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Author name code: schadee
ADS astronomy entries on 2022-09-14
author:"Schadee, Aert" 

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Title: Book reviews
Authors: Hermsen, W.; Stamm, W.; Nieuwenhuijzen, H.; Plez, B.;
   Koch-Miramond, L.; Schadee, A.; De Greve, J. P.; Icke, Vincent;
   Kresák, Ľ.; Dekker, E.; Bonnet-Bidaud, J. -M.; Foing, B. H.
1994SSRv...67..421H    Altcode:
  No abstract at ADS

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Title: Book Review: The Cambridge guide to astronomical discovery /
    Cambridge U Press, 1992
Authors: Schadee, A.
1994SSRv...67..426S    Altcode: 1994SSRv...67..426L
  No abstract at ADS

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Title: Book-Review - the Astronomy and Astrophysics Encyclopedia
Authors: Maran, S. P.; Schadee, A.
1993SSRv...64..367M    Altcode:
  No abstract at ADS

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Title: Book reviews
Authors: Heintze, J. R. W.; van Genderen, A. M.; van Oss, R.; van
   der Klis, M.; Fárník, F.; Schadee, A.; Sylwester, J.; Torii, S.;
   Iwaniszewska, C.; Nieuwenhuijzen, H.; Kleczek, J.; Schwartz, S. J.
1993SSRv...64..363H    Altcode:
  No abstract at ADS

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Title: Book Review: Space science dictionary I / Academia Praha ;
    Elsevier, 1990
Authors: Schadee, A.
1992SSRv...61R.425S    Altcode:
  No abstract at ADS

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Title: Book Review: Molecular astrophysics / CUP, 1990
Authors: Schadee, A.
1991SSRv...58..191S    Altcode:
  No abstract at ADS

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Title: Book reviews
Authors: Hovenier, J. W.; Cornet, Gerard; De Greve, J. P.; Schadee,
   A.; Kresák, L.; Néeman, Y.
1991SSRv...58..189H    Altcode:
  No abstract at ADS

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Title: Book reviews
Authors: Iwanowska, W.; Sehnal, L.; van der Kruit, P. C.; Schadee,
   A.; Smoliński, J.; Longair, M. S.; Thé, P. S.; McLean, I. S.
1991SSRv...56..241I    Altcode:
  No abstract at ADS

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Title: Book Review: Introduction to stellar astrophysics. Vol. 2:
    Stellar atmospheres / CUP, 1989
Authors: Schadee, A.
1991SSRv...56..245S    Altcode:
  No abstract at ADS

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Title: Book Review: Introduction to stellar astrophysics Volume 1:
    Basic stellar observations and data / CUP, 1989
Authors: Schadee, A.
1990SSRv...54..452S    Altcode: 1990SSRv...54..452B
  No abstract at ADS

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Title: De zon, een overzicht.
Authors: Schadee, A.
1990Zenit..17..306S    Altcode:
  No abstract at ADS

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Title: Book reviews
Authors: Marov, M. Ya; Garmany, C. D.; Heck, André; Schadee, A.;
   McNally, D.; van der Kruit, P. C.; Pecker, J. -C.; de Jager, Cornelis;
   Somov, B. V.
1989SSRv...50..385M    Altcode:
  No abstract at ADS

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Title: Preflare activity.
Authors: Priest, E. R.; Gaizauskas, V.; Hagyard, M. J.; Schmahl, E. J.;
   Webb, D. F.; Cargill, P.; Forbes, T. G.; Hood, A. W.; Steinolfson,
   R. S.; Chapman, G. A.; Deloach, A. C.; Gary, G. A.; Jones, H. P.;
   Karpen, J. T.; Martres, M. -J.; Porter, J. G.; Schmieder, B.; Smith,
   J. B., Jr.; Toomre, J.; Woodgate, B.; Waggett, P.; Bentley, R.;
   Hurford, G.; Schadee, A.; Schrijver, J.; Harrison, R.; Martens, P.
1989epos.conf....1P    Altcode:
  Contents: 1. Introduction. 2. Magnetohydrodynamic
  instability. 3. Preflare magnetic and velocity fields. 4. Coronal
  manifestations of preflare activity.

