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Author name code: macqueen
ADS astronomy entries on 2022-09-14
author:"MacQueen, Robert" 

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Title: Application of a New Technique for Deriving Prominence Mass
    from SOHO EIT Fe XII (19.5 nm) Absorption Features
Authors: Gilbert, Holly R.; Falco, Lauren E.; Holzer, Thomas E.;
   MacQueen, R. M.
2006ApJ...641..606G    Altcode:
  In a previous study we developed a new technique for deriving prominence
  mass by observing how much coronal radiation in the Fe XII (19.5 nm)
  spectral line is absorbed by prominence material. In the present work
  we apply this new method, which allows us to consider the effects
  of both foreground and background radiation in our calculations,
  to a sample of different types of prominences (eruptive, quiescent,
  and surging) observed during the period 1999 July through 2004
  July. The masses of prominences involved in CMEs are not generally
  measured, but the accurate determination of such masses may help in
  assessing the dynamical importance of prominences in CME events. In
  the present study, we find the average mass of our sample of quiescent
  prominences to be 4.18×10<SUP>14</SUP> g, while the average mass
  of the eruptive prominences is 9.09×10<SUP>14</SUP> g, and that of
  surges is 1.53×10<SUP>14</SUP> g.

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Title: A New Technique for Deriving Prominence Mass from SOHO/EIT
    Fe XII (19.5 Nanometers) Absorption Features
Authors: Gilbert, Holly R.; Holzer, Thomas E.; MacQueen, R. M.
2005ApJ...618..524G    Altcode:
  It is presently unclear what role prominences play in the initiation and
  dynamics of coronal mass ejections (CMEs), although erupting prominences
  are strongly correlated with CMEs. The masses of prominences involved in
  CMEs are not generally measured, but the accurate determination of such
  masses may help in assessing the dynamical importance of prominences in
  CME events. In the technique for deriving prominence mass introduced in
  the present work, we use observations of coronal radiation in the Fe XII
  (19.5 nm) spectral line, which is absorbed by prominence material. This
  new method allows us to consider the effects of both foreground and
  background radiation in our calculations, and it can be applied to
  both quiescent and erupting prominences by using two versions of the
  method, which we label the “spatial-interpolative” version and the
  “temporal-interpolative” version. When both versions can be applied
  to the same event, we find that the temporal-interpolative approach
  yields the more accurate results. We have applied both versions to
  an erupting prominence observed on 1999 July 12 (this prominence has
  an associated CME), and we find that the two approaches result in
  similar mass determinations: (6.0+/-2.5)×10<SUP>14</SUP>g for the
  temporal-interpolative approach and (7.4+/-4.6)×10<SUP>14</SUP>g for
  the spatial-interpolative approach.

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Title: The mass content of Coronal Mass Ejections
Authors: Burkepile, J. T.; Hundhausen, A. J.; MacQueen, R. M.; deToma,
   G.; Darnell, J. A.; Gilbert, H. R.
2004AAS...204.1806B    Altcode: 2004BAAS...36Q.683B
  The total mass content of solar Coronal Mass Ejections (CMEs) can vary
  greatly between events. Most CMEs have estimated masses between 10e+14
  and 10e+16 grams of material. It is believed that most of the CME
  material is coronal in origin (Hildner et al. 1975) but the source of
  the mass remains largely unknown. The large fields-of-view of the LASCO
  C2 and C3 coronagraphs coupled with observations of the low corona from
  the MK4 K-Coronameter at the Mauna Loa Solar Observatory provide the
  observations needed to examine CME masses over a wide range of coronal
  scale heights. We utilize these observations to estimate both the amount
  of material which is ejected from the very low corona and the amount
  of mass which is 'swept up' by the CME as it propagates outward. <P
  />This research is funded by the National Science Foundation.

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Title: Dust Near The Sun
Authors: Mann, Ingrid; Kimura, Hiroshi; Biesecker, Douglas A.;
   Tsurutani, Bruce T.; Grün, Eberhard; McKibben, R. Bruce; Liou,
   Jer-Chyi; MacQueen, Robert M.; Mukai, Tadashi; Guhathakurta, Madhulika;
   Lamy, Philippe
2004SSRv..110..269M    Altcode:
  We review the current knowledge and understanding of dust in the inner
  solar system. The major sources of the dust population in the inner
  solar system are comets and asteroids, but the relative contributions
  of these sources are not quantified. The production processes inward
  from 1 AU are: Poynting-Robertson deceleration of particles outside of
  1 AU, fragmentation into dust due to particle-particle collisions,
  and direct dust production from comets. The loss processes are:
  dust collisional fragmentation, sublimation, radiation pressure
  acceleration, sputtering, and rotational bursting. These loss processes
  as well as dust surface processes release dust compounds in the
  ambient interplanetary medium. Between 1 and 0.1 AU the dust number
  densities and fluxes can be described by inward extrapolation of 1
  AU measurements, assuming radial dependences that describe particles
  in close to circular orbits. Observations have confirmed the general
  accuracy of these assumptions for regions within 30° latitude of the
  ecliptic plane. The dust densities are considerably lower above the
  solar poles but Lorentz forces can lift particles of sizes &lt; 5 μm
  to high latitudes and produce a random distribution of small grains
  that varies with the solar magnetic field. Also long-period comets
  are a source of out-of-ecliptic particles. Under present conditions
  no prominent dust ring exists near the Sun. We discuss the recent
  observations of sungrazing comets. Future in-situ experiments should
  measure the complex dynamics of small dust particles, identify the
  contribution of cometary dust to the inner-solar-system dust cloud, and
  determine dust interactions in the ambient interplanetary medium. The
  combination of in-situ dust measurements with particle and field
  measurements is recommended.

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Title: The Acceleration of Coronal Mass Ejections
Authors: Burkepile, J. T.; Hundhausen, A. J.; MacQueen, R. M.; Detoma,
   G.; Darnell, J. A.; Gilbert, H. R.
2003AGUFMSH21A..01B    Altcode:
  To determine quantitative estimates of the net force acting on a
  CME requires knowledge of the CME acceleration as a function of
  distance from the solar surface. The CME acceleration is determined
  directly from the observed time-height trajectory of the event by two
  methods: (a) sucessive differentials and (b) the use of polynomial
  and exponential function curve fitting to the trajectory, followed by
  successive derivatives. We examine the acceleration of a set of Coronal
  Mass Ejections (CMEs) observed over a wide range of coronal scale
  heights by combining observations of the low corona from the Mauna
  Loa Solar Observatory and the Extreme ultraviolet Imaging Telescope
  (EIT) on the Solar and Heliospheric Observatory (SOHO) spacecraft with
  observations from the LASCO coronagraphs onboard SOHO. We apply both of
  the above techniques to the events and conclude that CME acceleration
  is greatest in the low corona despite the strong force of gravity
  in that region. (In addition, CME start times determined from outer
  coronal (LASCO) observations alone tend to be systematically later
  than the actual start times, most likely due to the fact that LASCO
  observations cannot observe CME acceleration in the low corona.)

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Title: The J- and K-Band Brightness of the Solar F Corona Observed
    during the Solar Eclipse on 1998 February 26
Authors: Ohgaito, R.; Mann, I.; Kuhn, J. R.; MacQueen, R. M.;
   Kimura, H.
2002ApJ...578..610O    Altcode:
  We analyze J- and K-band observations of the 1998 solar eclipse
  and derive the F-corona brightness in the K band between 3 and
  7 R<SUB>solar</SUB> from the center of the Sun and in the J band
  out to 5 R<SUB>solar</SUB>. The falloff in the K-band brightness
  from 3 to 7 R<SUB>solar</SUB> is fitted with a radial power law
  with exponent -2.4+/-0.1 at the solar equator and with exponent
  -2.9<SUP>+0.2</SUP><SUB>-0.1</SUB> at the solar pole. This slope is
  gentler than that derived from observations in 1983 but is steeper
  than that derived from observations for the 1991 eclipse. The radial
  profiles agree well with models that explain the F corona with weakly
  absorbing dust particles. Comparison of the J- and K-band brightness at
  3 R<SUB>solar</SUB> from the center of the Sun indicates a reddening
  of the F corona with respect to the solar spectrum. The reddening is,
  however, less pronounced compared to the F corona observed during the
  1983 total solar eclipse. This fact may be attributed to a change in
  the composition of dust near the Sun. As with the radial profiles, the
  reddening in 1998 is better explained with models that assume weakly
  absorbing rather than strongly absorbing dust particles in the solar
  corona. Similar to recent eclipse observations, we do not detect an
  excess emission feature of near-solar dust in the F corona. We hence
  can reject the hypothesis that suggests a correlation between the
  detection of an emission feature and the solar activity cycle.

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Title: Narrow Coronal Mass Ejections
Authors: Gilbert, Holly R.; Serex, Elizabeth C.; Holzer, Thomas E.;
   MacQueen, R. M.; McIntosh, Patrick S.
2001ApJ...550.1093G    Altcode:
  Narrow coronal mass ejections (CMEs), defined arbitrarily as events
  whose apparent angular width is 15° or less, are a small subset of
  all CMEs. Little is known of the properties of these events and whether
  these properties differ from those of the larger, more typical CMEs. We
  have included in this study 15 narrow CMEs observed in the period from
  1999 March through December, and we have examined their structure,
  angular size, projected radial velocity (speed), and likely surface
  associations. We find it useful to break these events into two classes:
  structured and unstructured. Unstructured narrow events are generally
  narrower and slower than the structured events, but both classes of
  narrow CMEs exhibit speeds similar to those of larger CMEs. We found
  that 11 of 15 events studied may be traced to regions on the solar
  surface near a relatively sharp bend in a polarity-reversal line,
  as revealed from Hα synoptic maps. We contrast the properties of the
  narrow CMEs with those of the larger CME population.

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Title: Solar Coronal Brightness Changes and Mass Ejections during
    Solar Cycle 22
Authors: MacQueen, R. M.; Burkepile, J. T.; Holzer, T. E.; Stanger,
   A. L.; Spence, K. E.
2001ApJ...549.1175M    Altcode:
  Observations of the brightness of the outer solar corona from the
  Solar Maximum Mission (SMM) coronagraph during solar cycle 22 (1980,
  then 1984-1989) are compared with the occurrence rate and the mass of
  coronal mass ejections (CMEs) observed during this period. We find that
  the brightness and, hence, mass of the outer corona increased by more
  than a factor of 4 from solar minimum (1986) to late 1989, when the
  SMM ceased operation. The peak brightness (mass) in 1989 was roughly
  equivalent to that observed in the latter part of 1980. Accompanying a
  sharp increase in brightness (mass) of the corona in early 1989 was a
  concomitant increase in both the occurrence rate and the average mass
  of CMEs.

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Title: A New Method of Determining Line-of-Sight Velocity Using
    MLSO/CHIP He I 1083 nm Observations
Authors: Holzer, T. E.; Gilbert, H. R.; Elmore, D. F.; MacQueen, R. M.
2000SPD....3102107H    Altcode:
  A new method for determining line-of-sight velocity has been developed
  for the MLSO/CHIP He I 1083 nm instrument. The method involves tuning
  the Lyot-type spectral filter to seven different positions during
  each observing sequence (lasting about 3 minutes). The algorithm for
  line-of-sight velocity determination using these seven filter positions
  yields an accuracy of better than 10 km/s over a line-of-sight velocity
  range from -100 km/s to +100 km/s. The method is applicable to the
  observation of filaments, surges, sprays, and other features exhibiting
  sufficiently strong absorption or emission in the 1083 nm line. It
  therefore will be particularly useful in the study of eruptive events
  seen against the solar disk, such as filament eruptions associated with
  earthward-directed coronal mass ejections. The High Altitude Observatory
  (HAO) is part of the National Center for Atmospheric Research (NCAR),
  which is sponsored by the National Science Foundation under the
  management of the University Corporation for Atmospheric Research.

