples
  we analyzed. C2 clasts contain chondrules, aggregates, and individual
  fragments of coarse-grained silicates in an opaque matrix principally
  composed of saponite and anhydrous ferromagnesian silicates with flaky
  textures similar to phyllosilicates. These anhydrous ferromagnesian
  silicates are interpreted as the product of heating of pre-existing
  serpentine. The carbonaceous chondrite clasts we have studied from these
  two howardites are, with one notable exception (clast N from EET87513),
  mineralogically distinct from typical carbonaceous chondrites. However,
  these clasts have very close affinities to carbonaceous chondrites
  and have also experienced thermal metamorphism and aqueous alteration,
  but to different degrees.

---------------------------------------------------------
Title: Time-Series Observations of O Stars. II. Optical Observations
    of zeta Ophiuchi
Authors: Reid, A. H. N.; Bolton, C. T.; Crowe, R. A.; Fieldus, M. S.;
   Fullerton, A. W.; Gies, D. R.; Howarth, I. D.; McDavid, D.; Prinja,
   R. K.; Smith, K. C.
1993ApJ...417..320R    Altcode:
  We present photopolarimetry and extensive high-resolution,
  high-signal-to-noise optical spectroscopy of the rapidly rotating late
  O-type star Ζ Ophiuchi (HD 149757). The polarimetric data show no
  substantial variability over 1 week (σ<SUB>p</SUB> &lt; 0.04%), while
  the spectroscopic data show characteristic line-profile variations in
  the form of "bumps" migrating from blue to red on typical time scales
  of several hours. These variations are relatively strong (amplitude
  ∼1% of the continuum level) in He I λ4471, and Si III λλ4552,
  4567, 4575. They are seen at lower amplitudes in Mg II λ4481, but
  are almost undetectable (amplitude ≲0.3%) in He II λλ4541, 4686
  and N III λλ4511, 4515, 4518. We attribute this to a combination
  of equatorial gravity darkening and a latitudinally confined origin
  of the variations. <P />Using a Fourier CLEAN technique, it is shown
  that the line-profile variations can be adequately represented as
  a set of sinusoids. The periods, combined with an estimate of the
  rotational period, lead us to rule out rotational modulation as the
  origin of the variability. The phase changes of the sinusoids across the
  line-profiles indicate a repetitive pattern, consistent with sectorial
  (1 = -m) nonradial pulsation. We find four periods: P = 3.339 hr (|m|
  = 4), 2.435 hr (|m| = 5 or 6), 1.859 hr (|m| = 9±1), and either 1.366
  or 1.292 hr (|m| = 11±1). The "superperiods," P|m|, may be nearly
  commensurate (at ∼13-14 hr), but that commensurability is not exact.

---------------------------------------------------------
Title: Time-Series Observations of O Stars. III. IUE and HST
    Spectroscopy of zeta Ophiuchi and Implications for the “Photospheric
    Connection”
Authors: Howarth, Ian D.; Bolton, C. T.; Crowe, R. A.; Ebbets, D. C.;
   Fieldus, M. S.; Fullerton, A. W.; Gies, D. R.; McDavid, D.; Prinja,
   R. K.; Reid, A. H. N.; Shore, S. N.; Smith, K. C.
1993ApJ...417..338H    Altcode:
  Stellar-wind variability in the archetypal nonradially pulsating O star
  ζ Oph (09.5 V) is discussed on the basis of new time-series lUE and HST
  spectroscopy and archival results. Time-variable "discrete absorption
  components" are first observed at high velocities (≳ 10<SUP>3</SUP>
  km s<SUP>-1</SUP> ≃ 0.8υ<SUB>∞</SUB>) and then migrate blueward;
  the recurrence time scale for the phenomenon is ∼20 hr. This is
  the first record of this type of variability in a luminosity-class V
  star and provides support for the previously inferred ubiquity of such
  behavior across the 0-star regime. The accelerations are slower than
  predicted by steady state wind models and are unlikely to represent
  the time-averaged velocity law of the outflow. The UV results are
  discussed in the context of simultaneous optical observations (Paper
  II); no evidence is found to suggest that nonradial pulsations have any
  direct role in determining the gross observational characteristics of
  discrete absorption components, on either long (years) or short (hours)
  time scales. The line-driven instability provides a promising mechanism
  to account for variability observed in the UV P Cygni profiles of ζ
  Oph, and, by extension, in all other O stars.

---------------------------------------------------------
Title: Limits on mode identifications in rotating, non-radially
    pulsating stars.
Authors: Reid, A. H. N.; Aerts, C.
1993A&A...279L..25R    Altcode:
  We present CLEAN time-series analysis of synthetic line profiles
  obtained from a non-radially pulsating stellar model which incorporates
  effects of rotation. Two models (a low-degree l = 2, m = -1; and
  a high degree l = -m = 8) were calculated for a rapidly rotating
  late O-type star, where the prograde oscillation frequency in the
  corotating frame of the star is twice that of the stellar rotation
  frequency. An interpretation of the results based upon the usual
  slow-rotation assumptions gives a mis-identification of both period
  and mode of oscillation for the low-degree model, but correctly
  identifies the non-radial pulsation (NRP) characteristics of the
  sectorial model. The mis-identification of the low-degree model has
  possible implications for previous mode identifications, and we urge
  caution when analyzing the line profile variations of rapidly-rotating,
  non-radially pulsating stars.

---------------------------------------------------------
Title: Original Size of the Vredefort Structure, South Africa
Authors: Therriault, A. M.; Reid, A. M.; Reimold, W. U.
1993LPI....24.1419T    Altcode:
  The Vredefort structure is located approximately 120 km southwest of
  Johannesburg, South Africa, and is deeply eroded. Controversies remain
  on the origin of this structure with the most popular hypotheses being:
  (1) by impact cratering about 2.0 Ga; (2) as a cryptoexplosion structure
  about 2.0 Ga; and (3) by purely tectonic processes starting at about
  3.0 Ga and ending with the Vredefort event at 2.0 Ga. In view of recent
  work in which the granophyre dikes are interpreted as the erosional
  remants of a more extensive impact melt sheet, injected downward
  into the underlying country rocks, the impact origin hypothesis for
  Vredefort is adopted. In order to estimate the original dimensions of
  the Vredefort impact structure, it is assumed that the structure was
  initially circular, that its predeformation center corresponds to the
  center of the granitic core, and that the pre-Vredefort geology of the
  area prior to approximately 2.0 Ga ago is as suggested by Fletcher and
  Reimold. The spatial relationship between shock metamorphic effects,
  the shock pressures they record, and the morphological features of the
  crater were established for a number of large terrestrial craters. The
  principles of crater formation at large complex impact structures
  comparable in size to Vredefort were also established, although many
  details remain unresolved. An important conclusion is that the transient
  crater, which is formed directly by excavation and displacement by the
  shock-induced cratering flow-field (i.e., the particle velocity flow
  field existing in the region of the transient crater but behind the
  initial outgoing shock front), is highly modified during the late stage
  processes. The original transient crater diameter lies well within the
  final rim of the crater, which is established by structural movements
  during late-stage cavity modification.

---------------------------------------------------------
Title: Characterization of the Marquez Dome buried impact crater
    using gravity and magnetic data
Authors: Wong, A. M.; Reid, A. M.; Hall, S. A.; Sharpton, V. L.
1993LPI....24.1533W    Altcode:
  The buried impact crater, Marquez Dome, located in Leon County in
  east central Texas, is an approximately 15 km diameter structure whose
  central uplift is now partially exposed due to headward erosion of the
  post-impact cover. The central uplift is approximately 3 km in diameter
  and the rocks within it have been uplifted more than 1200 m above their
  regional level. The crater rim remains buried and previous attempts
  to determine its location have had to rely on seismic reflection data
  and geologic well logs. These attempts have been somewhat successful
  in mapping the extent of the disturbed zone around Marquez Dome,
  but more limited in their ability to image the shallow buried rim. In
  an attempt to define accurately the whole Marquez Dome structure and
  assist in the selection of drilling sites, a geophysical investigation
  involving gravity and magnetic data over the central uplift and the
  surrounding area has been undertaken.