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Title: High resolution microwave and X-ray observations of solar
    flares
Authors: Alissandrakis, C. E.; Schadee, A.; Kundu, M. R.
1988A&A...195..290A    Altcode:
  This paper presents an analysis of high spatial resolution observations
  of 18 weak flares, carried out during the Solar Maximum Year in the
  microwave range, H-alpha, and soft X-rays, together with observations
  of the associated hard X-ray emission and the photospheric magnetic
  field. This combination of observations made it possible to obtain a
  picture of the flare geometry and the relative position of the various
  emissions, to study the change of the geometry during the flare, to
  estimate the electron temperature and emission measure of the thermal
  plasma, and to compute the contribution of the free-free process in
  the microwave emission. Results are interpreted as evidence for the
  presence of energetic electrons even in the post-burst phase of some
  flares. There was also found a clear case of homologous radio and X-ray
  bursts, one case of foot-point expansion with a relative velocity of
  20 km/s at 6.16 cm, as well as some evidence of triggering of flares
  by disturbances moving with a velocity of 5000-13,000 km/s.

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Title: Coronal manifestations of preflare activity
Authors: Schmahl, E. J.; Webb, D. F.; Woodgate, B.; Waggett, P.;
   Bentley, R.; Hurford, G.; Schadee, A.; Schrijver, J.; Harrison, R.;
   Martens, P.
1986epos.conf.1.48S    Altcode: 1986epos.confA..48S
  A variety of coronal manifestations of precursors or preheating for
  flares are discussed. Researchers found that almost everyone with a
  telescope sees something before flares. Whether an all-encompassing
  scenario will ever be developed is not at all clear at present. The
  clearest example of preflare activity appears to be activated filaments
  and their manifestations, which presumably are signatures of a changing
  magnetic field. But researchers have seen two similar eruptions, one
  without any evidence of emerging flux (Kundu et al., 1985) and the
  other with colliding poles (Simon et al., 1984). While the reconnection
  of flux is generally agreed to be required to energize a flare, the
  emergence of flux from below (at least on short timescales and in
  compact regions) does not appear to be a necessary condition. In some
  cases the cancelling of magnetic flux (Martin, 1984) by horizontal
  motions instead may provide the trigger (Priest, 1985) Researchers
  found similarities and some differences between these and previous
  observations. The similarities, besides the frequent involvement of
  filaments, include compact, multiple precursors which can occur both at
  and near (not at) the flare site, and the association between coronal
  sources and activity lower in the atmosphere (i.e., transition zone
  and chromosphere).

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Title: Book-Review - Molecular Astrophysics
Authors: Diercksen, G. H. F.; Huebner, W. F.; Langhoff, P. W.;
   Schadee, A.
1986SSRv...44..178D    Altcode:
  No abstract at ADS

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Title: Book reviews
Authors: Gurtovenko, E. A.; Kostik, R. I.; Tlamicha, A.; Zerull, R.;
   Schadee, Aert; Mészáros, A.; Néeman, Y.; Giese, R. H.; Sinclair,
   A. T.; Kleczek, J.; Trendelenburg, E. A.; Hillebrandt, Wolfgang;
   Sehnal, L.; de Graaff, W.; Slottje, C.; Courvisier, T.; van Beek,
   H. F.; Baud, B.; de Jager, C.; Danby, J. M. A.; Somov, B. V.;
   Cassinelli, J.; Verbunt, F.
1986SSRv...44..177G    Altcode:
  No abstract at ADS