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Title: Prominence Densities as Derived from SOHO/EIT Fe XII (195
    Angstrom) Absorption Features
Authors: Gilbert, H.; Mize, L.; Holzer, T.; MacQueen, R.
2000SPD....31.0218G    Altcode: 2000BAAS...32..814G
  Prominences often appear in absorption when the sun is viewed in EUV
  emission lines formed at coronal temperatures. The coronal EUV radiation
  at wavelengths less than 504 anstroms undergoes Lyman continuum
  absorption by both hydrogen and helium (i.e., the coronal radiation
  ionizes hydrogen and helium atoms from their ground states). We can
  thus infer prominence column densities by measuring the amount of
  coronal radiation absorbed by prominence material along the line of
  sight, and by making assumptions concerning the ionization state and
  the helium abundance characterizing the prominence plasma. We do so
  by measuring 195 angstrom intensity along lines of sight inside and
  outside prominences, both just on the disk and just off the limb. Our
  absorption measurements are made using Fe XII (195 angstroms) data
  from the Extreme Ultraviolet Imaging Telescope (EIT) on board the
  SOHO spacecraft. Initial results using our technique yield prominence
  densities on the order of 10<SUP>10</SUP> cm<SUP>-3</SUP>. This is
  the first step in reaching our ultimate objective of attaining a
  quantitative measure of total prominence mass, which may be important
  in the dynamical processes involved in Coronal Mass Ejection initiation
  and evolution.

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Title: Temporal properties of He I 1083 nm dark points
Authors: MacQueen, R. M.; Hendrickson, M. A.; Woods, J. C.; Lecinski,
   A. R.; Elmore, D. F.; White, O. R.
2000SoPh..191...85M    Altcode:
  The intensity of a sample of large, high-contrast and isolated dark
  points has been observed with full-disk images in the light of He i
  1083 nm from the Chromospheric Helium line Intensity Photometer (CHIP)
  on Mauna Loa, Hawaii. Temporal variations in the intensity encompassing
  a broad range of time scales have been recorded. Long-term changes
  in the intensity, although highly variable, are characterized by
  e-folding times on the order of 5 h. Superposed on these variations
  are frequent intensity variations, which occur over time scales
  ranging from the typical observing cadence of 3 min, to tens of
  minutes. Microflares-involving intensity changes of at least 50%
  over periods of minutes are observed frequently. Rapid cadence (
  min) observations reveal differences between rise and decay times and
  shorter-term variations in the intensity profiles of these microflares.

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Title: The J- and K-Band brightness of the solar F-corona observed
    during the solar eclipse on February 26, 1998.
Authors: Ohgaito, R.; Mann, I.; Kuhn, J. R.; MacQueen, R. M.; Lin,
   H.; Edmunds, D.
1999BAAS...31.1159O    Altcode:
  No abstract at ADS

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Title: The J- and K-Band Brightness of the Solar F-Corona Observed
    During the Solar Eclipse on February 26, 1998
Authors: Ohgaito, R.; Mann, I.; Kuhn, J. R.; MacQueen, R. M.; Lin,
   H.; Edmunds, D.
1999DPS....31.5502O    Altcode:
  The solar eclipse on February 26 1998 was observed from an open flying
  aircraft at an altitude of almost 6 km above the Pacific about 800
  km southwest from Panama City. The solar F-corona, produced by light
  scattering and thermal emission from dust around the Sun, was observed
  with a low atmospheric straylight level in the J and K-band over a field
  of view of 7 degrees. The data show no indication for the existence of
  pronounced brightness features in the solar F-corona, such as often
  discussed as evidence for the existence of dust rings. The shape
  of the corona is slightly elliptic but symmetric in the north-south
  direction. The data show a reddening of the coronal brightness compared
  to the solar spectrum. The color of the F-corona is influenced by the
  temperature of dust particles, by their spatial distribution, as well
  as by their size distribution that influences especially the forward
  scattering that is seen in the corona from dust particles close to the
  observer. We will discuss the color variation from the solar equator
  to the solar pole and with distances from the Sun and compare it to
  models of dust light scattering and thermal emission.

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Title: Probable Detection of a Bright Infrared Coronal Emission Line
    of Si IX near 3.93 Microns
Authors: Kuhn, J. R.; MacQueen, R. M.; Streete, J.; Tansey, G.; Mann,
   I.; Hillebrand, P.; Coulter, R.; Lin, H.; Edmunds, D.; Judge, P.
1999ApJ...521..478K    Altcode:
  We report here the probable detection of an emission line of Si
  IX that was observed from an open C130 aircraft over the Pacific
  Ocean during the 1998 total solar eclipse. Although the IR data
  themselves are inconclusive because of the uncertainty in the precise
  central wavelengths of the narrowband filters during the eclipse,
  the consistency of the measured IR limb excess with simultaneous EUV
  emission measured by SOHO/Coronal Diagnostic Spectrometer and the EUV
  Imager Telescope support our detection claim. This line appears to
  be the brightest IR coronal line yet observed, and its existence may
  significantly improve future prospects for obtaining optical coronal
  magnetic field measurements.

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Title: Initial CHIP He I Observations of Solar Limb Activity
Authors: MacQueen, R. M.; Blankner, J. G.; Elmore, D. F.; Lecinski,
   A. R.; White, O. R.
1998SoPh..182...97M    Altcode:
  A new instrument capable of 3-min time resolution full-disk and limb
  observations in the Hei 1083 nm spectral line has been in operation
  at the High Altitude Observatory's Mauna Loa Solar Observatory (MLSO)
  since April 1996. We discuss instrument capabilities and performance
  and present some initial observations of limb activity from the first
  year of instrument operation. We compare limb Hei and Hα observations
  of quiescent and active prominences, comment on the role of Doppler
  shifts in interpreting the Hei observations, and illustrate the use
  of disk/limb Hei observations of a CME-associated eruptive filament
  in mass-ejection studies.

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Title: Chromospheric Helium Imaging Photometer (an Instrument for
    High Time Cadence 1083-nm Wavelength Solar Observations)
Authors: Elmore, David F.; Card, Gregory L.; Chambellan, Clarke W.;
   Hassler, Donald M.; Hull, Howard L.; Lecinski, Alice R.; MacQueen,
   Robert M.; Streander, Kim V.; Streete, John L.; White, Oran R.
1998ApOpt..37.4270E    Altcode:
  No abstract at ADS

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Title: A Study of the Origin and Dynamics of Coronal Mass Ejections
Authors: Burkepile, J. T.; Hundhausen, A. J.; Bagenal, F.; McAllister,
   A. H.; MacQueen, R. M.
1997SPD....28.0125B    Altcode: 1997BAAS...29..883B
  Coronal mass ejections (CMEs) are dynamic events that typically
  involve the expulsion of 10(15) to 10(16) grams of coronal and
  chromospheric plasma into interplanetary space. The relationship
  between mass ejections and other forms of solar activity, especially
  those evident on the solar disk, remains unclear. In an attempt to
  accurately determine CME onset times and origins, we have combined
  observations from the Solar Heliospheric Observatory (SOHO) Large
  Angle Spectroscopic Coronagraphs (LASCO), the SOHO Extreme Ultraviolet
  Imaging, the Mauna Loa Observatory (MLO) white light and chromospheric
  instruments and the Yohkoh Soft X-ray Telescope. Mass ejections believed
  to have occurred both at or near the limb of the sun and on the solar
  disk have been employed in the comparison. When available, the MLO and
  LASCO white light observations have been combined to determine material
  trajectories, and hence accurate CME onset times. The evolution of
  the magnetic fields and associated plasma structures prior to, during
  and after mass ejections have been examined by comparing He-I and Hα
  chromospheric disk signatures with EUV and X-ray observations.

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Title: Solar Chromospheric and Coronal Explorer
Authors: Walker, Arthur B.; Scherrer, Philip H.; Hoover, Richard B.;
   Tandberg-Hanssen, Einar; Barbee, Troy W.; Ling, James C.; MacQueen,
   R. M.; Timothy, J. Gethyn; Adamson, Paul; Mennzel, Mike T.; Petheram,
   John C.; Shattuck, Paul L.
1996SPIE.2804..286W    Altcode:
  The presence of the solar magnetic field has a profound effect on
  the structure of the lower chromosphere, and is responsible for the
  formation of the upper chromosphere and the corona, and the acceleration
  of the solar wind. The variation of the field induces variations in
  the chromosphere and the corona on time scales from 0.001 seconds to
  centries. SOHO, and subsequent approved solar missions such as TRACE
  will bring powerful observational capabilities to bear on critical
  questions relating to solar variability. However, the most fundamental
  question--how energy is transferred from the magnetic field into the
  solar plasma--will require observations of diagnostic quality on a
  spatial scale of 50 - 100 kilometers; this is an order of magnitude
  beyond the capability of any planned mission. Our mission concept,
  the Solar Chromospheric and Coronal Explorer (SCCE) is designed to
  investigate the mechanisms underlying the variability of the solar
  atmosphere, by attaining spectroscopic observations of the solar
  atmosphere over a wide range of temperatures (4,500 K to 100,000,000 K),
  with very high angular (0.1 arcseconds) and temporal (0.001 seconds)
  resolution, that will permit models of the physical processes that
  underlie the phenomena of solar activity to be formulated and tested
  at the scale, 50 - 75 kilometers that appears to be fundamental. The
  architecture of the SCCE is based on advances in multilayer optics,
  which permit broad spectral response, and high angular and spectral
  resolution to be achieved in a volume, and at a cost that is compatible
  with deployment within the fiscal and physical constraints of the
  MIDEX program.

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Title: BOOK REVIEW: Total Eclipses of the Sun (Expanded
    Edition). J. B. Zirker.
Authors: MacQueen, R. M.
1996Icar..123..585M    Altcode:
  No abstract at ADS

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Title: The Large-Scale Density Structure of the Solar Corona and
    the Heliospheric Current Sheet
Authors: Guhathakurta, Madhulika; Holzer, Thomas E.; MacQueen, R. M.
1996ApJ...458..817G    Altcode:
  We have investigated the three-dimensional distribution of the
  polarization-brightness product (PB) and then quantitatively
  determined the electron density distribution relative to the
  inferred heliographic current sheet during the declining phase
  of solar cycle 20 (1973-1976). The current sheet is taken as the
  center of the bright, dense structures from combined synoptic
  pB data from ground-based K-coronameter and the white- light
  coronagraph aboard Skylab. Analyses of pB scans as a function of
  minimum distance from the current sheet (θ<SUB>min</SUB>) over the
  radial distance range 1.13 to 5.0 R<SUB>sun</SUB> (from Sun center)
  led to the following new results: (1) a quantitative description
  of pB obtained around the inferred neutral line is given by the
  following equation: <P />pB(p,θ<SUB>min</SUB>) = pB<SUB>p</SUB>(p)
  + [pB<SUB>cs</SUB>(p)-pB<SUB>p</SUB>(p)]e-θmin2/w2(r), <P
  />where p is the shortest distance to the line of sight from
  the Sun center, pB<SUB>cs</SUB>(p) and pB<SUB>p</SUB>(P) are the
  observed polarized brightness at the current sheet and the poles,
  respectively, and w(r) is the half-width of the distribution;
  (2) the electron density obtained by inverting the pB data
  is given by <P />N(r,θ<SUB>mg</SUB>) = N<SUB>p</SUB>(r) +
  [N<SUB>p</SUB>(r)-N<SUB>p</SUB>(r)]e<SUP>-θmg2/w2(r)</SUP>d ,
  <P />where N(r,θ<SUB>mg</SUB>) is the number of free electrons
  per cm<SUP>3</SUP>, N<SUB>cs</SUB>(r) and N<SUB>p</SUB>(r) are the
  electron densities at the current sheet and the poles, respectively,
  and θ<SUB>mg</SUB> is the magnetic latitude. Here θ<SUB>mg</SUB> is
  given by <P />θ<SUB>mg</SUB> = [-cos θ sin α sin (φ-φ<SUB>0</SUB>)
  + sin θ cos α] <P />where θ and φ are heliographic latitude and
  longitude, α is the tilt angle of the dipole axis with the rotation
  axis, and φ<SUB>0</SUB> is the intersection of the heliomagnetic and
  heliographic equators; (3) during the period studied (the last third
  of the solar cycle), the mean pB at the current sheet and above the
  polar holes is approximately independent of the phase of the solar
  cycle; and (4) the organization of pB data about the neutral line
  allows inference of the boundary of the polar coronal holes. <P />The
  usefulness of one-dimensional white-light density constraint in solar
  wind modeling has already been demonstrated by Habbal et al. The
  present three-dimensional model should prove very useful in better
  understanding of the global hydromagnetic structure of the corona
  and the solar wind, relating as it does to the magnetic structure
  of the corona, as opposed to heliocentric coordinates. For example,
  the density model could provide constraints on coronal temperature,
  flow velocity, and magnetic structure subject to a suitable analysis
  of geometric effects, which in turn would provide constraints on energy
  balance in the coronal expansion.