---------------------------------------------------------
Title: EET87513 Clast N: A CM2 Fragment in an HED Polymict Breccia
Authors: Buchanan, P. C.; Zolensky, M. E.; Reid, A. M.; Barrett, R. A.
1993LPI....24..209B    Altcode:
  Xenoliths of material resembling carbonaceous chondrites have been
  found in several HED polymict breccias. Most workers concluded that
  these clasts are related to CM2 meteorites on the basis of texture, bulk
  composition, and mineralogy. Data on clast N, a carbonaceous chondrite
  fragment from the howardite EET87513 large enough (approximately 4x5mm
  on the surface of the slab from which it was separated) to extract
  bulk samples for INAA and oxygen isotope analysis and to provide
  a thin section for electron microprobe, SEM, and TEM analysis is
  reported. Preliminary data for this clast were previously reported. INAA
  was performed at Oregon State University and bulk oxygen isotopic
  composition was determined at the University of Chicago. These data
  confirm that EET87513 clast N is a fragment of CM2 material.

---------------------------------------------------------
Title: Origin of the Vredefort Structure, South Africa: Impact Model
Authors: Therriault, A. M.; Reid, A. M.; Reimold, W. U.
1993LPI....24.1421T    Altcode:
  A model is presented for the evolution of the Vredefort structure, based
  on reasoned constraints on the original size of the Vredefort structure
  from observational data and comparison with other terrestrial impact
  craters. The models for complex craters (ring and multi-ring basins)
  of Croft, Grieve, and co-workers, and Schultz and co-workers, were
  used to reconstruct the Vredefort impact event, using a final crater
  diameter of 300 km, as estimated by Therriault. The sequence of events
  (stages 2-5) is illustrated diagramatically. The stages are: initial
  penetration, excavation and compression, dynamic rebound and uplift,
  maximum radial growth and collapse, and final crater form.

---------------------------------------------------------
Title: Time-Series Spectroscopy of Sigma Ophiuchi
Authors: Reid, A. H. N.; et al.
1993npsp.conf..190R    Altcode: 1993IAUCo.139..190R
  No abstract at ADS

---------------------------------------------------------
Title: Impactite and pseudotachylite from Roter Kamm Crater, Namibia
Authors: Degenhardt, J. J., Jr.; Buchanan, P. C.; Reid, A. M.
1992lmip.conf...20D    Altcode:
  Pseudotachylite is known to occur in a variety of geologic settings
  including thrust belts (e.g., the Alps and the Himalayas) and impact
  craters such as Roter Kamm, Namibia. Controversy exists, however, as
  to whether pseudotachylite can be produced by shock brecciation as
  well as by tectonic frictional melting. Also open to debate is the
  question of whether pseudotachylites form by frictional fusion or
  by cataclasis. It was speculated that the pseudotachylite at Roter
  Kamm was formed by extensional settling and adjustment of basement
  blocks during 'late modification stage' of impact. The occurrence
  of pseudotachylite in association with rocks resembling quenched
  glass bombs and melt breccias in a relatively young crater of known
  impact origin offers a rare opportunity to compare features of these
  materials. Petrographic, x-ray diffraction, and electron microprobe
  analyses of the impactites and pseudotachylites are being employed to
  determine the modes of deformation and to assess the role of frictional
  melting and comminution of adjacent target rocks.

---------------------------------------------------------
Title: Mg/Si in the Earth, Planets, and Meteorites
Authors: Jakes, P.; Reid, A. M.
1992Metic..27R.239J    Altcode:
  The "primitive materials," i.e., carbonaceous chondrites (CV,CI,CM) [1]
  and interplanetary dust particles [2,3] have Mg/Si ratios similar to
  those of the solar photosphere [1]. The bulk composition of the Earth
  and that of the terrestrial planets are believed to have higher than
  "primitive" Mg/Si ratios [4], whereas ordinary and enstatite chondrites
  have lower than primitive Mg/Si ratios [5]. The separation of Mg from
  Si may result from reduction of silicon into a metallic phase through
  the reaction of silicates with C or H2(6) or through temperature-induced
  reduction of silicates (oxygen volatilization) [7,8]. Reduction leads to
  the formation of a residuum with higher than original Mg/Si ratios. High
  temperatures may also cause the vaporization of silicon and also lead
  to higher Mg/Si ratios in the residual phase [4]. Lower Mg/Si ratios
  could result from partial melting of a primitive material in which
  Si preferentially enters the melt, leaving a high Mg/Si residuum. The
  recrystallization of silicon- bearing metal in the presence of silicates
  may also provide a mechanism to decrease Mg/Si ratios. This process
  is documented by the presence of silica/silicates in the meteoritic
  metals (CV3 Leoville and Efremovka and other chondrites, e.g., Renazzo,
  ALH85085 [9]). Since Mg/Si fractionation may result from the extreme
  temperatures, the other siderophile and volatile element abundances must
  also be considered. The high contents of volatile elements in enstatite
  chondrites exclude the possibility of such high-temperature processes,
  and condensation under highly reducing conditions best explains
  the observed abundances. The aubrites, i.e., enstatite achondrites,
  however, all have attributes of high-T, low f[O(sub)2] processing and
  may have formed through the recrystallization of superheated highly
  fractionated (planetary processed?) material. An explanation of the
  Earth's higher than primitive Mg/Si was sought in the differences
  of volatility of Si and Mg, and hence in the thermal regime during
  the formation of the early solar system [4] and in the siderophile
  behavior of Si under reducing conditions [10]. Since Palme and Nickel
  [5] have shown that the Mg number (Mg/Si ratio) in the upper mantle of
  the Earth relates to the degree of fractionation of the mantle, e.g.,
  to Ca/Al ratios. The explanation of different Mg/Si ratios between
  the primitive chondrites and Earth's mantle could be found in mantle
  fractionation, i.e., the formation of the Earth's crust. We argue for
  the chondritic composition of the Earth in respect of Mg/Si and that
  the ancient upper mantle was significantly fractionated prior to 3.9 AE
  [11,12,13]. The early fractionation is reflected in the high Mg/Si of
  the present peridotitic mantle. The upper mantle has been fractionated
  throughout geologic time due to the formation of the basaltic melts
  that contribute to the growth of the Earth's crust. These melts
  are rich in Si relative to Mg, whereas the residuum is rich in Mg
  relative to Si. The early melts were either erupted on the surface
  or retained within the mantle. The erupted portion may be returned to
  the mantle in the form of eclogite in the same way that recent oceanic
  "basaltic" crust (with eclogite mineralogy) is recycled to the mantle
  [14]. Since the eclogites do not completely homogenize with the upper
  mantle and retain their petrological and geochemical identity [15],
  the formation of basalts (eclogites) strongly influences the Mg/Si
  ratio of the noneclogitic, i.e., peridotite mantle (residual mantle has
  higher Mg/Si whereas basalt has lower Mg/Si than the original parent
  rock). The "lost" crustal component [11] (3.9 AE old) may be present
  in the upper mantle (transition) zone in its eclogitic (or griquaitic)
  form. We suggest therefore that sampling of the upper mantle through the
  analysis of pristine peridotites does not represent the bulk mantle but
  represents only one major mantle component. Mantle sampling is biased
  toward the rocks we interpret as primitive. The Earth's upper mantle may
  well be chondritic in respect to Mg/Si, if the eclogites present are
  added back into the estimates of mantle composition. References. [1]
  Anders E. and Grevesse N. (1989), Geochim. Cosmochim. Acta, 53,
  197-214. [2] Rietmeijer F.J.M. (1987), Abs. LPSC 18, 832-833. [3] Dikov
  P.Yu. et al. (1990), Geokhimiya, 789-795. [4] Ringwood A.E. (1989),
  Earth Planet. Sci. Lett., 95, 1-7. [5] Palme H. and Nickel K.G. (1985),
  Geochim. Cosmochim. Acta, 49, 2123-2132. [6] Baedecker P.A and Wasson
  J.T. (1975), Geochim. Cosmochim. Acta, 39, 735-765. [7] Jakes P. et
  al., (1992), Abs. LPSC 23, 599-600. [8] Dickinson T.L. et al.,
  (1992), Abs. LPSC 23, 309-310. [9] Zanda B. (1992), Abs. LPSC 23,
  1569-1570. [10] Wanke H.(1981), Phil. Trans. R. Soc. Lond., A 303,
  287-302. [11] Harper C.L. and Jacobsen S.B. (1992), EOS, 323. [12]
  Collerson K.D. et al. (1991), Nature, 349, 209-214. [13] Galer S.G.G
  and Goldstein S.L. (1991), Geochim. Cosmochim. Acta, 55, 227-239. [14]
  Ringwood A.E. [15] Hatton C.J. and Gurney J.J. (1987), in Mantle
  xenoliths P.H. Nixon ed., John Wiley &amp; Sons.