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Title: Preflare activity.
Authors: Priest, E. R.; Gaizauskas, V.; Hagyard, M. J.; Schmahl, E. J.;
   Webb, D. F.; Cargill, P.; Forbes, T. G.; Hood, A. W.; Steinolfson,
   R. S.; Chapman, G. A.; Deloach, A. C.; Gary, G. A.; Jones, H. P.;
   Karpen, J. T.; Martres, M. -J.; Porter, J. G.; Schmieder, B.; Smith,
   J. B., Jr.; Toomre, J.; Woodgate, B.; Waggett, P.; Bentley, R.;
   Hurford, G.; Schadee, A.; Schrijver, J.; Harrison, R.; Martens, P.
1986NASCP2439....1P    Altcode:
  Contents: 1. Introduction: the preflare state - a review of previous
  results. 2. Magnetohydrodynamic instability: magnetic reconnection,
  nonlinear tearing, nonlinear reconnection experiments, emerging flux and
  moving satellite sunspots, main phase reconnection in two-ribbon flares,
  magnetic instability responsible for filament eruption in two-ribbon
  flares. 3. Preflare magnetic and velocity fields: general morphology of
  the preflare magnetic field, magnetic field shear, electric currents in
  the preflare active region, characterization of the preflare velocity
  field, emerging flux. 4. Coronal manifestations of preflare activity:
  defining the preflare regime, specific illustrative events, comparison
  of preflare X-rays and ultraviolet, preflare microwave intensity and
  polarization changes, non-thermal precursors, precursors of coronal
  mass ejections, short-lived and long-lived HXIS sources as possible
  precursors.

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Title: Survey of an active region in H<SUB>&amp;</SUB>alpha;
    and X-rays.
Authors: Schadee, Aert; Martin, Sara F.
1986lasf.conf..360S    Altcode: 1986lasf.symp..360S
  The authors studied Hale Active Region No. 16918 during almost
  15 hours of simultaneous observation by Big Bear Solar Observatory
  (H<SUB>&amp;</SUB>alpha;) and HXIS (3.5 - 5.5 keV) aboard SMM on 18 -
  22 June 1980.

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Title: On the nature of small X-ray flux over active regions
Authors: Schadee, Aert
1986AdSpR...6f..41S    Altcode: 1986AdSpR...6...41S
  Long-lived weak X-ray flux is often observed in active regions. The
  speculation that this flux is the collective result of a manifold of
  “nanoflares” is investigated. Modelling nanoflares as instantaneously
  energized loops, it is shown that these loops cannot be shorter than
  10 000 km. A modest number of loops with lengths ranging from 10 000
  to 30 000 km and electron densities of (1 - 3) × 10<SUP>11</SUP>
  cm<SUP>-3</SUP> could produce the observed X-ray flux.

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Title: Can nanoflares produce weak X-ray sources?
Authors: Schadee, Aert
1986lasf.conf..356S    Altcode: 1986lasf.symp..356S
  Long-lived weak X-ray flux is often observed in active
  regions. The speculation that this flux is the collective result
  of a manifold of nanoflares is investigated. Modelling nanoflares
  as instantaneously energized loops, it is shown that these loops
  cannot be shorter than 10,000 km. A modest number of loops with
  lengths ranging from 10,000 to 30,000 km and electron densities of
  (1 - 3)×10<SUP>11</SUP>cm<SUP>-3</SUP> could produce the observed
  X-ray flux.

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Title: Identification of two X-ray miniflares with
    H<SUB>α</SUB>-subflares
Authors: Schadee, A.; Gaizauskas, V.
1984AdSpR...4g.117S    Altcode: 1984AdSpR...4..117S
  Active regions show many short-lived emissions in the 3.5 - 5.5
  keV range that are 100 to 1000 times weaker than “normal” X-ray
  flares. The hypothesis that they may well be miniflares is supported
  by the simultaneous occurrence of 2 H<SUB>α</SUB>-subflares at the
  site of weak X-ray sources.