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Title: The Role of Particle Size in Producing the F-Coronal Scattered
    Brightness
Authors: MacQueen, R. M.; Davidson, W. C.; Mann, I.
1996ASPC..104..349M    Altcode: 1996IAUCo.150..349M; 1996pcdi.conf..349M
  No abstract at ADS

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Title: Observation and analysis of the F-corona brightness
Authors: Mann, I.; MacQueen, R. M.
1996AdSpR..17c..53M    Altcode: 1996AdSpR..17...53M
  In the context of dust measurements on a solar probe, we present an
  analysis of a 1991 eclipse observation by Hodapp et al. /1/ with respect
  to the solar F-corona brightness (published in MacQueen and Greeley,
  /2/). Although the data are limited by observing conditions, we can
  still gain some information which may be compared with our present
  knowledge about the interplanetary dust cloud based on the analysis of
  zodiacal light data, which describe the dust in regions outward from
  the sun. Past visible light measurements showed that the F-corona
  has roughly the same brightness in the ecliptic and over the poles,
  but that the radial gradient of the latter is steeper. In the 1991
  infrared observations, the ecliptic radial gradient is flatter than
  has been observed in the visible, whereas the polar radial gradient
  is rather similar to past, visible spectral region observations. This
  appears to point to the existence of different components in the dust
  cloud as also discussed to explain the zodiacal light /3/. Also in the
  present data there is no clear signature for the beginning of the dust
  free zone around the sun, one conclusion being that dust (of some type)
  possibly approaches the sun to within 4 solar radii. As far as the size
  distribution of dust in the solar vicinity is concerned we discuss a
  study by Davidson et al. /4/, which shows that the present F-corona
  data can be fitted with distinctly different size distributions.

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Title: ACOS: HAO's next generation Coronal Observing Facility at
    Mauna Loa
Authors: Hassler, D. M.; Elmore, D. F.; Lecinski, A.; Streander,
   K.; Burkepile, J.; Stanger, A.; Hundhausen, A. J.; Rottman, G. J.;
   MacQueen, R. M.
1995SPD....26..721H    Altcode: 1995BAAS...27..970H
  No abstract at ADS

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Title: Solar Coronal Dust Scattering in the Infrared
Authors: MacQueen, R. M.; Greeley, Bradford W.
1995ApJ...440..361M    Altcode:
  Observations of the total and polarized brightness of the solar corona
  at wavelength 2.12 microns during the total solar eclipse of 1991 July
  11 are employed to separate the contribution of the electron-scattered
  component and the remaining, nonpolarized component, the latter
  dominating in the outer corona. After corrections are applied to account
  for a two-component sky or instrument background, the brightness
  of the ecliptic and polar corona are fitted by r<SUP>-1.9</SUP> and
  r<SUP>-2.3</SUP>, respectively, over the radial distance range 3-8
  solar radii from Sun center. The ecliptic outer-coronal brightness is
  compared with a Mie-scattering model of interplanetary dust particles
  based upon three particle-size distributions deduced from, respectively,
  lunar microcrater counts (Lamy &amp; Perrin 1986), interplanetary
  dust flux measurements (Gruen et al. 1985), and for an arbitrary
  population of large particles (radii greater than 3 x 10<SUP>-5</SUP>
  cm). Particle physical characteristics and spatial distributions are
  those assumed in past studies of the zodiacal cloud. For reasonable
  assumed space number densities of particles, the models agree with the
  magnitude of observed ecliptic coronal brightness. But in all cases,
  the models predict a steeper brightness falloff with radial distance
  that that observed, with those models for which the power-law exponent
  for the space distribution is v = 1.3 being the most discrepant with
  the observed radial gradient.

---------------------------------------------------------
Title: Scattering models for the solar infrared F-corona brightness
Authors: Davidson, W. C.; MacQueen, R. M.; Mann, I.
1995P&SS...43.1395D    Altcode:
  Model calculations are made of the infrared brightness in the solar
  F-corona motivated by recent infrared solar eclipse observations. Two
  different approaches are employed to describe the scattering properties
  of interplanetary dust : Mie scattering theory and diffraction theory,
  with and without an isotropic scattering term. In addition. two
  different particle size distributions are used in the calculations and
  the resultant line of sight brightness is compared with observational
  data of the solar F-corona between 3 and 8 solar radii ( R) in the
  ecliptic plane. It is found that the use of diffraction theory without
  an isotropic scattering contribution gives a very poor match with the
  observations, for both assumed particle size distributions. However,
  both the diffraction theory including isotropic scattering and the
  Mie scattering theory agree reasonably with the observed brightness,
  and especially its radial slope within the corona. for the model size
  distribution which is dominated by large particles. Only Mie theory
  may be employed in describing the second model size distribution
  because diffraction theory poorly describes the scattering due to
  the small particles which dominate this size distribution. It is
  concluded that the derivation of particle size distributions from the
  F-coronal brightness is still ambiguous and a further analysis needs
  either improved observations, or the application of further reasonable
  physical assumptions.

---------------------------------------------------------
Title: CFHT eclipse observation of the very fine-scale solar corona
Authors: Koutchmy, S.; Belmahdi, M.; Coulter, R. L.; Demoulin, P.;
   Gaizauskas, V.; MacQueen, R. M.; Monnet, G.; Mouette, J.; Noens,
   J. C.; November, L. J.
1994A&A...281..249K    Altcode:
  At the July 11, 1991 solar total eclipse, a modern large optical
  telescope, Canada-France-Hawaii telescope (CFHT), was used to
  probe the solar corona. The best possible pictures were obtained
  with the CFHT, using fast imaging techniques and post-facto image
  selection and processing. Several cameras were run during totality
  to acquire sub-arcsec spatial resolution white-light images, with
  both narrow-band and broad-band filters. The setup and the observing
  procedure are described. Preliminary results, together with an
  evaluation of the merits of the experiment, are given, as well as a
  sample of images. Fine-scale coronal features were observed for the
  first time in a time series, confirming the importance of plasmoid-like
  activity in the inner corona. The observation of the smallest coronal
  feature ever reported is analyzed, giving a typical cross-section of
  0.4 +/- 0.1 arcsec. On a larger scale, dark loops around a foreground
  prominence are resolved for the first time, suggesting that sheet-like
  voids exist above a filament channel.

---------------------------------------------------------
Title: The solar F-corona at 2.12 pin: calculations of near-solar
    dust in comparison to 1991 eclipse observations
Authors: Mann, L.; MacQueen, R. M.
1993A&A...275..293M    Altcode:
  A comparison of 1991 solar eclipse coronal observations over the range
  of 3R<SUB>sun</SUB>-8R<SUB>sun</SUB> at wavelength 2.12 μm, with model
  calculations of thermal emission and scattering from interplanetary dust
  particles (IDPs) is presented. The observed brightness in the ecliptic
  plane shows a monotonic decrease which can be approximated with a
  radial power law with exponent 2. No signature in the brightness,
  due to enhanced dust concentration or emission near the Sun can be
  detected. The modelling attempts result in an average deviation,
  relative to the observations, of less than 12%, under reasonable
  assumptions about the spatial distribution and optical and thermal
  properties of the IDPs. It is only possible to match the observational
  data with a model of scattering and thermal emission where particles can
  approach up to 3R<SUB>sun</SUB> towards the Sun. The data suggest that
  it is necessary to alter the local variation of number density of dust
  particles within 10R<SUB>sun</SUB>. The deduced temperature of the IDPs
  is about 10% below their blackbody temperature, and the best fit with
  observations involves a variation in the IDP albedo with distance from
  the Sun, suggesting physical changes to the near-solar IDP population.

---------------------------------------------------------
Title: The three-dimensional structure of `loop-like' coronal mass
    ejections
Authors: MacQueen, R. M.
1993SoPh..145..169M    Altcode:
  We have measured the brightness and latitudinal extent of the depleted
  (cavity) region behind the leading edge of three coronal mass ejection
  (CME) events from the Skylab epoch. The events chosen are among those
  believed to be typical of non-impulsive, `loop-like' CMEs (Sime,
  MacQueen, and Hundhausen, 1984). The pre-event coronal brightness has
  been matched by a model corona, assuming both a background contribution
  and a contribution from a range of hypothetical streamer models,
  distinguished by differing longitudinal extent. Then, assuming that
  the cavities are voided regions in which the local electron density
  is negligible, we estimate their minimum line-of-sight extent and find
  them to be comparable to, or greater than, their measured latitudinal
  extent. As a result, we suggest this unambiguously demonstrates
  the three-dimensional nature of these — and likely, this class of
  — events.

---------------------------------------------------------
Title: The Solar Corona from 3 to 8 Solar Radii: Comparison of
    Calculations and New Observational Results
Authors: Mann, I.; MacQueen, R. M.
1992DPS....24.1102M    Altcode: 1992BAAS...24..951M
  No abstract at ADS

---------------------------------------------------------
Title: A search during the 1991 solar eclipse for the infrared
    signature of circumsolar dust
Authors: Hodapp, Klaus-Werner; MacQueen, R. M.; Hall, Donald N. B.
1992Natur.355..707H    Altcode:
  THEORETICAL suggestions<SUP>1-3</SUP> that there should be a ring
  of dust in near-ecliptic orbit about the Sun were supported by
  observations, during a total solar eclipse on 12 November 1966, of
  enhanced infrared emission<SUP>4-6</SUP> from the solar corona at a
  distance of 4 Rsolar from the Sun's centre. The infrared emission was
  attributed to the sublimation of dust grains as they spiral into the
  Sun because of the Poynting-Robertson effect, by which solar radiation
  creates a tangential drag. Two months after the 1966 eclipse, the
  feature at 4 Rsolar was seen again in observations from a stratospheric
  balloon-borne coronagraph, as were additional features at 3.5, 8.7
  and 9.2 R (ref. 6). Observations since then, however, have failed
  unambiguously to corroborate the earlier observations. We searched
  for excess infrared emission in the solar equatorial plane during the
  11 July 1991 eclipse, using a wide-angle infrared camera on Mauna Kea,
  but failed to find any signature of dust evaporation. We argue that the
  earlier observations were credible, and therefore that the circumsolar
  dust ring is a transient feature, perhaps due to the injection of dust
  into near-solar space by a Sun-grazing comet.

---------------------------------------------------------
Title: A Search for the Infrared Signature of Circumsolar Dust
Authors: MacQueen, R. M.; Hodapp, K. -W.; Hall, D. N. B.
1991BAAS...23R1449M    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Sungrazing comets observed by the solar maximum mission
    coronagraph
Authors: MacQueen, R. M.; St. Cyr, O. C.
1991Icar...90...96M    Altcode:
  Ten sungrazing comets were discovered by the High Altitude Observatory's
  white light coronagraph on the NASA Solar Maximum Mission spacecraft
  during an observing period which covered about 6 years. In addition,
  observation of another sungrazing comet discovered by the SOLWIND
  coronagraph was confirmed. The comets exhibited a wide range of
  brightness near the Sun, spanning roughly 8 astronomical magnitudes. No
  comets were observed postperihelion, and no discernible coronal effects
  could be detected as a result of any comet disappearance. The comet
  apparent motions and orientation of tails are consistent with all of the
  comets belonging to the Kreutz sungrazer group, a conclusion in support
  of the orbital analysis of nine of the objects by Marsden (1989). The
  observing programs employed by the instrument to detect coronal
  mass ejection events are shown to be well-suited for the detection
  of sungrazers. The appearance of these comets is seen to be highly
  episodic over the time period of SMM coronagraph operation. Estimates
  of the comet head properties, including size, are offered, based upon
  the observed comet behavior.