---------------------------------------------------------
Title: Time Series Observations of O Stars. I. IUE Observations of
    Variability in the Stellar Wind of zeta Puppis
Authors: Prinja, R. K.; Balona, L. A.; Bolton, C. T.; Crowe, R. A.;
   Fieldus, M. S.; Fullerton, A. W.; Gies, D. R.; Howarth, I. D.; McDavid,
   D.; Reid, A. H. N.
1992ApJ...390..266P    Altcode:
  Stellar wind variability in Zeta Pup (O4 I(n)f) is described based on
  31 high-resolution IUE observations secured over 5 1/2 days in 1989
  April. Extensive changes are evident in the absorption regions of Si
  IV 1393.76, 1402.77A and N IV 1718.55A P Cygni profiles. Both lines
  exhibit similar patterns of variability, which are characterized by the
  development and subsequent blueward migration, of discrete absorption
  components. The formation of four discrete features is identified
  over about 2.2 days of intensive observations, with a recurrence
  time of about 15 hr. The time scales, velocities, and accelerations
  of the progressive absorption enhancements are determined. These
  changes are accompanied by fluctuations of up to about 200 km/s in
  the maximum observed blue edge velocities in saturated C IV and N V
  P Cygni profiles.

---------------------------------------------------------
Title: Matrix Pyroxenes in Howardites and Polymict Eucrites
Authors: Buchanan, P. C.; Reid, A. M.
1992LPI....23..173B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Mineralogy of Dark Clasts in CT Chondrites, Encrites and
    Howardites
Authors: Zolensky, M. E.; Weisberg, M. K.; Buchanan, P. C.; Prinz,
   M.; Reid, A.; Barrett, R. A.
1992LPI....23.1587Z    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Excess Heat and the Early Planet Evolution
Authors: Jakes, P.; Reid, A. M.; Casanova, I.
1992LPI....23..597J    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Silicate Melts at Super Liquidus Temperatures: Reduction
    and Volatilization
Authors: Jakes, P.; Sen, S.; Matsuishi, K.; Reid, A. M.; King, E. A.;
   Casanova, I.
1992LPI....23..599J    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Three New Chondrites from Namibia
Authors: Reid, A. M.; Jakes, P.; Zolensky, M. E.; Miller, R.
1992LPI....23.1135R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: A Magnetic Survey Across the Roter Kamm Impact Crater, Namibia
Authors: Reimold, W. U.; Reid, A. M.; Jakes, P.; Zolensky, M. E.;
   Miller, R.
1992LPI....23.1143R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: "Bronzite" Granophyre: New Insight on Vredefort
Authors: Therriault, A. M.; Reid, A. M.
1992LPICo.790...72T    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Impactite and Pseudotachylite from Roter Kamm Crater, Namibia
Authors: Degenhardt, J. J., Jr.; Buchanan, P. C.; Reid, A. M.
1992LPICo.790...20D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Bronzite Granophyre: New insight on Vredefort
Authors: Therriault, A. M.; Reid, A. M.
1992lmip.conf...72T    Altcode:
  The Vredefort Dome is located near the center of the Witwatersrand
  Basin, about 120 km southeast of Johannesburg, South Africa. Its
  origin is enigmatic, ranging from a major impact event to endogenous
  processes, either igneous or tectonic. A unique melt rock, the
  'Bronzite' Granophyr, occurs in the Vredefort structure as vertical
  ring dikes along the contact between sedimentary collar and core of
  Archaean granites, and as vertical dikes extending northwest-southeast
  and northeast-southwest in the granitic core. The granophyre rocks
  have an unusual composition and high content of recrystallized
  sedimentary inclusions compared to common intrusive igneous rocks
  with similar SiO2 content (61 to 70 percent by weight). The unique
  nature of the granophyre has been underlined in previous studies
  and origin hypotheses as an impact melt or as a highly contaminated
  intrusive mafic magma have also been discussed. We present new results
  obtained from a recent detailed petrographic and geochemical study of
  a very large and texturally diverse suite of 'Bronzite' Granophyre,
  representing all dikes occurring at Vredefort.

---------------------------------------------------------
Title: Eucrite and Diogenite Clasts in Three Antarctic Achondri2tes
Authors: Buchanan, P. C.; Reid, A. M.
1991LPI....22..149B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Bholghati howardite: Petrography and mineral chemistry
Authors: Reid, A. M.; Buchanan, Paul; Zolensky, M. E.; Barrett, R. A.
1990GeCoA..54.2161R    Altcode:
  A 10 g sample of the Bholghati howardite was disaggregated in order
  to separate two eucrite clasts, several small carbonaceous clasts,
  fragments of diogenitic pyroxene, and bulk matrix. The eucrite clasts
  show evidence of moderately rapid cooling from a melt, followed
  by prolonged subsolidus annealing. The carbonaceous clasts mostly
  resemble CM2 carbonaceous chondrites with low-iron silicates and
  Fe-Ni sulphides in a fine grained dark matrix. One clast, however,
  is mineralogically, petrographically, and compositionally similar
  to a CI 1 chondrite. Both carbonaceous and eucritic clasts have a
  complex history prior to incorporation into the howardite matrix
  with no evidence of significant metamorphism since assembly. Most
  clasts in the howardite breccia are monomineralic, with pyroxene
  and plagioclase pre-dominant. Pyroxenes range from 'diogenitic' to
  'eucritic' with diogenitic compositions most abundant; a significant
  number of intermediate compositions are present, consistent with
  derivation from a series of rocks related by fractionation.

---------------------------------------------------------
Title: Clast Populations in Three Antarctic Achondrites
Authors: Buchanan, B. C.; Reid, A. M.; Schwarz, C.
1990LPI....21..141B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Observations on Granitic Clasts in Granphyre from the Vredefort
    Dome, South Africa
Authors: Reimold, W. U.; Reid, A. M.; Therriault, A. M.
1990LPI....21.1009R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Carbonaceous fragments in the Bholghati howardite
Authors: Reid, A. M.; Buchanan, P. C.; Barrett, R. A.; Zolensky, M. E.
1989Metic..24R.319R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Four Year Modulation of Periodic Radio Outbursts from LSI
    +61 degrees 303
Authors: Gregory, P. C.; Xu, Huang-Jian; Backhouse, C. J.; Reid, A.
1989ApJ...339.1054G    Altcode:
  New 6 cm observations of the binary radio, X-ray, and gamma-ray
  star LSI + 61 deg 303 obtained in August 1984 and September 1986
  are presented. The data accumulated to date provide evidence for a
  strong modulation in the amplitude of the 26.496 day periodic radio
  outbursts. The modulation occurs on a time scale of 4 yr. Two possible
  explanations are considered: (1) variable beaming from a precessing
  relativistic jet and (2) variable accretion due to quasi-cyclic Be
  star envelope variations.