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Title: Relationships of a growing magnetic flux region to flares
Authors: Martin, S. F.; Bentley, R. D.; Schadee, A.; Antalova, A.;
   Kucera, A.; Dezső, L.; Gesztelyi, L.; Harvey, K. L.; Jones, H.;
   Livi, S. H. B.; Wang, J.
1984AdSpR...4g..61M    Altcode: 1984AdSpR...4...61M
  Some sites for solar flares are known to develop where new magnetic
  flux emerges and becomes abutted against opposite polarity pre-existing
  magnetic flux (review by Galzauskas/1/). We have identified and analyzed
  the evolution of such flare sites at the boundaries of a major new and
  growing magnetic flux region within a complex of active regions, Hale
  No. 16918. This analysis was done as a part of a continuing study of the
  circumstances associated with flares in Hale Region 16918, which was
  designated as an FBS target during the interval 18 - 23 June 1980. We
  studied the initiation and development of both major and minor flares in
  Hα images in relation to the identified potential flare sites at the
  boundaries of the growing flux region and to the general development
  of the new flux. This study lead to our recognition of a spectrum of
  possible relationships of growing flux regions to flares as follows:
  (1) intimate interaction with adjacent old flux - flare sites centered
  at new/old flux boundary, (2) forced or “intimidated” interaction
  in which new flux pushes old field having lower flux density towards a
  neighboring old polarity inversion line where a flare then takes place,
  (3) “influential” interaction - magnetic lines of force over an old
  polarity inversion line, typically containing a filament, reconnect to
  the new emerging flux; a flare occurs with erupting filament when the
  magnetic field overlying the filament becomes too weak to prevent its
  eruption, (4) inconsequential interaction - new flux region is too small
  or has wrong orientation for creating flare conditions, (5) incidental -
  flare occurs without any significant relationship to new flux regions.

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Title: Enhanced X-Ray Emission above 3.5-KEV in Active Regions in
    the Absence of Flares
Authors: Schadee, A.; de Jager, C.; Svestka, Z.
1983SoPh...89..287S    Altcode:
  We demonstrate that even in the absence of flares there are very
  often volumes of hot plasma in the corona above active regions with
  temperatures in excess of 10 million degrees. Characteristics of
  this hot plasma and its time variations seem to be different in
  active regions of different phase of development. These hot plasma
  regions are sources of very weak, but clearly recognizable, X-ray
  emission above 3.5 keV. Long-lived X-ray brightenings, 10<SUP>4</SUP>
  times weaker than a flare, but lasting up to 10 hr occur predominantly
  along the H<SUB>∥</SUB> = 0 line, apparently low in the corona. After
  major flares, long-lived X-ray emission is also radiated from tops of
  arches extending high into the corona. Some other long-lived sources,
  far from the H<SUB>∥</SUB> = 0 line, may be associated with newly
  emerging flux. Short-lived X-ray sources, with fluxes ranging from
  subflare levels to 10<SUP>−3</SUP> times the flare flux, last for
  2 to more than 30 min and are probably microflares. They seem to be
  most frequent in growing young active regions and appear often in
  areas with newly emerging flux.

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Title: Radio, X-ray, and optical observations of the flare of June
    13, 1980, at 6<SUP>h</SUP>22<SUP>m</SUP> UT
Authors: Kattenberg, A.; Allaart, M.; de Jager, C.; Schadee, A.;
   Schrijver, J.; Shibasaki, K.; Švestka, Z.; van Tend, W.
1983SoPh...88..315K    Altcode:
  A subflare of importance Sf was observed on June 13, 1980 simultaneously
  by instruments aboard the Solar Maximum Mission (SMM) and various
  ground based observatories. We describe and compare different kinds
  of observations, with emphasis on the Hard X-Ray Imaging Spectrometer
  (HXIS) images and spectra, and on the one-dimensional microwave images
  with high time and spatial resolution, obtained with the Westerbork
  Synthesis Radio Telescope (WSRT). The fast electrons causing the X-ray
  and microwave impulsive bursts had a common acceleration source, but the
  burst were produced at the opposite footpoints of the loops involved,
  with microwaves emitted near to a sunspot penumbra. The flare (of a
  `compact' type) was probably triggered by an emerging flux, and two
  possible interpretations of this process are briefly discussed.