---------------------------------------------------------
Title: The Effect of Solar Activity on Sungrazing Comets
Authors: St. Cyr, O. C.; Hundhausen, A. J.; MacQueen, R. M.
1990BAAS...22.1323S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: SMM Observations of Sungrazing Comets
Authors: MacQueen, R. M.; St. Cyr, O. C.; Hundhausen, A. J.
1989BAAS...21.1144M    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The solar coronal mass ejection of 20 21 November, 1973
Authors: MacQueen, R. M.; Holzer, T. E.
1988SoPh..116..349M    Altcode:
  The coronal transient event of 20-21 November is unusual in that its
  appearance is distinctly non-loop-like; rather, the transient resembles
  a confined ray or fan-like volume. Studies of the distribution of the
  coronal material with time indicate that this is a mass ejection event,
  involving about 1 × 10<SUP>15</SUP> g of material from the lower
  corona. Analysis of the polarization signal of the event suggests that
  the event is associated with chromospheric activity in a region near
  longitude E68. The observed properties (distributions in brightness
  and polarization) of the transient are compared with the properties
  of a well-studied event of typical loop-like appearance, but rotated
  to simulate an `edge-on' appearance; the differences suggest that
  the 20-21 November event is not such an edge-on, loop-like transient,
  but rather is most simply described as an axisymmetric-cylindrical or
  conical volume, the boundaries of which remain constant over the events'
  lifetime. On this basis, the variation of the transient spatial density
  with height and the variation of density with time can be specified
  rather more certainly than for previously-studied coronal mass ejection
  events. Densities are found to range from 3 × 10<SUP>−16</SUP>
  g cm<SUP>−3</SUP> at 2.1 R<SUB>⊙</SUB> heliocentric height early
  in the event to 1 × 10<SUP>−18</SUP> g cm<SUP>−3</SUP> at 4.0
  R<SUB>⊙</SUB> late in the event. Typical temporal variations of the
  ejected material (at a given heliocentric height) are found to be on the
  order of 10<SUP>−18</SUP> g cm<SUP>−3</SUP> s<SUP>−1</SUP>. The
  mass and momentum balance in the event have been estimated from the
  observed parameters, employing a multiparameter approach. We find that a
  model with modest mass flux typified by material speed u<SUB>0</SUB> ≲
  50 km s<SUP>−1</SUP> and a near balance between the event's pressure
  gradient force and gravity — with possibly a small hydromagnetic
  wave contribution to the total pressure — is consistent with the
  observations. The kinetic energy of the event, determined from the
  motion of the center of mass of the ejected material, is only about
  10<SUP>26</SUP> ergs, and thus is the smallest for any solar mass
  ejection studied to date.

---------------------------------------------------------
Title: Measurement of the 3-dimensional positions of type III bursts
    in the solar corona.
Authors: Poquerusse, M.; Steinberg, J. L.; Caroubalos, C.; Dulk,
   G. A.; MacQueen, R. M.
1988A&A...192..323P    Altcode:
  The Stereo 5 experiment observed the Sun at 60 and 30 MHz simultaneously
  on the Earth (Nançay), and on the Soviet spacecraft Mars 7. It recorded
  many normal type III's and type IIIb's during the period 1974 Jan
  10 to 19 at a time when the "stereo" angle Earth-Sun-spacecraft was
  large enough (≈35°) to allow an accurate triangulation. The time
  delay Δt of type III bursts between the two observing stations was
  measured with an uncertainty of ≈0.1 s. A ground interferometer
  furnished a 2-dimensional position at 75 MHz with an uncertainty
  of ≈0.1 R_sun;. Combining the two, the authors calculate for the
  first time the three dimensional positions of type III sources in
  the corona. Simultaneous observations of the corona in visible light
  from Skylab allow the apparent radio source positions to be related
  to slowly evolving coronal structures.

---------------------------------------------------------
Title: A New High-Resolution CCD Spectrometer for the Mcdonald
    Observatory 2.7-METER Telescope
Authors: Tull, P. J.; Macqueen, R. G.
1988igbo.conf...52T    Altcode: 1988igbo.conf...52M
  The authors have developed a reflecting analogue of the white-pupil
  spectrograph concept that was proposed by Baranne (1972). The general
  configuration of this spectrograph is given, as well as the reasoning
  behind the decisions that have determined its design.

---------------------------------------------------------
Title: Solar Physics. (Book Reviews: Progress in Solar Physics)
Authors: MacQueen, R. M.
1986Sci...233.1333D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Obituary
Authors: Eddy, J. A.; MacQueen, R. M.
1986SoPh..104..257E    Altcode: 1986SoPh..104..257.
  No abstract at ADS

---------------------------------------------------------
Title: Gordon Allen Newkirk, Jr., 1928 - 1985.
Authors: Eddy, J. A.; MacQueen, R. M.
1986SoPh..104..256E    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The propagation of coronal mass ejection transients
Authors: MacQueen, R. M.; Hundhausen, A. J.; Conover, C. W.
1986JGR....91...31M    Altcode:
  Measurements of the direction of propagation of 29 coronal mass
  ejection events observed during the Skylab epoch (1973-1974) and 19
  events observed during the SMM epoch (1980) reveal that the former
  undergo an average 2.2° equatorward deflection, while the latter do not
  deviate signficantly from radial motion. No differences between eruptive
  prominence-associated or flare-associated events can be detected for
  either epoch. The results suggest that coronal mass ejection events
  are influenced by the background coronal magnetic and flow patterns;
  the nonradial forces affecting the Skylab epoch mass ejections arise
  from the large-scale dipolar magnetic field and flow configuration
  present at that time.

---------------------------------------------------------
Title: Coronal Magnetic Fields - a Mini Survey
Authors: MacQueen, R. M.
1986ASSL..123....5M    Altcode: 1986shtd.symp....5M
  Some recent progress in understanding the nature of the evolution of the
  global coronal magnetic field is reviewed. Particularly, the efforts
  of Hoeksema (1984) in defining the character of the evolving modes
  of the potential coronal field are compared with the currently-known
  evidence for evolution of coronal white light structures. Recent
  work in examining the soft X-ray intensity of coronal holes over a
  major portion of the solar cycle is noted, as are two new studies
  investigating the relation of coronal mass ejections to the ambient
  global coronal magnetic field.

---------------------------------------------------------
Title: Broadening of looplike solar coronal transients
Authors: MacQueen, R. M.; Cole, D. M.
1985ApJ...299..526M    Altcode:
  The broadening of the tops of nine outwardly expanding looplike
  coronal mass-ejection transients observed during 1973-1974 and 1980
  has been examined. Five of the nine transients exhibit increased
  breadth with time (height); although the rates vary widely, no event
  shows an increase which can be fitted by a power-law form with a
  greater-than-linear increase with height. The breadth of four events
  decreases with height. When all nine events are considered together,
  the transient breadth with height is fitted with an expression h
  varies as R exp 0.48 with large scatter. In addition, measurements of
  the total observed loop length of the nine transients show that this
  length L varies as R exp 1.30. Both of these results are contrary
  to the predictions of one model of loop expulsion as a result of an
  assumed azimuthal magnetic field gradient. Finally, when combined with
  the facts that looplike mass ejections are usually associated with
  the occurrence of eruptive prominences, and that such mass ejections
  are generally accelerated through the corona, it is found that the
  observed variation of transient breadth with height contradicts some
  characteristics of self-similar fluid flow which have been ascribed
  to mass-ejection transients.

---------------------------------------------------------
Title: The Broadening of Looplike Solar Coronal Transients
Authors: MacQueen, R. M.; Cole, D.
1985BAAS...17..636M    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Coronal Mass Ejections - Acceleration and Surface Associations
Authors: MacQueen, R. M.
1985SoPh...95..359M    Altcode:
  The fact that eruptive-prominence associated coronal mass ejection
  events may be accelerated over significant heights and times in the
  corona complicates the determination of possible surface or low coronal
  associations. A specific example of one such eruptive-prominence
  associated event, that observed in both the inner and outer solar
  corona on August 5, 1980, is used to illustrate the magnitude of
  the uncertainty of determining an onset time of the ejection. It is
  noted that such uncertainties may influence statistically-determined
  associations.

---------------------------------------------------------
Title: Reply
Authors: Sime, D. G.; MacQueen, R. M.; Hundhausen, A. J.
1985JGR....90..563S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Recent Interpretation of Coronal Transient Results
Authors: MacQueen, R. M.
1985spit.conf..969M    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Coronal Mass Ejection Transients
Authors: MacQueen, R. M.
1985spit.conf...89M    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Density distribution in looplike coronal transients: A
    comparison of observations and a theoretical model
Authors: Sime, D. G.; MacQueen, R. M.; Hundhausen, A. J.
1984JGR....89.2113S    Altcode:
  Examination of the intensity changes in five outer coronal “looplike”
  transients observed by the Skylab coronagraph shows general tendencies
  (1) greatest concentration of material at the flanks rather than at
  the tops of the bright loops that characterize these transients, (2)
  presence of a large region of depleted density within these loops, and
  (3) developement of bright legs that contain most of the material in
  the transient and that display very little lateral motion as the top of
  the bright loop moves radially outward through the outer corona. These
  properties of looplike coronal transients provide useful constraints on
  theoretical models of this phenomenon. In particular, direct comparison
  of the observed density distributions with those predicted by models
  of compressional waves initiated by an impulsive energy release in
  the low corona are a necessary test of these models. These models
  predict a maximum enhancement at the top of the loop, rather than at
  the flanks and “legs” that move laterally with a significant fraction
  of the propagation speed of the loop top, in conflict with the observed
  tendencies. If the observed loops are taken to have the geometry assumed
  in the compressive wave models (“toroidal symmetry” about a rotation
  axis passing through the center of the sun), the predicted density
  enhancements are several times larger than those inferred from the
  observations. Agreement cannot be achieved without use of a geometry
  which conflicts with that used for the model calculations.

---------------------------------------------------------
Title: The Kinematics of Solar Inner Coronal Transients
Authors: MacQueen, R. M.; Fisher, R. R.
1983SoPh...89...89M    Altcode:
  The kinematic properties of a dozen `loop-like' coronal transients have
  been examined over the range 1.2-2.4 R⊙ from Sun center. Values and
  trends of transient geometry, including radial height, lateral width
  at maximum extent, distance from loop top to height of maximum width,
  and lateral width at a fixed height above the instrument occulting
  disk at 1.2 R⊙, are given. Radial and lateral speeds of expansion
  are tabulated, and range from 60-900 km s<SUP>-1</SUP>, and 10-500
  km s<SUP>-1</SUP>, respectively. Flare-associated events are found to
  exhibit the highest speeds, and show little acceleration with height;
  on the other hand, eruptiveassociated events exhibit large accelerations
  (some in excess of 50 m s<SUP>-2</SUP>). This clear discrimination
  between flare and eruptive-associated events suggests that two different
  physical processes are present; it is suggested that flare-associated
  events result from an impulsive, localized input to the corona. On
  the other hand, accelerated, eruptive-associated events are subjected
  to appreciable net forces over radial heights of one solar radius
  (or more) above the solar limb. It is conjectured that the pressure
  gradient forces responsible for the generation of the solar wind may
  play an important role in accelerating these latter events.

---------------------------------------------------------
Title: The excitation of type II radio bursts in the corona
Authors: Wagner, W. J.; MacQueen, R. M.
1983A&A...120..136W    Altcode:
  Simultaneous radioheliograph and orbital coronagraph observations
  of coronal transient activity shows metric type II radio emission
  originating early in the event, well below the visible white light
  transient. The authors suggest that the shock which excites the type
  II emission is independent of the transient, in the sense that it is
  initiated in the low corona (probably in association with a flare)
  and travels through the already-existing transient disturbance with
  a propagation speed significantly greater than that of the front
  edge of the transient itself. Radio emission then results when the
  flare shock overtakes, first, the region of principal density pile-up
  along the sides of the expanding transient and only later the top of
  the transient.