---------------------------------------------------------
Title: The Bholghati Howardite: Petrography and Mineral Chemistry
Authors: Reid, A. M.; Buchanan, P.
1989LPI....20..892R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Carbonaceous Fragments in the Bholghati Howardite
Authors: Reid, A. M.; Buchanan, P. C.; Barrett, R. A.; Zolensky, M. E.
1989LPICo.712..206R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Pink Spanel Troctolites in Apollo 14 Breccias
Authors: Collins, D. T.; Reid, A. M.
1989mtak.conf...26C    Altcode: 1989LPITR8903...26C
  No abstract at ADS

---------------------------------------------------------
Title: The Bholghati Consortium: Preliminary Chemical and Petrologic
    Characterization of the Bholghati Howardite
Authors: Gosselin, D. C.; Laul, J. C.; Smith, M. R.; Reid, A. M.
1988Metic..23Q.270G    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Dynamic Crystallization Experiments on Chondrule Melts of
Porphyritic Olivine Composition: Comparison of Olivine Compositions
    from Natural and Experimentally Produced Chondrules
Authors: Lofgren, G. E.; Reid, A. M.
1988LPI....19..688L    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Bholghati Consortium: Preliminary Chemical and Petrologic
    Characterization of the Bholghati Howardite
Authors: Gosselin, D. C.; Laul, J. C.; Smith, M. R.; Reid, A. M.
1988LPICo.665E..13G    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Composition of gold grains in the Vaal Placer, Klerksdorp,
    South Africa
Authors: Reid, A. M.; Le Roex, A. P.; Minter, W. E. L.
1988MinDe..23..211R    Altcode:
  Separated gold grains from 94 samples of the Vaal Placer, Klerksdorp
  gold field, South Africa have been analyzed for Au, Ag and Hg. Average
  gold grain compositions in these samples range from 80 to 95 weight
  percent Au, 4 to 18 weight percent Ag and 0.5 to 4 weight percent
  Hg with an average composition around Au 90, Au 8, Hg 2. Individual
  grains are homogeneous but significant differences exist between gold
  grains from single small samples and also between average compositions
  in separate samples. The data do not fit any simple model of gold
  compositional control by provenance or by metamorphic homogenization.

---------------------------------------------------------
Title: Variable radio source GT0116+622 is a possible counterpart
    to Cas γ-1
Authors: Gregory, P. C.; Duric, N.; Reid, A.; Picha, J.; Stevenson, T.
1986Natur.323..602G    Altcode:
  Identification of celestial γ-ray sources has proved to be
  very difficult because of the large positional uncertainties
  (typically several degrees) and the transient nature of many of these
  objects. Highly variable radio emission is a striking characteristic
  of the most secure source of very high-energy radiation, Cygnus X-3
  (ref. 1). Here we report the discovery of another highly variable
  radio source which coincides in position with the transient TeV γ-ray
  source Cas γ-1. We have obtained an accurate radio position with the
  Very Large Array (VLA) telescope but no optical counterpart was found
  on the Mount Palomar Sky Survey prints. We have also obtained upper
  limits on radio emission from the binary X-ray pulsar, 4U0115+634,
  another proposed identification for Cas γ-1.

---------------------------------------------------------
Title: Compositions of 7 Allan Hills polymict eucrites and one
    diogenite
Authors: Reid, A. M.; Le Roex, A. P.
1984LPICo.537E..64R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Ferrobasalts from the Spiess Ridge segment of the Southwest
    Indian Ridge
Authors: le Roex, A. P.; Dick, H. J. B.; Reid, A. M.; Erlank, A. J.
1982E&PSL..60..437L    Altcode:
  Highly vesicular, microporphyritic basaltic rocks have been dredged
  from the slow-spreading Spiess Ridge segment of the Southwest Indian
  Ridge. All the samples recovered are hyalocrystalline with plagioclase,
  clinopyroxene and olivine as phenocryst and microphenocryst
  phases. Titanomagnetite occurs as euhedral microphenocrysts in
  some of the more evolved samples. In terms of bulk rock and quench
  glass chemistry the lavas are characterised by highly evolved
  compositions(e.g. FeO*=10.3-14.2%;TiO <SUB>2</SUB>=2.0-3.4%;K
  <SUB>2</SUB>O=0.50-1.1%;MgO=6.0-3.5%;Zr=160-274ppm;Nb=14-32ppm)
  and can be classified as ferrobasalts. Isotopic and
  incompatible element ratios of the lavas(e.g. <SUP>87</SUP>Sr/
  <SUP>86</SUP>Sr=0.70325-0.70333;Zr/Nb=8.4-11.3;Y/Nb=2.3-1.4)
  indicate their strongly "enriched" nature (see also Dickey et
  al. [6]). Quantitative major and trace element modelling indicates
  that most of the compositional variations observed can be attributed to
  low-pressure fractional crystallisation of plagioclase, clinopyroxene
  and minor olivine and titanomagnetite. The range in composition can
  be accounted for by up to 65% fractional crystallisation. We suggest
  that the extreme differentiation of the Spiess Ridge lavas is related
  not to spreading rate, but to rate of magma supply. The basaltic
  melts appear to have evolved in a newly established zone of magmatic
  activity, associated with the most recent northward jump of the Bouvet
  triple junction, where they were effectively isolated from significant
  admixture of primitive magmas.

---------------------------------------------------------
Title: Analysis of palaeomagnetic inclination data
Authors: McFadden, P. L.; Reid, A. B.
1982GeoJ...69..307M    Altcode: 1982GeoJI..69..307M
  No abstract at ADS

---------------------------------------------------------
Title: Descriptions of stony meteorites
Authors: Score, R.; King, T. V. V.; Schwarz, C. M.; Reid, A. M.;
   Mason, B.
1982mvla.rept...19S    Altcode:
  The individual specimens, arranged by class are described. Within the
  chondrites, the specimens are grouped according to the Van Schmus-Wood
  classification, and the descriptions follow the order of increasing
  petrographic type. The original weight of the specimen is given to
  the nearest gram (nearest 0.1 gram for specimens weighing less than
  100 grams). Material on al characterized meteorites collected together
  with descriptions of some meteorites is included. Specimens weighing
  less than 100 grams are listed without descriptions, unless they show
  distinctive features.

---------------------------------------------------------
Title: Basaltic Achondrite Meteorites from the Antarctic
Authors: Reid, A. M.
1982AntJ...16...65R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Overview of Antarctic achondrites
Authors: Reid, A. M.
1982mvla.rept...59R    Altcode:
  The distribution of achondrite classes in the Antarctic and
  non-Antarctic collections are compared. The numbers in the non-Antarctic
  column are an unreliable guide to the real distribution of achondrite
  types in the total terrestrial infall because of the vagaries of
  observation, recognition, and recovery. The Antarctic meteorites
  provide a better guide since they are more easily recognized and are
  all carefully studied and cataloged. There remarked differences between
  the Antarctic and non-Antarctic achondrite collections. Diogenites
  are more abundant inthe Antarctic collection, comprising over half
  the classified samples.