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Title: Pre-Flare and Post-Flare X-Ray Variations in Active Regions
Authors: Svestka, Z.; Schadee, A.
1983SoPh...86..267S    Altcode:
  Extremely low background noise of the HXIS experiment aboard the SMM
  made it possible to detect &gt; 3.5 keV X-ray emissions from non-flaring
  active regions which are 10<SUP>3</SUP>-10<SUP>4</SUP> times weaker than
  the X-ray flux from flares. Short-lived X-ray bursts and long-lived
  X-ray enhancements of various intensities seem to characterize active
  regions in different phases of their development. After major two-ribbon
  flares, giant X-ray arches are seen in the corona, slowly decaying for
  many hours after the flare end. Associated with these arches appear
  to be quasi-periodic flare-like variations of purely coronal nature.

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Title: The Queen's Flare - its Structure and Development - Precursors
    Pre-Flare Brightenings and Aftermaths
Authors: de Jager, Cornelis; Machado, Marcos E.; Schadee, Aert;
   Strong, Keith T.; Švestka, Zdeněk; Woodgate, Bruce E.; van Tend, W.
1983SoPh...84..205D    Altcode:
  We continue previous research on the limb flare of 30 April, 1980, 20:20
  UT, observed in X-rays by several instruments aboard the Solar Maximum
  Mission (SMM). It is shown quantitatively that the flare originated in
  an emerging magnetically confined kernel (diameter ∼ 20″) which
  existed for about ten to fifteen minutes, and from which energetic
  electrons streamed, in at least two injections, into a previously
  existing complicated magnetic loop system thus forming a less bright but
  extended and long-lived tongue. The tongue had a length of ∼ 35 000 km
  and lasted ∼ 90 min in X-rays (∼ 10 keV); at lower energies (∼ 0.7
  keV) it was larger (∼ 80 000 km) and lasted longer. The total number
  of energetic electrons (≈ 10<SUP>37</SUP>) initially present in the
  kernel is of the same order as the number present in the tongue after
  the kernel's decline. This gives evidence that the energetic electrons
  in the tongue originated mainly in the kernel. The electron number
  densities in the kernel and tongue at maximum brightness were ∼ 4.5
  × 10<SUP>11</SUP> and ∼ 1 × 10<SUP>11</SUP> cm<SUP>#X2212;3</SUP>,
  respectively. During the first eight minutes of its existence the tongue
  was hotter than the kernel, but it cooled off gradually. Its decline in
  intensity and temperature was exponential; energy was lost by radiation
  and by conduction through the footpoints of the loop system. These
  footpoints have a cross-section of only ∼ 3 × 10<SUP>6</SUP>
  km<SUP>2</SUP>. This small value, as well as photographs in a CIV UV
  emission line, suggests a highly filamentary structure of the system;
  this is further supported by the finding that the tongue had a `filling
  factor' of ∼ 10<SUP>#X2212;2</SUP>. Several faint X-ray brightenings
  (≲ 0.005 of the flare's maximum intensity) were observed at various
  locations along the solar limb for several hours before and after the
  flare. At ∼ 30 min before the flare's onset a faint (≲ 0.02) flare
  precursor occurred, coinciding in place and shape with the flare. First
  the kernel precursor was brightest but the tongue precursor increased
  continuously in brightness and was the brightest part of the precursor
  some 10-15 min after the first visibility of the kernel precursor,
  until the start of the main flare. This suggests (weak) continuous
  electron acceleration in the tongue during a period of at least 30
  min. The main flare was caused by strong emergence of magnetic field
  followed by two consecutive field line reconnections and accelerations
  in a small loop system, causing footpoint heating. Subsequently plasma
  streamed (convectively) into a pre-existing system of larger loops,
  forming the tongue.