---------------------------------------------------------
Title: Detection of Slow, Bright Coronal Transients
Authors: Garcia, C.; Fisher, R.; MacQueen, R.
1983BAAS...15..706G    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Kinematics of Solar Coronal Transients
Authors: MacQueen, R. M.; Fisher, R. R.
1983BAAS...15..707M    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Density Distribution in Loop-Like Coronal Transients: A
    Comparison of Observations and a Theoretical Model
Authors: Sime, D. G.; MacQueen, R. M.; Hundhausen, A. J.
1983BAAS...15..707S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Properties of Coronal Voids
Authors: MacQueen, R. M.; Sime, D. G.; Picat, J. -P.
1983SoPh...83..103M    Altcode:
  Observations of the outer solar corona obtained by the High Altitude
  Observatory's coronagraph aboard Skylab reveal the presence of dark,
  ray-like structures in the corona. A systematic identification of these
  voids, which exist for periods of about 24 hr, is presented and their
  existence as a coronal phenomenon, as opposed to a subtle photographic
  effect, verified. Photometric analysis indicates that these features
  represent reductions in the coronal radiance on the order of 5% - or
  about 2-3 × 10<SUP>−10</SUP>B<SUB>⊙</SUB> at 3 R<SUB>⊙</SUB>. The
  use of a previously determined model of the electron component of the
  corona permits specification of the electron density in the voids
  over the range 2.5-4.5 R<SUB>⊙</SUB>. In spite of the inevitable
  uncertainties regarding their longitudinal extent, we estimate that
  their electron density is comparable to, or less than, that in coronal
  holes at similar heights. Projection of the phenomena onto synoptic
  surface maps indicates a close relationship with filaments and neutral
  lines; a potentially significant temporal correlation between the void
  formation and that of the underlying prominence is noted. The spatial
  and temporal resolution of the data set places stringent restrictions on
  any model which may be used to infer the physical processes of formation
  or decay of voids; several possibilities are suggested which involve
  either changes in the coronal base temperature or the magnetic flux.

---------------------------------------------------------
Title: Solar wind five. Proceedings of a conference held in Woodstock,
    Vermont, November 1 - 5, 1982.
Authors: Neugebauer, M.; Hollweg, J. V.; Barnes, A.; MacQueen, R.;
   Rosner, R.; Eddy, J. A.
1983swfp.book.....N    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Spacelab Lyman-Alpha and White Light Coronagraphs Program
Authors: Kohl, J. L.; Withbroe, G. L.; Weiser, H.; MacQueen, R. M.;
   Munro, R. H.
1981SSRv...29..419K    Altcode:
  The Harvard-Smithsonian Center for Astrophysics and the High Altitude
  Observatory have defined a joint coronagraphs experiment for a
  future Spacelab mission. The instrumentation package would include an
  ultraviolet light coronagraph to measure the intensity and profiles of
  spectral lines formed between 1.2 and 8 solar radii from Sun center and
  a white light coronagraph to measure the intensity and polarization
  of visible light. The overall goals of the joint program are to use
  new coronal plasma diagnostic techniques to understand the physical
  processes and mechanisms operating in the solar corona, to understand
  the acceleration of high-speed and low-speed solar wind streams and to
  extrapolate this knowledge to other stars in order to help understand
  the physics of stellar coronae and stellar mass loss.

---------------------------------------------------------
Title: The Evolution of a Coronal Streamer and the Photospheric
    Magnetic Field
Authors: Poland, A. I.; MacQueen, R. M.
1981SoPh...71..361P    Altcode:
  A large equatorial coronal streamer observed in the outer corona
  (3R<SUB>⊙</SUB>) grew in brightness and size during successive limb
  passages between October 6, 1973 and January 10, 1974 (solar rotations
  1606-1611). Unlike previous studies of streamers and their photospheric
  associations, no definite surface feature could be identified in the
  present case. This suggests that the streamer is associated with the
  large scale photospheric magnetic field. Comparison of the streamer
  growth with observed underlying photospheric magnetic flux changes
  indicated that as the streamer increased in brightness, areal extent,
  and density, the photospheric magnetic flux decreased. Three possible
  explanations for the streamer's growth are presented; the conceptually
  simplest being that the decrease in photospheric field results in an
  opening of the flux tubes under the streamer which permits an increased
  mass flux through the streamer.

---------------------------------------------------------
Title: The Pinhole/Occulter Facility
Authors: Hudson, H. S.; Kohl, J. L.; Lin, R. P.; MacQueen, R. M.;
   Tandberg-Hanssen, E.; Pabbs, J. R.
1981pof..rept.....H    Altcode:
  A large occulting system in space can be used for high resolution
  X-ray observations and for large aperture coronagraphic observations in
  visible and UV light. The X-ray observations can combine high angular
  resolution in hand (10 keV) X-radiation with the high sensitivity
  of a multiple pinhole camera, and can permit sensitive observations
  of bremsstrahlung from nonthermal particles in the corona. The
  large aperture coronagraphs have two major advantages: high angular
  resolution and good photon collection. This will permit observations
  of small scale structures in the corona for the first time and will
  give sufficient counting rates above the coronal background rates
  for sensitive diagnostic analysis of intensities and line profiles
  for coronal structures in the solar wind acceleration region. The
  technical basis for performing observations with a large occulting
  system in these three wavelength ranges is described as well as a
  pinhole/occulter facility presently being considered for Spacelab. Some
  indications about future developments are included.

---------------------------------------------------------
Title: New Mauna Loa coronagraph systems
Authors: Fisher, R. R.; Lee, R. H.; MacQueen, R. M.; Poland, A. I.
1981ApOpt..20.1094F    Altcode:
  A new set of instruments, consisting of two coronagraph systems,
  has been installed and is operating at the Mauna Loa Observing
  Station, Hawaii. The instruments are the 23-cm objective Mark III
  K-coronameter (K-III) system, a photoelectric instrument used to
  observe the inner solar corona from 1.2 R0 to 2.2 R0 and the 12.5-cm
  objective Prominence Monitor system used for the detection of H-alpha
  limb activity. New features of the K-coronameter system include the
  use of achromatic wave plates for wide bandpass operation and linear
  diode array detectors. Raster scans of the coronal image are obtained
  in 1.5 min for a critical sampling scheme of 20-sec of arc resolution
  (10 x 10-sec of arc pixels) in the coronal pB image. This represents
  a 350 information gain factor for each detection channel when compared
  with the previous Mauna Loa K-coronameters.

---------------------------------------------------------
Title: The high altitude observatory of the national center for
    atmospheric research Boulder, Colorado
Authors: MacQueen, R. M.
1980SoPh...68..411M    Altcode:
  The High Altitude Observatory attempts to carry out a balanced program
  of theoretical and experimental research in solar, solar-terrestrial,
  and stellar-related physics. The scientific efforts are carried
  out within a sectional structure including the major areas of Solar
  Atmosphere and Magnetic Fields, Coronal/Interplanetary Physics, and
  Solar Variability. As one division of a National Center, the Observatory
  attempts to provide leadership through operation and sponsorship of
  seminars on specialized topics and organization of workshops to exploit
  data collections. In addition to the examples given, the Observatory,
  under NASA sponsorship, has organized a workshop series on solar
  flares, a central theme of which was the interpretation of Skylab
  results. This effort has resulted in the publication of a volume Solar
  Flares, edited by P. Sturrock, Colorado Associated University Press,
  1979. Through these efforts, and the participation of individual staff
  members on advisory committees and working groups within the national
  and international framework, the Observatory continues to play a role
  in the guidance of research in solar and related physics.

---------------------------------------------------------
Title: The Orientation of Pre-Transient Coronal Magnetic Fields
Authors: Trottet, G.; MacQueen, R. M.
1980SoPh...68..177T    Altcode:
  Loop-like white light coronal transients are generally believed to
  be nearly planar sheets which are thin compared to the loop extent;
  however, this picture may be questioned since virtually no observations
  (of the more than 100 transient events observed during 1973-74 Skylab
  period) show such loops edge-on. From the group of transient events
  studied by Munro etal. (1979) for which definite surface associations
  exist, we find loop transients are strongly correlated with filament
  regions where the filament axis was oriented north-south. From
  direct soft X-ray observations of an expanding arch, the possible
  identification of the soft X-ray signature of footpoints of transient
  loops, and monochramatic observations of low coronal loops, we infer
  that loop-like coronal transients have their origin in low-lying coronal
  loops nearly co-planar with the north-south aligned filament axis. The
  situation with respect to non-loop events is less clear; such events
  apparently often arise from more complex filament geometries. Possible
  reasons for the preference of transients to arise from north-south
  filament-oriented regions are discussed.

---------------------------------------------------------
Title: Measurements of coronal kinetic temperatures from 1.5 to 3
    solar radii
Authors: Kohl, J. L.; Weiser, H.; Withbroe, G. L.; Noyes, R. W.;
   Parkinson, W. H.; Reeves, E. M.; Munro, R. H.; MacQueen, R. M.
1980ApJ...241L.117K    Altcode:
  A rocket-borne Lyman-alpha coronagraph has been used to make the first
  measurements of the spectral line profile of resonantly scattered
  hydrogen Lyman-alpha coronal radiation between 1.5 and 3 solar
  radii. These data provide, for the first time, direct measurements of
  coronal temperatures above 1.5 solar radii. Data were obtained in a
  coronal hole, quiet region, and streamer. The widths of the profiles
  from the quiet region decrease with height and correspond to a steady
  decrease in hydrogen kinetic temperature, with increasing radius, from
  about 2.5 million K at r = 2 solar radii to about 1 million K at r =
  9 solar radii. In the coronal hole the measured line widths indicate
  a kinetic temperature of 1.8 million K at r = 2.5 solar radii.

---------------------------------------------------------
Title: The Spacelab Lyman-Alpha and White-Light Coronagraphs Program
Authors: Kohl, J. L.; MacQueen, R. W.; Withbroe, G. L.; Munro, R.;
   Weiser, H.
1980BAAS...12..793K    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Coronal Transients: A Summary
Authors: MacQueen, R. M.
1980RSPTA.297..605M    Altcode: 1980RSLPT.297..605M
  Observations with orbiting coronagraphs have illuminated the role
  of coronal mass ejections in solar activity, and raised a number
  of questions concerning their origin, the nature of the forces
  driving the coronal material, and their signature in interplanetary
  space. Current models of the ejection process -- including
  propagation of loops as a result of azimuthal field gradients,
  ring currents or a build-up of magnetic pressure from below -- are
  summarized, as are magnetohydrodynamic codes intended to stimulate
  transient conditions. Metric radio observations, can, in principle,
  distinguish the relative role of the magnetic field in the ejection
  process; observations to date are surveyed. It is concluded that at
  present, no compelling evidence is available to distinguish between
  transient driving mechanisms, but future observations of the corona
  and interplanetary medium may resolve the present ambiguity.

---------------------------------------------------------
Title: The High Altitude Observatory coronagraph/polarimeter on the
    Solar Maximum Mission.
Authors: MacQueen, R. M.; Csoeke-Poeckh, A.; Hildner, E.; House, L.;
   Reynolds, R.; Stanger, A.; Tepoel, H.; Wagner, W.
1980SoPh...65...91M    Altcode:
  The High Altitude Observatory Coronagraph/Polarimeter, to be flown
  on the National Aeronautics and Space Administration's Solar Maximum
  Mission satellite, is designed to produce images of the solar corona in
  seven wavelength bands in the visible spectral range. The spectral bands
  have been chosen to specifically exclude or include `chromospheric'
  spectral lines, so as to allow discrimination between ejecta at high
  (coronal) and low (chromospheric) temperatures, respectively. In
  addition, the instrument features spectral filters designed to permit
  an accurate color separation of the F and K coronal components, and a
  narrow band (5.5 Å) filter to observe the radiance and polarization
  of the Fe XIV 5303 Å line. The effective system resolution is better
  than 10 arc sec and the instrument images a selected quadrant (or
  smaller field) on an SEC vidicon detector. The total height range
  that may be recorded encompasses 1.6 to more than 6.0R<SUB>⊙</SUB>
  (from Sun center). The instrument is pointed independently of the
  SMM spacecraft, and its functions are controlled through the use
  of a program resident within the onboard spacecraft computer. Major
  experimental goals include: (a) Observation of the role of the corona
  in the flare process and of the ejecta from the flare site and the
  overlying corona; (b) the study of the direction of magnetic fields in
  stable coronal forms, and, perhaps, ejecta; and (c) examination of the
  evolution of the solar corona near the period of solar maximum activity.