---------------------------------------------------------
Title: Igneous Layering in an Achondritic Meteorite
Authors: McSween, H. Y., Jr.; Reid, A. M.
1981Metic..16Q.359M    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Major Element Compositions and Rb-Sr, Sm-Nd Isotopic
    Systematics of Allan Hills Polymict Eucrites
Authors: Wooden, J. L.; Brown, R.; Bansal, B.; Shih, C. -Y.; Wiesmann,
   H.; Nyquist, L. E.; Reid, A. M.
1981Metic..16..404W    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: A preliminary report on the achondrite meteorites in the 1979
    U. S. Antarctic meteorite collection
Authors: Reid, A.; Score, R.
1981PolRe..20...33R    Altcode:
  Seventy-three meteorite samples were collected in Antarctica during
  the austral summer of 1979-80. A description is presented of the seven
  achondrites found among the meteorite samples. The achondrites described
  include an ALHA79017-polymict eucrite, an EETA79001-shergottite,
  an EETA79002-diogenite, an EETA79004-eucrite, an EETA79005-polymict
  eucrite, an EETA79006-howardite, and an EETA79011-polymict eucrite. The
  most exciting single aspect of the 1979 collection is undoubtedly the
  discovery of a new member of the shergottite group of meteorites. Sample
  EETA79001 is just under 8 kg and should thus provide ample material
  for detailed studies. In addition to the achondrites, a unique iron
  meteorite with abundant silicate (orthopyroxene) inclusions and a
  large diogenite is also discussed.

---------------------------------------------------------
Title: Chemical and Isotopic Studies of the Allan Hills Polymict
    Eucrites
Authors: Wooden, J.; Reid, A.; Brown, R.; Bansal, B.; Wiesmann, H.;
   Nyquist, L.
1981LPI....12.1203W    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Summary Statistics of 1977 and 1978 Antarctic Meteorite
    Collections and a Glimpse of the 1979 Collection
Authors: King, T. V. V.; Score, R.; Schwarz, C.; Reid, A. M.; Mason,
   B. H.
1980Metic..15..315K    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Antarctic polymict eucrites
Authors: Reid, A. M.; Schwarz, C. M.
1980LPICo.412..104R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Petrogenetic Models for Eucrite Genesis
Authors: Reid, A. M.; Duncan, A. R.; Le Roex, A.
1979LPI....10.1022R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Unequilibrated and Equilibrated Eucrites
Authors: Reid, A. M.; Barnard, B. M.
1979LPI....10.1019R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Major element composition in Luna 20 glasses.
Authors: Warner, J. L.; Reid, A. M.; Ridley, W. I.; Brown, R. W.
1979rhrm.conf..420W    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Abundance and composition of phases in the Luna 20 regolith
    45 - 125 µm fraction.
Authors: Reid, A. M.; Warner, J. L.; Ridley, W. I.; Brown, R. W.
1979rhrm.conf..372R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Non-Mare "Igneous" Clasts in Apollo 15 Breccias
Authors: Reid, A. M.; Richardson, S. H.; Duncan, A. R.
1977LPI.....8..801R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: In search of LKFM (low K Fra Mauro basalt).
Authors: Reid, A. M.; Duncan, A. R.; Richardson, S. H.
1977LPSC....8.2321R    Altcode:
  The term Low K Fra Mauro Basalt (LKFM) was first used by Reid et
  al. (1972) in connection with a study of glass compositions in the
  less than 1 mm fraction of three Apollo 15 soils. If the glass data
  have been interpreted correctly, then rocks of LKFM composition are a
  major component of the lunar crust. This interpretation is supported
  by the orbital X-ray and gamma-ray data which are consistent with the
  LKFM composition for several areas of the lunar surface. A description
  is presented of a search of Apollo 15 breccia samples for clasts which
  have igneous textures and are not obviously mare basalts. The objectives
  of this search were to assess the nature of nonmare igneous rocks in
  the Apollo 15 breccias and, in particular, to search for evidence of
  the elusive igneous LKFM. Reasonable evidence is found that rocks with
  the composition of LKFM are a major constituent of the lunar crust.

---------------------------------------------------------
Title: A description of two automated control systems for the
    electron microprobe
Authors: Frost, M. T.; O'Hara, K.; Suddaby, P.; Grant, G.; Reid,
   A. F.; Wilson, A. F.; Zuiderwyk, M.
1976XRS.....5..180F    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Characterization of crust formation on a parent body of
    achondrites and the moon by pyroxene crystallography and chemistry.
Authors: Takeda, H.; Miyamoto, M.; Ishii, T.; Reid, A. M.
1976LPSC....7.3535T    Altcode:
  Single crystal X-ray diffraction and electron microprobe techniques
  were used to study lunar crustal pyroxenes in a cataclastic norite,
  a pyroxene-rich clast, and anorthosite lunar samples, and also
  in meteorites including diogenites, eucrites, and the Yamoto (1)
  howardite. The crystallographic and chemical characteristics of
  pyroxenes in these materials are compared and are discussed in terms
  of the lower stability limit of pigeonite. A mechanical mixing model
  of howardite is proposed.

---------------------------------------------------------
Title: Aioun EL Atrouss: A New Hypersthene Achondrite with Eucritic
    Inclusions
Authors: Lomena, I. S. M.; Toure, F.; Gibson, E. K., Jr.; Clanton,
   U. S.; Reid, A. M.
1976Metic..11...51L    Altcode:
  Preliminary investigations have been made on two separate pieces
  from the Aioun el Atrouss meteorite that fell on April 17, 1974
  in southeast Mauritania. The major portion of the meteorite is a
  brecciated hypersthene achondrite with orthopyroxene (En74) as the
  major phase. Clasts of eucrite, up to 7 per cent in volume within
  a single slice, occur within the hypersthene achondrite host. No
  evidence has been found of reaction between the two meteorite types,
  nor of the presence of any materials intermediate in composition.

---------------------------------------------------------
Title: Cristallographic and chemical studies of a bronzite and
    chromite in the Yamato (B) achondrite.
Authors: Takeda, H.; Reid, A. M.; Yamanaka, T.
1976Metic..11..183T    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Nakhlites Part I: Petrography and Mineral Chemistry
Authors: Bunch, T. E.; Reid, A. M.
1975Metic..10..303B    Altcode:
  The two Nakhlite meteorites (Nakhla and Lafayette) are described,
  and their possible origin is discussed. It is shown that both objects
  are cumulates of clinopyroxene with augite as the major mineral and
  with lesser abundances of olivine, plagioclase, K-feldspar, Fe-Ti
  oxides, FeS, pyrite, chalcopyrite, and possibly iddingsite. Also,
  both meteorites are unbrecciated, and their texture is dominated by
  elongate subhedral to euhedral prisms of clinopyroxene. The data are
  shown to be compatible with the Nakhlites' being cumulative rocks from
  a common basaltic parent liquid. It is established that these objects
  are not of lunar origin, and it is concluded that the position of the
  parent body relative to other planetary bodies remains to be determined.

---------------------------------------------------------
Title: The Nakhlites Part II: Where, When and How
Authors: Reid, A. M.; Bunch, T. E.
1975Metic..10..317R    Altcode:
  The Nakhla and Lafayette meteorites are pyroxenite cumulates that
  show no simple relation to chondrites, basaltic achondrites, or lunar
  rocks. They present evidence of magma tic activity occurring on a
  highly differentiated parent body relatively late in the history of
  the solar system similar in some respects to the Earth.