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Title: 3.5 keV X-ray Emission in Absence of Flares
Authors: Schadee, A.; de Jager, C.; Svestka, Z.
1983BAAS...15R.704S    Altcode:
  No abstract at ADS

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Title: The limb flare of 1980 April 30 as seen by the hard X-ray
    imaging spectrometer
Authors: van Beek, H. F.; de Jager, C.; Schadee, A.; Svestka, Z.;
   Boelee, A.; Duijveman, A.; Galama, M.; Hoekstra, R.; Hoyng, P.; Fryer,
   R.; Simnett, G. M.; Imhof, J. P.; LaFleur, H.; Maseland, H. V. A. M.;
   Mels, W. M.; Schrijver, J.; van der Laan, J. J. M.; van Rens, P.; van
   Tend, W.; Werkhoven, F.; Willmore, A. P.; Wilson, J. W. G.; Machado,
   M. E.; Zandee, W.
1981ApJ...244L.157V    Altcode:
  X-ray imaging of the limb event of 1980 April 30 shows that the flaring
  involved two distinct components: a pointlike component, which was the
  source of the initial hard X-ray burst and an extensive tongue reaching
  some 30,000 km above the limb. The tongue had a higher temperature
  than the other parts of the structure and seemed to be enhanced by
  energetic electrons that derived their energy from the initial source.

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Title: Structural development of the X-ray limb flare of 30 April 1980
Authors: de Jager, C.; Hoyng, P.; Lafleur, H.; Schadee, A.; Svestka,
   Z.; van Beek, H. F.; van Tend, W.; Fryer, R.; Simnett, G. M.
1981AdSpR...1m.251D    Altcode: 1981AdSpR...1..251D
  We describe the development of the limb flare of 30 April 1980, 20:20
  UT, as observed by the Hard X-ray Imaging Spectrometer (HXIS) aboard
  the Solar Maximum Mission (SMM). It consisted of a short-lived bright
  nucleus (FWHM &lt; 10,000 km), just inside the Sun's limb; a longer
  lasting tongue, extending to a height of ~ 30,000 km, and a more
  complicated feature, approximately situated at the Sun's limb. The
  tongue was a pre-existing magnetic structure that started emitting
  X-rays only a few seconds after the bright nucleus, and which had a
  slightly higher temperature than the nucleus; its X-ray emission may
  be caused by electrons escaped from the nucleus.

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Title: Solar maximum mission experiment: Early results of the hard
    X-ray imaging experiment
Authors: Boelee, A.; de Jager, C.; Duijveman, A.; Galama, M.; Hoekstra,
   R.; Hoyng, P.; Imhof, J. P.; Lafleur, H.; Maseland, H. V. A. M.; Mels,
   W. A.; Schadee, A.; Schrijver, J.; Svestka, Z.; van Beek, H. F.;
   van Rens, P.; van der Laan, J. J. M.; van Tend, W.; Werkhoven, F.;
   Wiersma, G.; Zandee, W.; Simnett, G. M.; Charlton, C. P.; Fryer, R.;
   Willmore, A. P.; Wilson, J. W. G.; Machado, M. E.
1981AdSpR...1m.255B    Altcode: 1981AdSpR...1R.255B
  We have selected four widely different flares from the early
  period of operations of the Hard X-Ray Imaging Spectrometer (HXIS)
  on SMM to illustrate the characteristic imaging properties of this
  experiment. For the small flare of April 4, 1980, we demonstrate the
  instrument's capability for locating a compact source. In the weak,
  but extensive, flare of April 6 we show how well the instrument can
  display spatial structure, and also the low level of the instrument
  background. In the 1B flare of April 7 we are able to locate positions
  of the X-ray emission in the soft and hard channels, and estimate
  the positional variations of the emission patches. Finally, in the IN
  flare of April 10, which produced the strongest hard X-ray burst we
  have seen so far, we repeat some of the studies made for the April 7
  event, and also demonstrate the capability of the HXIS instrument to
  study the development, with high time resolution, of individual 8”
  × 8” elements of the flare.