---------------------------------------------------------
Title: National-Center Atmospheric Research
Authors: MacQueen, R. M.
1980BAAS...12..279M    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Skylab observations of the coronal structure overlying a type
    III producing active region.
Authors: Pick, M.; Trottet, G.; MacQueen, R. M.
1979SoPh...63..369P    Altcode:
  The coronal structure overlying, and presumably associated with, an
  isolated active region, McMath 12686, is identified during its west
  limb passage 15-17 January 1974. The region had a `flaring site' on
  its border close to a plage filament and exhibited various forms of
  activity, including type III burst production, during the three days
  of study. Although the coronal structure overlying the region was of
  small scale, its estimated electron density was ∼10 × that of the
  background corona, and it varied in density by a factor of two over
  a time scale of hours. Some implications of such a structure on the
  interpretation of type III emission are considered.

---------------------------------------------------------
Title: Lyman-α and White Light Observations of the Outer Solar
    Corona.
Authors: Munro, R. H.; Kohl, J. L.; MacQueen, R. M.; Noyes, R. W.;
   Parkinson, W. H.; Weiser, H.; Withbroe, G. L.
1979BAAS...11..398M    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The association of coronal mass ejection transients with
    other forms of solar activity.
Authors: Munro, R. H.; Gosling, J. T.; Hildner, E.; MacQueen, R. M.;
   Poland, A. I.; Ross, C. L.
1979SoPh...61..201M    Altcode:
  Coronal mass ejection transients observed with the white light
  coronagraph on Skylab are found to be associated with several other
  forms of solar activity. There is a strong correlation between
  such mass ejection transients and chromospheric Hα activity, with
  three-quarters of the transients apparently originating in or near
  active regions. We infer that 40% of transients are associated with
  flares, 50% are associated with eruptive prominences solely (without
  flares), and more than 70% are associated with eruptive prominences or
  filament disappearances (with or without flares). Nine of ten flares
  which displayed apparent mass ejections of Hα-emitting material from
  the flare site could be associated with coronal transients. Within
  each class of activity, the more energetic events are more likely to
  be associated with an observable mass ejection.

---------------------------------------------------------
Title: Multicolor imaging and photopolarimetry: Disk features,
    K and F coronas, zodiacal light
Authors: Weinberg, J. L.; MacQueen, R. M.
1978clus.nasa..143W    Altcode:
  The unique vantage points and viewing geometries afforded by a close-in
  solar probe are briefly examined with regard to line and continuum
  measurements of features on the solar disk, the K and F coronas, and
  the zodiacal light. Common instrument and observing requirements are
  identified, suggesting that a single instrument could provide much of
  the necessary observational data on these phenomena.

---------------------------------------------------------
Title: Temporal evolution of the equatorial K-corona.
Authors: MacQueen, R. M.; Poland, A. I.
1977SoPh...55..143M    Altcode:
  Observations of the equatorialK-coronal radiance at 2.5R<SUB>⊙</SUB>
  from Sun center and its variation with time, on a daily basis,
  during the Skylab mission (May 1973-February 1974) are presented. The
  observations are subdivided into three periods, each characterized
  by a different variation of the radiance pattern with time. During
  the initial period, encompassing two solar rotations, there are
  several data gaps, but the radiance pattern shows a more or less
  smooth variation with time; however, during the second period (also
  about two solar rotations duration) the radiance signal is neither
  persistent on the short term nor recurrent from one limb passage to
  the next. Finally, during the last period, of five solar rotations
  duration, the radiance signal exhibits an orderly periodic behavior
  of increasing intensity. These results are interpreted as indicating
  a general simplification of the coronal magnetic field through the
  mission and, in comparison with harmonic analysis of the surface
  magnetic field (Levine, 1977), as indicating a rapid response of
  equatorial outer coronal structures to abrupt changes in the global
  surface field structure.

---------------------------------------------------------
Title: Radiance calibration of the High Altitude Observatory
    white-light coronagraph on Skylab.
Authors: Poland, A. I.; Gosling, J. T.; MacQueen, R. M.; Munro, R. H.
1977ApOpt..16..926P    Altcode:
  The processing of over 35,000 photographs of the solar corona obtained
  by the white-light coronograph on Skylab is described. Calibration of
  the vast amount of data was complicated by temporal effects of radiation
  fog and latent image loss. These effects were compensated by imaging
  a calibration step wedge on each data frame. Absolute calibration of
  the wedge was accomplished through comparison with a set of previously
  calibrated glass opal filters. Analysis employed average characteristic
  curves derived from measurements of step wedges from many frames within
  a given camera half-load. The net absolute accuracy of a given radiance
  measurement is estimated to be 20%.

---------------------------------------------------------
Title: Measurement of stray radiance in the High Altitude
    Observatory's Skylab coronagraph.
Authors: Csoeke-Poeckh, A.; MacQueen, R. M.; Poland, A. I.
1977ApOpt..16..931C    Altcode:
  The paper outlines two techniques used for determining the instrumental
  stray radiance from orbital results obtained with the Skylab white light
  coronagraph. The first technique employs images of the lunar disk made
  near the time of solar eclipse to compare the apparent contrasts of
  maria and highlands recorded by the coronograph with those of previous
  studies and then determine the magnitude of the stray radiance and its
  variation along a radius. The second method determines the azimuthal
  variation of the stray radiance by measuring the change in the net
  radiance of a point in the coronal images as the image is rotated.

---------------------------------------------------------
Title: The Background Corona Near Solar Minimum.
Authors: Saito, K.; Poland, A.; Munro, R.; MacQueen, R.
1977BAAS....9Q.371S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: White light and radio studies of the coronal transient of 14
    15 September 1973
Authors: Smerd, S. F.; Dulk, G. A.; MacQueen, R. M.; Gosling,
   J. T.; Magun, A.; Stewart, R. T.; Sheridan, K. V.; Robinson, R. D.;
   Jacques, S.
1976SoPh...49..369S    Altcode:
  Observations of a coronal transient event were obtained in
  white light by the Skylab coronagraph and at metric wavelengths
  by the radioheliograph and spectrograph at Culgoora and the
  spectrograph-interferometer at Boulder. The continuum radio burst was
  found to originate above the outward-moving white light loop - a region
  of compressed material headed by a bow wave. The computed density
  in the region of radio emission, based on either gyro-synchrotron or
  harmonic plasma radiation mechanisms, was approximately 10 times the
  ambient coronal density; this is compatible with the density deduced
  from the white light observations. The magnetic energy density derived
  from the radio observations was greater than 10 times the thermal
  energy density, marginally larger than the kinetic energy density in
  the fastest moving portion of the transient, and considerably larger
  in most other regions. The ambient medium, the white light front, the
  compression region, the loop, and the slower, massive flow of material
  behind are each examined. It is found that the plasma was magnetically
  controlled throughout, and that magnetic forces provided the principal
  mechanism for acceleration of the transient material from the Sun.

---------------------------------------------------------
Title: White Light and Radio Studies of the Coronal Transient of
14-15 September 1973. I: Material Motions and Magnetic Field
Authors: Dulk, G. A.; Jacques, S.; Smerd, S. F.; MacQueen, R. M.;
   Gosling, J. T.; Steward, R. T.; Sheridan, K. V.; Robinson, R. D.;
   Magun, A.
1976SoPh...49..369D    Altcode:
  Observations of a coronal transient event were obtained in white
  light by the Skylab coronagraph and at metric wavelengths by the
  radioheliograph and spectrograph at Culgoora, Australia, and the
  spectrograph-interferometer at Boulder, Colo. The continuum radio burst
  was found to originate above the outward-moving white-light loop, a
  region of compressed material headed by a bow wave. The computed density
  in the region of radio emission, based on either gyrosynchrotron or
  harmonic plasma radiation mechanisms, was approximately 10 times the
  ambient coronal density; this is compatible with the density deduced
  from the white-light observations. The magnetic-energy density derived
  from the radio observations was greater than 10 times the thermal
  energy density, marginally larger than the kinetic energy density in
  the fastest-moving portion of the transient, and considerably larger
  in most other regions. The ambient medium, the white-light front, the
  compression region, the loop, and the slower massive flow of material
  behind are each examined. It is found that the plasma was magnetically
  controlled throughout and that magnetic forces provided the principal
  mechanism for acceleration of the transient material from the sun.

---------------------------------------------------------
Title: The speeds of coronal mass ejection events.
Authors: Gosling, J. T.; Hildner, E.; MacQueen, R. M.; Munro, R. H.;
   Poland, A. I.; Ross, C. L.
1976SoPh...48..389G    Altcode:
  The outward speeds of mass ejection events observed with the
  white light coronagraph experiment on Skylab varied over a range
  extending from less than 100 km s<SUP>−1</SUP> to greater than
  1200 km s<SUP>−1</SUP>. For all events the average speed within
  the field of view of the experiment (1.75 to 6 solar radii) was 470
  km s<SUP>−1</SUP>. Typically, flare associated events (Importance
  1 or greater) traveled faster (775 km s<SUP>−1</SUP>) than events
  associated with eruptive prominences (330 km s<SUP>−1</SUP>); no
  flare associated event had a speed less than 360 km s<SUP>−1</SUP>,
  and only one eruptive prominence associated event had a speed greater
  than 600 km s<SUP>−1</SUP>. Speeds versus height profiles for a
  limited number of events indicate that the leading edges of the ejecta
  move outward with constant or increasing speeds.

---------------------------------------------------------
Title: Initial Results from the High Altitude Observatory White
    Light Coronagraph on Skylab - A Progress Report
Authors: MacQueen, R. M.; Gosling, J. T.; Hildner, E.; Munro, R. H.;
   Poland, A. I.; Ross, C. L.
1976RSPTA.281..405M    Altcode: 1976RSLPT.281..405M
  The frequent, periodic observations by the white light coronagraph
  allow an examination of coronal variations over a broad range of
  temporal scales. Examples of the slowest and most rapid variations
  are presented. An example of extremely slow coronal variations is the
  gradual evolution - to a large equatorial streamer - in association
  with a marked decrease in solar activity, as the total magnetic flux
  in one hemisphere decreased. Another example is given of a long-lived
  quasi-stable coronal streamer, apparently associated with a stable
  filament channel; comparison of this streamer with coronal potential
  magnetic field computations show little correlation. The remainder
  of the paper summarizes some results on coronal transients - the most
  rapid variations observed. Characteristic mass and energies involved
  in mass ejection transients, their temporal and spatial distributions,
  their associations with surface phenomena and possible interplanetary
  signatures, and finally their role in coronal evolution are briefly
  noted.

---------------------------------------------------------
Title: Frequency of coronal transients and solar activity.
Authors: Hildner, E.; Gosling, J. T.; MacQueen, R. M.; Munro, R. H.;
   Poland, A. I.; Ross, C. L.
1976SoPh...48..127H    Altcode:
  The High Altitude Observatory's white light coronagraph aboard Skylab
  observed some 110 coronal transients - rapid changes in appearance
  of the corona - during its 227 days of operation. The longitudes
  of the origins of these transients were not distributed uniformly
  around the solar surface (51 of the 100 events observed in seven
  solar rotations arose from a single quadrant of longitude). Further,
  the frequency of transient production from each segment of the solar
  surface was well correlated with the sunspot number and Ca II plage
  (area × brightness) index in the segment, rotation by rotation. This
  correlation implies that transients occur more often above strong
  photospheric and chromospheric magnetic fields, that is, in regions
  where the coronal magnetic field is stronger and, perhaps, more
  variable. This pattern of occurrence is consistent with our belief
  that the forces propelling transient material outward are, primarily,
  magnetic. A quantitative relation between transient production from
  an area and the Zürich sunspot number appropriate to that area is
  derived, and we speculate that the relation is independent of phase
  in the solar activity cycle. If true, the Sun may give rise to as many
  as 100 white light coronal transients per month at solar cycle maximum.