---------------------------------------------------------
Title: A Geochemical and Petrographic Study of 1-2mm Fines from
    Apollo 17
Authors: Blanchard, D. P.; Korotev, R. L.; Brannon, J. C.; Jacobs,
   J. W.; Haskin, L. A.; Reid, A. M.; Donaldson, C. H.; Brown, R. W.
1975LPI.....6...57B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: A geochemical and petrographic study of 1 - 2 mm fines from
    Apollo 17.
Authors: Blanchard, D. P.; Korotev, R. L.; Brannon, J. C.; Jacobs,
   J. W.; Haskin, L. A.; Reid, A. M.; Donaldson, C. H.; Brown, R. W.
1975LPSC....6.2321B    Altcode:
  Samples of fines less than 1-mm and 155 1-2 mm particles from several
  Apollo 17 sites were analyzed for Na, Sc, Cr, Mn, Fe, Co, Ni, Hf,
  Ta, Th, and REE. Products of comminution and construction are present
  in the 1-2 mm particles, and the compositions of the rock fragments
  clearly indicate the general chemical characteristics of their parent
  rock types. The likely sources of materials for the glassy particles
  are considered. Glasses are enriched over their parent soils in Fe,
  Sc, Mn, and Cr, and are relatively enriched in light REE, so that some
  chemical fractionation accompanies glass-forming processes. Elements
  were determined by instrumental neutron activation analysis.

---------------------------------------------------------
Title: Crystallographic and chemical studies of a bronzite and
    chromite in the Yamato (B) achondrite.
Authors: Takeda, H.; Reid, A. M.; Yamanaka, T.
1975MNIPR...5...83T    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Nakhlites.
Authors: Bunch, T. E.; Reid, A. M.
1975Metic..10...92B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Phase chemistry of Apollo 14 soil sample 14259.
Authors: Aitken, F. K.; Anderson, D. H.; Bass, M. N.; Brown, R. W.;
   Butler, P., Jr.; Heiken, G.; Jakes, P.; Reid, A. M.; Ridley, W. I.;
   Takeda, H.; Warner, J.; Williams, R. J.
1974ModGe...5....1A    Altcode:
  Optical, X-ray-diffraction and electron-microprobe techniques were used
  to investigate 0.26 gm of Apollo 14 soil sample 14259. Major element
  microprobe analyses were made of 470 mineral grains and 388 glass
  grains. The mineral abundances in the soil are 45% plagioclase, 41%
  pyroxene, 7% olivine, 3% oxides, 2% K-feldspar; 1% nickel-iron, and
  less than 1% troilite. The glasses have a wide range of compositions
  but preferred values are evident and are interpreted as representative
  of rock types contributing to the soil at the Fra Mauro site. Eleven
  per cent of the glasses have compositions like those of mare basalts
  or mare soils and are believed to be mare-derived. Eighty-six per cent
  of the glasses are equivalent in composition to basalts that have
  higher Al, and lower Ca/Al and Fe/Mg ratios than mare basalts. The
  most abundant compositional type is named Fra Mauro basaltic glass and
  is subdivided into three related types. The other major glass type in
  the soil corresponds in composition to anorthositic gabbro.

---------------------------------------------------------
Title: Comparative Studies of Impact Glasses and Breccias
Authors: Fredriksson, K.; Brenner, P.; Nelen, J.; Noonan, A.; Dube,
   A.; Reid, A.
1974LPI.....5..245F    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Comparisons of Crystallographic and Chemical Characteristics
    of Pyroxenes Between Lunar Crustal Rocks and Achondrites
Authors: Takeda, H.; Ishii, T.; Reid, A. M.
1974LPI.....5..764T    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Chromium Partitioning Between Olivine and Pyroxene and the
    Redox State of Lunar Rocks
Authors: Jakes, P.; Reid, A. M.
1974LPI.....5..381J    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: A Refractory Glass Chondrule in the Vigarano Chondrite
Authors: Reid, A. M.; Williams, R. J.; Gibson, Everett K., Jr.;
   Fredriksson, Kurt
1974Metic...9...35R    Altcode:
  Vigarano, a type 3 carbonaceous chondrite, contains a chondrule composed
  of highly refractory Ca and Al rich glass with minor spinel. The
  chondrule formed from material similar to the Ca, M, Ti-rich aggregates
  that are common in Vigarano and other type 3 chondrites and formation
  of these refractory aggregates must predate formation of some Vigarano
  chondrules. Experiments with synthetic analogues and a comparison with
  studies in the system CaO-MgO-Al2O3-SiO2 indicate a temperature for
  formation of the chondrule at or above 1700 0Cfollowed by very rapid
  coo ling.

---------------------------------------------------------
Title: Luna 16 Revisited: The case for Aluminous Mare Basalts
Authors: Reid, A. M.; Jakes, P.
1974LPI.....5..627R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Rare Earth and Other Trace Elements in Some Individual 1-2MM
    Fines From Apollo 16 and 17
Authors: Haskin, L. A.; Blanchard, D. P.; Jacobs, J. W.; Korotev,
   R. L.; Herrmann, A. G.; Reid, A. M.
1974LPI.....5..310H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Crystal Chemical Control of Element Partitioning for Coexisting
    Pigeonite-Augite and Chromite-Ulvospinel
Authors: Takeda, H.; Miyamoto, M.; Reid, A. A.
1974LPI.....5..766T    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Apollo 16 1-2mm Fines, Sample 65702, Chemical and Petrographic
    Correlations
Authors: Reid, A. M.; Donaldson, C.; Jakes, P.; Brown, R. W.
1974LPI.....5..624R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Lunar petrology conference.
Authors: Ridley, W. I.; Reid, A. M.; Brett, P. R.
1974EOSTr..55....4R    Altcode:
  A Lunar Petrology Conference, sponsored by the Lunar Science Institute
  under NASA contract NSR-09-051-001 and attended by nearly 100
  scientists, was held from July 24 to 26, 1973, in Houston, Texas.The
  principal aim of the conference was to bring together penologists and
  geochemists active in lunar research to discuss the present status of
  lunar petrology. The emphasis was placed on discussion with a minimum
  of formal presentations. In each session two or three keynote speakers
  reviewed present knowledge and highlighted problem areas in order to
  encourage discussion. The 3-day meeting was characterized by lively,
  broad-ranging, often humorous discussion of a variety of problems. The
  following is a short synopsis of the major areas of discussion.

---------------------------------------------------------
Title: Crystal chemical control of element partitioning for coexisting
    chromite-ulvöspinel and pigeonite-augite in lunar rocks.
Authors: Takeda, H.; Miyamoto, M.; Reid, A. M.
1974LPSC....5..727T    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Feldspar basalts in lunar soil and the nature of the lunar
    continents
Authors: Reid, A. M.; Ridley, W. I.; Harmon, R. S.; Warner, J.; Brett,
   R.; Jakes, P.; Brown, R. W.
1974lssf.book..122R    Altcode:
  It is found that 25% on the Apollo-14 glasses have the same composition
  as the glasses in two samples taken from the Luna-16 column. The
  compositions are equivalent to feldspar basalt and anorthosite gabbro,
  and are similar to the feldspar basalts identified from Surveyor-7
  analysis for lunar continents.