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Title: Structural development of the X-ray limb flare of 30 April
    1980.
Authors: de Jager, C.; Fryer, R.; Hoyng, P.; Lafleur, H.; Schadee,
   A.; Simnett, G. M.; Svestka, Z.; van Beek, H. F.; van Tend, W.
1981hea..conf..251D    Altcode:
  No abstract at ADS

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Title: Solar Maximum Mission experiment: early results of the hard
    X-ray imaging experiment.
Authors: Simnett, G. M.; Boelee, A.; Charlton, C. P.; de Jager, C.;
   Duijveman, A.; Fryer, R.; Galama, M.; Hoekstra, R.; Hoyng, P.; Imhof,
   J. P.; Lafleur, H.; Machado, M. E.; Maseland, H. V. A. M.; Mels,
   W. A.; Schadee, A.; Schrijver, J.; Svestka, Z.; van Beek, H. F.;
   van Rens, P.; van der Laan, J. J. M.; van Tend, W.; Werkhoven, F.;
   Wiersma, G.; Willmore, A. P.; Wilson, J. W. G.; Zandee, W.
1981hea..conf..255S    Altcode:
  No abstract at ADS

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Title: Errata: "On the Zeeman effect in electronic transitions of
    diatomic molecules" [J. Quant. Spectrosc. Radiat. Transfer, Vol. 23,
    p. 517 - 531 (1978)].
Authors: Schadee, A.
1980JQSRT..23..533S    Altcode:
  No abstract at ADS

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Title: Unique definitions for the band strength and the
    electronic-vibrational dipole moment of diatomic molecular radiative
    transitions.
Authors: Schadee, A.
1978JQSRT..19..451S    Altcode:
  No abstract at ADS

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Title: On the Zeeman effect in electronic transitions of diatomic
    molecules.
Authors: Schadee, A.
1978JQSRT..19..517S    Altcode:
  No abstract at ADS

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Title: Theory of First Rotational Lines in Transitions of Diatomic
    Molecules
Authors: Schadee, A.
1975A&A....41..203S    Altcode:
  Summary. Correct expressions for the energies of the first rotational
  levels (those with J &lt; A + S) and the H6nl-London factors for
  transitions involving these levels are derived for doublet and triplet
  states and transitions in diatomic molecular spectra. Key words: first
  rotational lines H6nl-London factors - interstellar lines spectroscopy

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Title: Honl-London Factors for 3H-32 and 3L'-~J1 Transitions with
    Intermediate Coupling
Authors: Schadee, A.
1975A&A....41..213S    Altcode:
  Summary. H6nl-London factors of rotational lines for 3H - and -
  3H transitions of diatomic molecules are calculated, allowing for
  non-zero values of both the splitting constant of the state and the
  coupling constant Y of the H state. Key words: H6nl-London factors
  molecular spectro sco py

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Title: Book reviews
Authors: van de Stadt, Herman; Rawer, Karl; Schadee, A.; Noyes, R. W.;
   Bleeker, J. A. M.; Wittenberg, H.; de Graaff, W.; Akasofu, S. -I.;
   Hooykaas, R.; Bappu, M. K. V.; Atanasijević, I.; Icke, Vincent;
   van der Valk, F.; Kresàk, L.; Müller, Edith A.
1975SSRv...17..159V    Altcode:
  No abstract at ADS

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Title: On the Normalization of H6nl-London Factors
Authors: Schadee, A.
1971A&A....14..401S    Altcode:
  A new normalization of -London factors, which govern the intensity
  distribution within a molecular band, is presented. Problems posed
  by previous normalizations are solved. Key worde: -London factors -
  molecular spectroscopy

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Title: An Upper Limit of the Swan Band Intensity in a Sunspot Spectrum
Authors: Schadee, Aert
1970SoPh...15..345S    Altcode:
  There is no evidence for the C<SUB>2</SUB>(0,1) band in an investigated
  sunspot spectrum. Upper limits are given for the band intensity.

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Title: On the oscillator strengths of MgO and F<SUB>2</SUB>.
Authors: Main, R. P.; Schadee, A.
1969JQSRT...9..713M    Altcode:
  No abstract at ADS