---------------------------------------------------------
Title: Equatorial Electron Coronal Variations
Authors: MacQueen, R.
1976BAAS....8..369M    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Speeds of Coronal Mass Ejection Events
Authors: Hildner, E.; MacQueen, R. M.; Munro, R. H.; Poland, A. I.;
   Ross, C. L.; Gosling, J. T.
1976BAAS....8R.368H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Movie of Comet Kohoutek (1973f) as Observed Near Minimum
    Elongation by the Hao Coronagraph Aboard SKYLAB
Authors: Hildner, E.; Gosling, J. T.; MacQueen, R. M.; Munro, R. H.;
   Poland, A. I.; Ross, C. L.
1976NASSP.393..124H    Altcode: 1976IAUCo..25..124H
  No abstract at ADS

---------------------------------------------------------
Title: Radiation and structure of the solar atmosphere (Radiation
    et structure de l'atmosphère solaire).
Authors: Giovanelli, R. G.; Mein, P.; Bappu, M. K. V.; Jordan, C.;
   MacQueen, R. M.
1976IAUTA..16b..55G    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar activity (Activité solaire).
Authors: Newkirk, G.; Dunn, R. B.; Mehltretter, P.; MacQueen, R.;
   Bonnet, R. M.; White, O. R.; Fokker, A. D.; Zwaan, C.; Bruzek, A.;
   Durrant, C.; Grossmann-Doerth, U.; Mehltretter, J. P.; Svestka, Z.;
   de Feiter, L. D.; Tandberg-Hanssen, E.; Howard, R.; Stix, M.; Pneuman,
   G. W.; Hundhausen, A. J.; Sawyer, C.; Simon, P.
1976IAUTA..16b..13N    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: A search for forward scattering of sunlight from lunar
    libration clouds
Authors: Munro, R. H.; Gosling, J. T.; Hildner, E.; MacQueen, R. M.;
   Poland, A. I.; Ross, C. L.; Hopfield, A.
1975P&SS...23.1313M    Altcode:
  An attempt to determine the radiance of forward scattered sunlight
  from particles in lunar libration regions was made with the white light
  coronagraph on Skylab. The libration regions could not be distinguished
  against the solar K + F coronal background; an upper limit to the
  libration cloud radiance is determined to be 2·5 × 10 <SUP>-11</SUP>B
  <SUB>⊚</SUB>, where B <SUB>⊚</SUB> is the mean radiance of the
  solar disk. Employing a model of the particle composition and size
  distribution which has been proposed for the interplanetary medium,
  we determine upper limits for the density enhancements in the libration
  region from the upper limit of the forward scattered radiance presented
  herein. Similarly, the actual spatial density enhancement is calculated
  using the earlier observations of the libration region backscattered
  radiance (Roach, 1975). Enhancements of a factor of 10 <SUP>2</SUP>-10
  <SUP>3</SUP> are thus determined, depending upon material composition
  and size distribution used. By combining the forward and backscatter
  observations, it is possible to eliminate from consideration clouds
  whose power law particle size distribution exponent k is 2·5
  and complex index of refraction m is 1·33-0.05 i and 1·50-0.05 i
  (i.e. absorbing ice and quartz particles, respectively). Finally, the
  radiance contrast of a possible model libration cloud is calculated with
  respect to the K- and F-corona/zodiaal light background and is shown
  to be a maximum in the vicinity of solar elongation angle ∼30 deg.

---------------------------------------------------------
Title: The Large Coronal Transient of 10 June 1973. I: Observational
    Description
Authors: Hildner, E.; Gosling, J. T.; MacQueen, R. M.; Munro, R. H.;
   Poland, A. I.; Ross, C. L.
1975SoPh...42..163H    Altcode:
  During the 8.5 month flight of the High Altitude Observatory's white
  light coronagraph on board Skylab, over 100 coronal transients were
  observed. In this paper we present a description of one well observed
  loop transient, that of 10 June 1973. The transient apparently resulted
  from the eruption of a quiescent prominence on the limb; the emergence
  of a new, bipolar active region near the prominence may have caused
  the eruptior. The transient's leading edge rose from 3.6 to 5.0
  solar radii (R<SUB>⊙</SUB>) from Sun center at approximately 500 km
  s<SUP>−1</SUP> during the 32 min of coronagraph observations. Material
  in a pre-existing streamer was swept away by the transient, causing
  the streamer to disappear. The mass ejected into the corona above a
  projected height of 2 R<SUB>⊙</SUB> was ≈ 5.4 × 10<SUP>15</SUP> g,
  the potential energy associated with the ejected transient material was
  ⩾7.0 × 10<SUP>30</SUP> erg, and the kinetic energy of the ejected
  material is estimated as 1.7 × 10<SUP>30</SUP> erg. The 10 June 1973
  transient was, in most respects, typical of other loop transients
  observed by Skylab.

---------------------------------------------------------
Title: White Light and Radio Studies of the Coronal Transient of
    14-15 September 1973 I. Observations and Emission Mechanisms
Authors: Robinson, R.; MacQueen, R. M.
1975BAAS....7..348R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Direct Observations of a Flare Related Coronal and Solar
    Wind Disturbance
Authors: Gosling, J. T.; Hildner, E.; MacQueen, R. M.; Munro, R. H.;
   Poland, A. I.; Ross, C. L.
1975SoPh...40..439G    Altcode:
  Numerous mass ejections from the Sun have been detected with orbiting
  coronagraphs. Here for the first time we document and discuss the direct
  association of a coronagraph observed mass ejection, which followed a
  2B flare, with a large interplanetary shock wave disturbance observed
  at 1 AU. Estimates of the mass (2.4 × 10<SUP>16</SUP> g) and energy
  content (1.1 × 10<SUP>32</SUP> erg) of the coronal disturbance are
  in reasonably good agreement with estimates of the mass and energy
  content of the solar wind disturbance at 1 AU. The energy estimates as
  well as the transit time of the disturbance are also in good agreement
  with numerical models of shock wave propagation in the solar wind.

---------------------------------------------------------
Title: Photography of comet Kohoutek by Skylab white light
    coronagraph.
Authors: MacQueen, R. M.; Gosling, J. T.; Hildner, E.; Munro, R. H.;
   Poland, A. I.; Ross, C. L.; Keller, H. U.; Schmidt, H. U.
1975NASSP.355...19M    Altcode: 1975coko.conf...19M
  No abstract at ADS

---------------------------------------------------------
Title: Mass ejections from the Sun: A view from Skylab
Authors: Gosling, J. T.; Hildner, E.; MacQueen, R. M.; Munro, R. H.;
   Poland, A. I.; Ross, C. L.
1974JGR....79.4581G    Altcode:
  More than 30 instances of sudden mass ejections from the sun were
  observed with the white light coronagraph experiment aboard Skylab
  during the first 118 days of the mission. Typically, these ejections
  appear as large magnetic loops rooted at the sun, yet expanding
  outward through the solar corona at speeds of the order of 400 km
  s<SUP>-1</SUP>. The loops always appear to retain their magnetic
  connection to the sun. Eighteen of these ejections were associated
  with active and eruptive prominences and surges; only three ejections
  appear to have been flare initiated. Associations with ground-detected
  metric wavelength type 2 and 4 radio bursts occur for about 30% of these
  events; however, ground-detected type 2 and 4 radio bursts originating
  near the limb are almost invariably accompanied by coronagraph-observed
  ejections. Pressure or MHD waves run out ahead of the transient material
  ejecta; at times these waves can be detected by their effects on nearby
  coronal structures. For one event, that of August 10, 1973, we make
  the following estimates: (1) mass content, 4 × 10<SUP>15</SUP> grams;
  (2) mass flow rate, 1.1 × 10<SUP>12</SUP> grams s<SUP>-1</SUP> (3)
  energy content, 8.4 × 10<SUP>30</SUP> ergs; and (4) energy flow rate,
  7.7 × 10<SUP>26</SUP> ergs s<SUP>-1</SUP>. Locally, this represents
  a significant mass and energy input to the solar wind; we suggest that
  the ejections are the coronal counterparts of nonrecurrent (including
  shocks) solar wind disturbances detected near the orbit of the earth.

---------------------------------------------------------
Title: Observed streamer curvature in the outer solar corona
Authors: Wilson, D. C.; MacQueen, R. M.
1974JGR....79.4575W    Altcode:
  The first observations of coronal streamers to an elongation angle
  of 12.5° (50 R<SUB>s</SUB> from sun center) were taken aboard the
  Apollo 15 command module in lunar orbit. Streamer curvature in both
  heliocentric latitude and heliocentric longitude may be determined from
  the positions of three curved streamers. This curvature is interpreted
  by assuming that it is not transient and that streamers trace flow from
  a stationary position on the solar surface. The azimuthal curvature
  is explained by corotation of streamer material with the sun out to
  approximately 25 R<SUB>s</SUB>, followed by a constant radial velocity
  of 275 km/s and force free flow to 60 R<SUB>s</SUB>. The curvature
  toward the solar equator implies a meridional flow of 45 ±15 km/s
  between 50 and 60 R<SUB>s</SUB>. If constant angular momentum is
  assumed beyond 60 R<SUB>s</SUB>, the resultant azimuthal and meridional
  velocities are consistent with the solar wind observed at 1 AU. The
  radial velocity, including a small expected acceleration between 60
  R<SUB>s</SUB> and 1 AU, is typical of slow-speed solar wind. Streamer
  curvature is compared with interplanetary magnetic field models.

---------------------------------------------------------
Title: The coronal radiance in the intermediate infrared.
Authors: Mankin, W. G.; MacQueen, R. M.; Lee, R. H.
1974A&A....31...17M    Altcode:
  Summary. An observed value of the spectral mean of the coronal radiance
  in the intermediate infrared U.5-13 of 9+5 x - - at 4 R0 is presented,
  with the observed change in radiance with elongation angle over the
  range 3.5- 12.5 R0. The observations are consistent with the model of
  silicate emission proposed by Kaiser (1970), but a two component model
  is required to reconcile these observations and the measurements by
  Peterson (1971) at wavelengths of 2.2 and less. Key words: F corona -
  thermal emission - interplanetary dust

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Title: The High Altitude Observatory White Light Coronagraph
    Experiment
Authors: MacQueen, R. M.; Gosling, J. T.; Hildner, E.; Munro, R. H.;
   Poland, A. I.; Ross, C. L.
1974IAUS...57..505M    Altcode:
  No abstract at ADS

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Title: Airborne far infrared solar spectroscopy
Authors: Mankin, W. G.; Eddy, J. A.; Lee, R. H.; MacQueen, R. M.
1974SPIE...44..133M    Altcode:
  A description is provided of an instrument which has been developed
  to measure the far infrared brightness temperature of the sun. The
  instrument consists of a 20 cm aperture photoguided telescope, a high
  resolution Michelson interferometer, a helium cooled gallium doped
  germanium bolometer, and two blackbodies for radiometric reference. The
  instrument along with its supporting electronic equipment, including
  a minicomputer, is mounted aboard a Sabreliner, which carries it to
  an altitude of 12 km for observations above the tropopause.

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Title: The High Altitude Observatory white light coronagraph
Authors: MacQueen, R. M.; Gosling, J. T.; Hildner, E.; Munro, R. H.;
   Poland, A. I.; Ross, C. L.
1974SPIE...44..207M    Altcode:
  Most of the instruments of the Apollo Telescope Mount are
  satellite-borne because they observe in regions of the electromagnetic
  spectrum where the telluric atmosphere is opaque. For the coronagraph of
  the High Altitude Observatory, observing in visible light, this is not
  so. The structure of the solar corona is obscured from ground-based
  observations by scattered light in the earth's atmosphere, and
  observations from space are required to reduce this scattered light
  to a level which is negligible with respect to the brightness of the
  outer solar corona.