---------------------------------------------------------
Title: Apollo 17 Lunar Samples: Chemical and Petrographic Description
Authors: Apollo 17 Preliminary Examination Team; Gast, P. W.; Phinney,
   W. C.; Duke, M. B.; Muehlberger, W. R.; Hubbard, N. J.; Butler, P.;
   Laughon, R. B.; Annexstad, J. O.; Heiken, G. H.; Agrell, S.; Brett,
   P. R.; Clanton, U. S.; Carrier, W. D.; Fruland, R.; Fryxell, R.;
   Gooley, R.; Horz, F.; Jackson, E. D.; Lofgren, G. E.; Marvin, U. B.;
   McKay, D. S.; Meyer, C.; Morrison, D. A.; Nagle, S.; Reid, A. M.;
   Ridley, W. I.; Simonds, C. H.; Stuart-Alexander, D.; Warner, J. L.;
   Williams, R. J.; Wilshire, H. G.; Bansal, B.; Bennett, L.; Clark,
   R. S.; Eldridge, J. S.; Felix, W. D.; Gibson, E. K.; Keith, J. E.;
   Lewis, C. F.; Moore, C. B.; Moore, G. W.; Northcutt, K. J.; O'Kelley,
   G. D.; Perkins, R. W.; Portenier, W. R.; Rancitelli, L. A.; Reynolds,
   M. A.; Rhodes, J. M.; Robbins, M. K.; Rogers, K. V.; Schonfeld, E.;
   Simms, L. A.; Wainwright, J.; Wogman, N. A.
1973Sci...182..659A    Altcode: 1973Sci...182..659G
  No abstract at ADS

---------------------------------------------------------
Title: Apollo 15 green glasses
Authors: Ridley, W. I.; Reid, A. M.; Warner, J. L.; Brown, R. W.
1973PEPI....7..133R    Altcode:
  Apollo 15 breccia 15427 and soils 15101, 15261 and 15301 contain
  abundant spheres and fragments of a green glass that is remarkably
  constant in composition. The glass is rich in Fe and Mg, and low in
  Ti, unlike any known lunar basalt, and may be derived from material
  of pyroxenitic composition in the Apennine Front.

---------------------------------------------------------
Title: Major Element Composition of Glasses in two Apollo 16 Soils
    and a Comparison with Luna 20 Glasses
Authors: Ridley, W. I.; Reid, A. M.; Warner, J.; Brown, R. W.; Gooley,
   R.; Donaldson, C.
1973LPI.....4..625R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Inverted Pigeonites from a Clast of Rock 15459
Authors: Takeda, H.; Ridley, W. I.; Reid, A. M.; Brett, R.
1973LPI.....4..701T    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Zirconolite (versus zirkelite) in Lunar Rocks
Authors: Wark, D. A.; Reid, A. F.; Lovering, J. F.; El Goresy, A.
1973LPI.....4..764W    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Coexisting bronzite and clinobronzite in the Steinbach
    meteorite.
Authors: Reid, A. M.; Williams, R. J.; Takeda, H.
1973Metic...8R..66R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Apollo 16 Lunar Samples: Petrographic and Chemical
    Description
Authors: Apollo 16 Preliminary Examination Team; Gast, P. W.;
   Phinney, W. C.; Duke, M. B.; Jackson, E. K.; Hubbard, N. J.; Butler,
   P.; Laughon, R. B.; Agrell, S. O.; Bass, M. N.; Brett, R.; Carrier,
   W. D.; Clanton, U. S.; Eaton, A. L.; Head, J.; Heiken, G. H.; Horz,
   F.; Lofgren, G. E.; McKay, D. S.; Morrison, D. A.; Muehlberger,
   W. R.; Nagle, J. S.; Reid, A. M.; Ridley, W. I.; Simonds, C.;
   Stuart-Alexander, D.; Warner, J. L.; Williams, R. J.; Wilshire, H.;
   Bansal, B. M.; Brannon, J. A.; Landry, A. M.; Rhodes, J. M.; Rodgers,
   K. V.; Wainwright, J. E.; Bennett, L.; Clark, R. S.; Keith, J. E.;
   O'Kelley, G. D.; Perkins, R. W.; Rancitelli, L. A.; Portenier, W. R.;
   Robbins, M. K.; Schonfeld, E.; Gibson, E. K.; Lewis, C. F.; Moore,
   C. B.; Moore, D. R.
1973Sci...179...23A    Altcode: 1973Sci...179...23G
  No abstract at ADS

---------------------------------------------------------
Title: Glass compositions in Apollo 16 soils 60501 and 61221
Authors: Ridley, W. I.; Reid, A. M.; Warner, J. L.; Brown, R. W.;
   Gooley, R.; Donaldson, C.
1973LPSC....4..309R    Altcode: 1973GeCAS...4..309R
  No abstract at ADS

---------------------------------------------------------
Title: Major Element Composition of Glasses in Three Apollo 15 Soils
Authors: Reid, A. M.; Warner, J.; Ridley, W. I.; Brown, R. W.
1972Metic...7..395R    Altcode:
  Approximately 180 glasses in each of three Apollo 15 soils have
  been analyzed for nine elements. Cluster analysis techniques allow
  the recognition of preferred glass compositions that are equated with
  parent rock compositions. Green glass rich in Fe and Mg, poor in Al
  and Ti may be derived from deep seated pyroxenitic material now present
  at the A penn ine Front. Fra Mauro basalt (KREFP) is most abundant in
  the LM soil and is tentatively identified as ray material from the
  A ristillus-A u to lycu s area. High land basalt (anortho sitic gab
  bro), believed to be derived from the lunar highlands, has the same
  composition as at other landing sites, but is less abundant. The A
  penn ine Front is probably not true highland material but may contain a
  substantial amount of material with the composition of Fra Mauro basalt,
  but lacking the high-K content. Glasses with mare basalt compositions
  are present in the soils and four subgroups are recognized, one of which
  is compositionally equivalent to the large Apollo 15 basalt samples.

---------------------------------------------------------
Title: Petrology of Mare Fecunditatis
Authors: Jakes, P.; Ridley, W. I.; Reid, A. M.; Warner, J.; Harmon,
   R. S.; Brett, R.; Brown, R. W.
1972LPI.....3..430J    Altcode:
  No abstract at ADS

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Title: The Apollo 15 lunar samples: A preliminary description.
Authors: Gast, P. W.; Phinney, W. C.; Duke, M. B.; Silver, L. T.;
   Hubbard, N. J.; Heiken, G. H.; Butler, P.; McKay, D. S.; Warner,
   J. L.; Morrison, D. A.; Horz, F.; Head, J.; Lofgren, G. E.; Ridley,
   W. I.; Reid, A. M.; Wilshire, H.; Lindsay, J. F.; Carrier, W. D.;
   Jakes, P.; Bass, M. N.; Brett, P. R.; Jackson, E. D.; Rhodes, J. M.;
   Bansal, B. M.; Wainwright, J. E.; Parker, K. A.; Rodgers, K. V.;
   Keith, J. E.; Clark, R. S.; Schonfeld, E.; Bennett, L.; Robbins, M.;
   Portenier, W.; Bogard, D. D.; Hart, W. R.; Hirsch, W. C.; Wilkin,
   R. B.; Gibson, E. K.; Moore, C. B.; Lewis, C. F.
1972Sci...175..363G    Altcode:
  No abstract at ADS

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Title: Chemistry of Highland and Mare Basalts as Inferred from
    Glasses in the Lunar Soils
Authors: Reid, A. M.; Ridley, W. I.; Warner, J.; Harmon, R. S.; Brett,
   R.; Jakes, P.; Brown, R. W.
1972LPI.....3..640R    Altcode:
  No abstract at ADS

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Title: Apollo 15 glasses and the distribution of non-mare crustal
    rock types.
Authors: Warner, J.; Ridley, W. I.; Reid, A. M.; Brown, R. W.
1972afls.conf..179W    Altcode:
  No abstract at ADS

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Title: Microprobe analyses of glasses in lunar soils.
Authors: Brown, R. W.; Ridley, W. I.; Warner, J. L.; Reid, A. M.
1972magl.book.....B    Altcode:
  No abstract at ADS