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Title: Zirconium Isotope Ratios in the S-Type Star HR 1105
Authors: Schadee, Aert; Davis, Dorothy N.
1968ApJ...152..169S    Altcode:
  The spectrum of the bright non-variable star HR 1105 was studied at
  3 A/mm; it is S type with some features of type M. The wavelengths
  of isotopes of ZrO were computed and used to improve the molecular
  constants by comparison with laboratory measurements. Direct use of
  isotope shifts is not possible. The isotope ratios of zirconium in HR
  1105 were estimated by fitting elaborately computed ZrO profiles to the
  observed spectrum in a limited, supposedly uncon- taminated, region. Two
  sets of isotope ratios which best match the stellar spectrum were found:
  (a) a terrestrial mixture, but with a high abundance of unstable Zr93,
  i.e., Zr93/Zr9° ~ ~, and (b) the ratios Zr91/Zr90, Zr92/Zr90, and
  Zr94/Zr9° larger by a factor of 2 or 3 than the terrestrial ratios,
  with Zr93 at low abundance. The present observations do not permit a
  choice between these two possible isotopic mixtures. An upper limit
  to Zr96 is probably less than 10 per cent of the Zr content. No trace
  of strong lines of ZrO'7 or ZrO'8 was found. Thus Zr isotopes produced
  by the s-process apparently differ, in this star, from the terrestrial
  values, and the supposed production of 018 has probably not occurred

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Title: Molecular Band Intensities in G and K Stars
Authors: Schadee, Aert
1968ApJ...151..239S    Altcode:
  Intensities of CO, CH, C2, and CN bands are studied for G and K stars
  with various surface gravities and metal content, assuming different
  C, N, and 0 compositions. Atmospheric models are based on a scaled,
  solar T(r) relation A simple method predicts the molecular intensities
  accurately, and it is therefore not necessary to work out the equilibria
  of all possible C, N, and 0 compounds in detail. The dependences of
  the computed band intensities on the metal content, Teff, and g are
  discussed and found to be in agreement with the observations. The
  possibilities of determining CNO abundances from ob- served band
  intensities are also discussed. The molecular equilibria are dominated
  by the association of CO, which is complete for stars later than KO. Two
  independent spectral features are required to deter- mine the C and 0
  abundances, like the G-band and an [Oi] line in oxygen-rich giants. In
  oxygen-rich dwarfs, there is oniy one easily observable feature, the
  G-band, which yields a relation between 0 and C. In carbon-rich stars
  the C2 and CH intensities are not independent since each is a function
  of the abun- dance difference between carbon and oxygen. For oxygen-rich
  dwarfs and carbon-rich stars the second datum required to derive 0 and
  C can only be obtained from infrared CO observations. The nitrogen
  abundance may be determined from CN bands for carbon-rich stars, if
  the C - 0 abundance difference is known, and for oxygen-rich stars, if
  both the carbon and the oxygen abundances are known. The division of
  late-type stars into oxygen-rich and carbon-rich is extremely sharp;
  differences of more than 1 per cent from the mathematical equality
  0 = C places a star in either class. All bands of C and N compounds
  are formed near r 0.1 in carbon-rich stars and, except for CO, near
  r 1 or 2 in oxygen-rich stars. Especially in the latter stars, the
  optical depth of formation (r) is a function of the CNO composition,
  and since the carbon depletion is a critical function of both r and
  the CNO composi- tion, an a priori assumption of (r) in determining
  abundances may lead to erroneous results

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Title: Zr isotope ratios in HR 1105.
Authors: Schadee, A.; Davis, D. N.
1967PASP...79..437S    Altcode:
  No abstract at ADS

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Title: Zirconium Isotope Ratios in HR 1105
Authors: Schadee, A.; Davis, D. N.
1967PASP...79Q.437S    Altcode:
  No abstract at ADS

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Title: The Solar Line at λ8668 Å Interpreted as CN
Authors: Schadee, Aert
1967ApJ...147..363S    Altcode:
  No abstract at ADS

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Title: On the Rotational Temperature of a Sunspot
Authors: Schadee, Aert
1966ApJ...145..348S    Altcode:
  No abstract at ADS

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Title: Reduction of Molecular Line Intensities
Authors: Schadee, A.
1966IAUS...26...92S    Altcode:
  No abstract at ADS

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Title: The formation of molecular lines in the solar spectrum (Errata:
    17 537)
Authors: Schadee, A.
1964BAN....17..311S    Altcode:
  No abstract at ADS