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Title: The High Altitude Observatory white-light coronagraph
    experiment of Skylab.
Authors: MacQueen, R. M.
1974JOSA...64..523M    Altcode:
  No abstract at ADS

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Title: The Outer Solar Corona as Observed from Skylab: Preliminary
    Results
Authors: MacQueen, R. M.; Eddy, J. A.; Gosling, J. T.; Hildner, E.;
   Munro, R. H.; Newkirk, G. A., Jr.; Poland, A. I.; Ross, C. L.
1974ApJ...187L..85M    Altcode:
  The white-light coronagraph experiment has made frequent, periodic
  observations of the solar corona from 1.5 R0 to 6.0 R0 during the Skylab
  mission, and these observations will permit the determination of the
  three-dimensional extent of coronal forms. There are several time
  scales on which visual changes in coronal structures occur, ranging
  from approximately one-half rotation to less than hours. A number of
  events corresponding to the shortest time scale - coronal transients
  - cause major restructuring of the corona. Subject headings: corona,
  solar - solar wind

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Title: The High Altitude Observatory white light coronagraph.
Authors: MacQueen, R. M.; Gosling, J. T.; Hildner, E.; Munro, R. H.;
   Poland, A. I.; Ross, C. L.
1974inas.conf..207M    Altcode:
  No abstract at ADS

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Title: Skylab: a Progress Report (presented by G. Newkirk)
Authors: MacQueen, R. M.
1974IAUS...57..489M    Altcode:
  No abstract at ADS

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Title: Airborne far infrared solar spectroscopy.
Authors: Mankin, W. G.; Eddy, J. A.; Lee, R. H.; MacQueen, R. M.
1974inas.conf..133M    Altcode:
  No abstract at ADS

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Title: Observations from space of the solar corona/inner zodical light
Authors: Macqueen, R. M.; Ross, C. L.; Matingly, T.
1973P&SS...21.2173M    Altcode:
  Observations, from the Apollo 16 Spacecraft, in lunar orbit, of
  the total radiance of the K + F corona, from 3 R<SUB>⊙</SUB> to
  55 R<SUB>⊙</SUB> are presented and discussed. The logarithmic
  slope of the K + F coronal radiance, in the region r &gt; 20
  R<SUB>⊙</SUB>, is found to be n = 1.93, slightly less steep than
  previous determinations. The photometric axis of the radiance is found
  to be displaced 3 ± 1° north of the ecliptic, for the region r &gt;
  20 R<SUB>⊙</SUB>, and this displacement is interpreted as an annual
  variation due to non-coincidence of the ecliptic and the symmetry axis
  of the zodiacal cloud.

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Title: Study of He I Emission Lines in the Solar Atmosphere. II. The
    Infrared Lines at 10 830 A and 20 581 A
Authors: Streete, J. L.; MacQueen, R. M.; Tandberg-Hanssen, E.
1973A&A....28..125S    Altcode:
  Summary. The 20581 A line of the He I singlet series has been
  observed for the first time in two quiescent prominences with a new
  all-reflective system. Simultaneously we observed the corresponding
  triplet line at 10830 A and studied the triplet-singlet line intensity
  ratio. librium, we find the ratio to vary from about 125 to 575 in
  different parts of the prominences observed. We deduce from these
  data that the ratio is determined by the optical depth in the 584 A
  resonance line, whose net radiative bracket exhibits values between
  approximately 5 x i0- and 2 x i0- . While this ratio should have values
  around 45 for a prominence plasma in local thermodynamic equi Key words:
  helium lines - prominences - excitation conditions

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Title: The Outer Solar Corona as Observed from Skylab: Preliminary
    Results.
Authors: Poland, A. I.; Gosling, J. T.; Hildner, E. G.; MacQueen,
   R. M.; Munro, R. H.; Ross, C. L.
1973BAAS....5..419P    Altcode:
  No abstract at ADS

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Title: Observed Streamer Curvature in the Outer Solar Corona.
Authors: Wilson, D. C.; MacQueen, R. M.
1973BAAS....5..446W    Altcode:
  No abstract at ADS

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Title: Observations of Far Infrared Atmospheric Windows at 44
    cm<SUP>-1</SUP> and 50 cm<SUP>-1</SUP> from Pikes Peak
Authors: Mankin, W. G.; Eddy, J. A.; MacQueen, R. M.; Lee, R. H.;
   Querfeld, C. W.
1973NPhS..245....8M    Altcode: 1973Natur.245....8M
  ABSORPTION by atmospheric water vapour seriously restricts astronomical
  observations from the ground in the far infrared region of the
  spectrum. Between 300 cm<SUP>-1</SUP> and 18 cm<SUP>-1</SUP>, the
  atmosphere is nearly opaque from the ground, except from high mountain
  sites where weak windows appear at 29 and 22 cm<SUP>-1</SUP> (350 and
  450 µm). These windows were first observed by Gebbie<SUP>1</SUP>;
  they have since been used by several investigators for mountain top
  astronomical measurements<SUP>2-10</SUP>. To our knowledge, there
  have been no astronomical observations from the ground in the region
  between 300 cm<SUP>-1</SUP> and the 29 cm<SUP>-1</SUP> window. In this
  frequency decade of the electromagnetic spectrum astronomy has required
  the use of aircraft<SUP>11-16</SUP> and balloons<SUP>17-24</SUP>
  as observing platforms.

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Title: Measurements of the Solar Brightness Temperature in the
    Far Infrared
Authors: Eddy, J. A.; Lee, R. H.; MacQueen, R. M.; Mankin, W. G.
1973BAAS....5..271E    Altcode:
  No abstract at ADS

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Title: Solar Corona Photography
Authors: MacQueen, R. M.; Ross, C. L.; Evans, R. E.
1973NASSP.330R..34M    Altcode:
  No abstract at ADS

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Title: Observations of Coronal Forms: 31 July - 13 September 1971
Authors: MacQueen, R. M.; Ross, C. L.; Hansen, R. T.; Dollfus, A.;
   Mouradian, Z.; Worden, A.
1972BAAS....4Q.387M    Altcode:
  No abstract at ADS

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Title: Observations of Coronal Forms: 7 March - 7 June 1970
Authors: Hansen, R. T.; Hansen, S. F.; Newkirk, G. A.; MacQueen,
   R. M.; Gosling, J. T.; Poland, A. I.
1972BAAS....4T.383H    Altcode:
  No abstract at ADS

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Title: The intermediate infrared coronal radiance.
Authors: Mankin, W. G.; MacQueen, R. M.; Lee, R. H.
1971BAAS....3R.262M    Altcode:
  No abstract at ADS

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Title: Computer Controlled Telescope and Interferometer for Eclipse
    Observations
Authors: Mankin, William G.; MacQueen, Robert M.; Lee, Robert H.
1971fosp.conf..267M    Altcode:
  No abstract at ADS

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Title: Far infrared airborne spectroscopy.
Authors: Eddy, J. A.; Lee, R. H.; Léna, P. J.; MacQueen, R. M.
1970ApOpt...9..439E    Altcode:
  Equipment and techniques employed in an airborne far ir (80-400 μ)
  spectral measurement of the solar brightness temperature are described,
  with particular attention paid to the scanning Michelson interferometer
  and the radiometric calibration. The airborne performance of several
  telescopic guiding systems, a liquid helium cooled bolometer, and golay
  cells are discussed, summarizing experience gained on twenty-five jet
  aircraft flights.

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Title: A computer-controlled infrared eclipse telescope.
Authors: Lee, R. H.; MacQueen, R. M.; Mankin, W. G.
1970ApOpt...9.2653L    Altcode:
  No abstract at ADS

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Title: Far Infrared Measurement of the Solar Minimum Temperature
Authors: Eddy, John A.; Léna, Pierre J.; MacQueen, Robert M.
1969SoPh...10..330E    Altcode:
  Radiometric measurement of the brightness temperature of the mean
  solar disk has been made in the wavelength range from 238 μ to 312
  μ (42.1 cm<SUP>-1</SUP> to 32.1 cm<SUP>-1</SUP>), using a Michelson
  interferometer of resolution 0.25 cm<SUP>-1</SUP>, carried on the NASA
  research aircraft at altitude 12.6 km. A mean temperature 4370 ± 260
  K is obtained. The result is compared with other measurements of the
  solar minimum temperature and with the prediction of the BCA Model.

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Title: The Temperature Minimum from Far-Infrared Measurements
Authors: Eddy, John A.; Lena, Pierre J.; MacQueen, R. M.
1969BAAS....1..275E    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar Brightness Temperature and Spectra: 80-400 Microns
    Wavelength
Authors: Eddy, John A.; Léna, Pierre J.; MacQueen, R. M.
1969BAAS....1Q.187E    Altcode:
  No abstract at ADS

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Title: Infrared scattering observations in the upper atmosphere
Authors: Eddy, John A.; MacQueen, Robert M.
1969JGR....74.3322E    Altcode:
  Observations of sky emission and absorption in the far infrared (mean
  wavelength 120 μ) and, simultaneously, sky emission at wavelength 6 μ
  have been made by P. Kuhn (ESSA) from the NASA CV-990 aircraft flying
  at 12-km altitude over the middle Pacific at latitudes 10°-15°N. A
  lack of correlation between the near- and far-infrared data, especially
  during times of visible cirrus cloud cover above the aircraft, indicates
  a wavelength-dependent atmospheric phenomenon, which is interpreted as
  scattering. The contributions of scattering by molecules, aerosols,
  water drops, and ice crystals in the upper atmosphere are estimated,
  and it is shown that the latter water drops and ice crystals may account
  for the observed phenomenon. The possible influence of scattering on
  past high-altitude solar observations is briefly discussed.

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Title: Infrared Observations of the Outer Solar Corona
Authors: MacQueen, R. M.
1968ApJ...154.1059M    Altcode:
  Observations of the outer solar corona at wavelength 2.2 ,~ have been
  carried out in two experiments: during the period of totality of the
  solar eclipse of November 12, 1966, with the use of a ground-based
  telescope, and during a stratospheric balloon ifight on January 9,
  1967, by employing a coronagraph. The experiments are discussed, and
  the coronal radiance is presented over the range 3-10 Ro. The presence
  of four features is attributed to thermal emission of interplanetary
  dust. Scans obtained from the balloon experiment over a range of
  position angles show isophotes peaked away from the ecliptic at a
  position which closely coincides with the invariable plane. Attempts
  to assess the origin of the continuum radiance are presented and lead
  to calculations of a scattered infrared F- coronal component and a
  thermal component based upon large-particle cross-sections

---------------------------------------------------------
Title: Infrared Observations of the Outer Solar Corona.
Authors: MacQueen, Robert Moffat
1968PhDT.........2M    Altcode:
  No abstract at ADS

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Title: Infrared Observations of Thermal Radiation From Interplanetary
    Dust at the Eclipse of November 12, 1966 (ABSTRACT)
Authors: Peterson, Alan W.; MacQueen, Robert M.
1967NASSP.150...89P    Altcode:
  No abstract at ADS

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Title: Infrared Observations of the Outer Solar Corona.
Authors: MacQueen, R. M.
1967AJ.....72Q.814M    Altcode:
  The 2.2 p infrared coronal radiance has been measured with a
  ground-based telescope during the total solar eclipse of 12 Xovember
  1966 from 2Re to 6 Re, and during a stratospheric balloon flight of a
  coronagraph, from 3.7 Re to 10 Re. Features superposed on a continuum
  corona at 3.5 Re and 4.0 Re were observed in the former circumstances,
  and features at 4.0 Ro, 8.7 Re, and 9.25 Re noted from the latter
  measurements. Isophotes of the continuum corona obtained from the
  balloon flight data show a peak displaced from the ecliptic, and
  closely coinciding with the invariable plane of the solar system. The
  experiments are discussed, and the observations are presented, and
  compared with a model of thermal emission of circumsolar dust.

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Title: Near Infrared Radiation from the Solar Atmosphere During the
    Total Solar Eclipse of 20 July 1963
Authors: Taylor, J. H.; MacQueen, R. M.
1964ApOpt...3.1506T    Altcode:
  No abstract at ADS