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Title: Preliminary Examination of Lunar Samples from Apollo 14
Authors: Anderson, D. H.; Bass, M. N.; Bennett, A. D.; Bogard, D. D.;
   Brett, R.; Bromwell, L. G.; Butler, P., Jr.; Carrier, W. D., III;
   Clark, R. S.; Cobleigh, T.; Duke, M. B.; Gast, P. W.; Gibson, E. K.,
   Jr.; Hart, W. R.; Heiken, G. H.; Hirsch, W. C.; Hörz, F.; Jackson,
   E. D.; Johnson, P. H.; Keith, J. E.; Lewis, C. F.; Lindsay, J. F.;
   Martin, J. R.; Melson, W. C.; Mitchell, E. D.; Moore, C. B.; Morrison,
   D. A.; Nance, W. B.; Phinney, W. C.; Reid, A. M.; Reynolds, M. A.;
   Richardson, K. A.; Ridley, W. I.; Schonfeld, E.; Shepard, A. B.;
   Sutton, R. L.; Trask, N. J.; Warner, J.; Wilkin, R. B.; Wilshire,
   H. G.; Wones, D. R.; Lunar Sample Preliminary Examination Team (1)
1971Sci...173..681A    Altcode:
  No abstract at ADS

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Title: Apollo 12 Igneous Rocks 12004, 12008, 12009, and 12022:
    Metal Grains and their Relation to the Crystallization History
Authors: Brett, R.; Butler, P., Jr.; Meyer, C., Jr.; Reid, A. M.;
   Takeda, H.; Williams, R. J.
1971LPI.....2..212B    Altcode:
  No abstract at ADS

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Title: Apollo 12 igneous rocks 12004, 12008, 12009, and 12022:
    A mineralogical and petrological study
Authors: Brett, R.; Butler, P., Jr.; Meyer, C., Jr.; Reid, A. M.;
   Takeda, H.; Williams, R.
1971LPSC....2..301B    Altcode:
  No abstract at ADS

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Title: Tranquillityite: A new silicate mineral from Apollo 11 and
    Apollo 12 basaltic rocks
Authors: Lovering, J. F.; Wark, D. A.; Reid, A. F.; Ware, N. G.; Keil,
   K.; Prinz, M.; Bunch, T. E.; El Goresy, A.; Ramdohr, P.; Brown, G. M.;
   Peckett, A.; Phillips, R.; Cameron, E. N.; Douglas, J. A. V.; Plant,
   A. G.
1971LPSC....2...39L    Altcode:
  No abstract at ADS

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Title: Electron Microprobe, Fission Track and Activation Analysis
    of Lunar Samples.
Authors: Frick, C.; Hughes, T. C.; Lovering, J. F.; Reid, A. F.;
   Ware, N. G.; Wark, D. A.
1971LPI.....2..205F    Altcode:
  No abstract at ADS

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Title: Apollo 11 samples: Major mineral chemistry
Authors: Reid, A. M.; Frazer, J. Z.; Fujita, H.; Everson, J. E.
1970GeCAS...1..749R    Altcode: 1970LPSC....1..749R
  No abstract at ADS

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Title: A refractory glass chondrule in the Vigarano chondrite.
Authors: Reid, A. M.; Williams, R. J.; Gibson, E. K., Jr.; Fredriksson,
   K.
1970Metic...5R.218R    Altcode:
  No abstract at ADS

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Title: Phase Chemistry, Structure, and Radiation Effects in Lunar
Samples:
Authors: Arrhenius, G.; Asunmaa, S.; Drever, J. I.; Everson, J.;
   Fitzgerald, R. W.; Frazer, J. Z.; Fujita, H.; Hanor, J. S.; Lal, D.;
   Liang, S. S.; MacDougall, D.; Reid, A. M.; Sinkankas, J.; Wilkening, L.
1970Sci...167..659A    Altcode:
  Phase chemistry, structure, and radiation effects were studied in rock,
  breccia, and soil samples. The regolith apparently developed in the
  final stages of accretion and was modified by later impact processes
  and radiation weathering. Exposure ages indicate transfer of buried
  igneous rock fragments to the near surface late in lunar history. With
  a few exceptions igneous rock fragments, soil, and breccia share the
  same distinctive chemistry, probably acquired before accretion of the
  moon. The igneous rocks texturally resemble basaltic achondrites, and
  the soil and breccias contain glassy spheres analogous to chondrules.

---------------------------------------------------------
Title: Crystal chemistry of high pressure polymorphs of ABO
    <SUB>3</SUB>, AB <SUB>2</SUB>O <SUB>4</SUB> and AB <SUB>4</SUB>O
    <SUB>8</SUB> compounds, and their possible identifications with the
    phases occurring in the mantle
Authors: Reid, A. F.
1970PEPI....3..204R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Newly observed high pressure transformations in Mn
    <SUB>3</SUB>O <SUB>4</SUB>, CaAl <SUB>2</SUB>O <SUB>4</SUB>, and
    ZrSiO <SUB>4</SUB>
Authors: Reid, A. F.; Ringwood, A. E.
1969E&PSL...6..205R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Composition of "irradiated" pyroxenes and feldspars in the
    Kapoeta Howardite.
Authors: Wilkening, L.; Lal, D.; Reid, A. M.
1969Metic...4Q.298W    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: High pressure transformations of spinels (I)
Authors: Ringwood, A. E.; Reid, A. F.
1968E&PSL...5..245R    Altcode: 1969E&PSL...5..245R
  The effects of high pressures (up to 200 kb) and high temperatures
  (∼1000°C) upon 36 spinels have been investigated in an attempt to
  define the principal patterns of spinel transformations. Fifteen
  new transformations were found. Among A <SUP>2+</SUP>B
  <SUP>3+</SUP><SUB>2</SUB>O <SUB>4</SUB> spinels, the most common
  transformation mode is complete disproportionation into oxide
  mixtures, AO + B <SUB>2</SUB>O <SUB>3</SUB>. In contrast, among A
  <SUP>2+</SUP><SUB>2</SUB>B <SUP>4+</SUP>O <SUB>4</SUB> spinels,
  the most common transformations are either to denser single A
  <SUP>2+</SUP><SUB>2</SUB>B <SUP>4+</SUP>O <SUB>4</SUB> phases
  or to mixtures of A <SUP>2+</SUP>O (rocksalt) + A <SUP>2+</SUP>B
  <SUP>4+</SUP>O <SUB>3</SUB> (ilmenite) type phases. Two cases of
  complete disproportionation into AO + BO <SUB>2</SUB> (rutile)
  were observed. The bearing of these observations upon the probable
  transformation mode of Mg <SUB>2</SUB>SiO <SUB>4</SUB> (spinel-like
  phase) in the Earth's mantle is discussed.

---------------------------------------------------------
Title: High pressure polymorphs of olivines: The K <SUB>2</SUB>NiF
    <SUB>4</SUB> type
Authors: Ringwood, A. E.; Reid, A. F.
1968E&PSL...5...67R    Altcode: 1969E&PSL...5...67R
  No abstract at ADS

---------------------------------------------------------
Title: High pressure transformation of alkali aluminosilicates and
    aluminogermanates
Authors: Ringwood, A. E.; Reid, A. F.; Wadsley, A. D.
1967E&PSL...3...38R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Radiocarbon from Cosmic Radiation
Authors: Anderson, E. C.; Libby, W. F.; Weinhouse, S.; Reid, A. F.;
   Kirshenbaum, A. D.; Grosse, A. V.
1947Sci...105..576A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: New Comet Reid (1927b)
Authors: Reid
1927IAUC..135....1R    Altcode:
  Observatory Capetown telegraphs: Comet Reid 8m0 January 26th 19h43m5
  U.T. R.A. = 22 30 40.15 Decl. = -57 49 5 dRA = +44s dDecl. = -4'
  discovered January 25th. As cipher preceding seconds of right ascension
  and north polar distance in the telegram from Cape the cipher 7 is
  used. Thus the position should be apparent (see "Important notice"
  Circular No. 125).