Author name code: leroy
ADS astronomy entries on 2022-09-14
=author:"Leroy, B." 
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Title: VizieR Online Data Catalog: MiMeS survey of magnetism in
    massive stars (Wade+, 2016)
Authors: Wade, G. A.; Neiner, C.; Alecian, E.; Grunhut, J. H.; Petit,
   V.; de Batz, B.; Bohlender, D. A.; Cohen, D. H.; Henrichs, H. F.;
   Kochukhov, O.; Landstreet, J. D.; Manset, N.; Martins, F.; Mathis, S.;
   Oksala, M. E.; Owocki, S. P.; Rivinius, T.; Shultz, M. E.; Sundqvist,
   J. O.; Townsend, R. H. D.; Ud-Doula, A.; Bouret, J. -C.; Braithwaite,
   J.; Briquet, M.; Carciofi, A. C.; David-Uraz, A.; Folsom, C. P.;
   Fullerton, A. W.; Leroy, B.; Marcolino, W. L. F.; Moffat, A. F. J.;
   Naze, Y.; St, Louis N.; Auriere, M.; Bagnulo, S.; Bailey, J. D.;
   Barba, R. H.; Blazere, A.; Bohm, T.; Catala, C.; Donati, J. -F.;
   Ferrario, L.; Harrington, D.; Howarth, I. D.; Ignace, R.; Kaper, L.;
   Luftinger, T.; Prinja, R.; Vink, J. S.; Weiss, W. W.; Yakunin, I.
Bibcode: 2016yCat..74560002W
Altcode:
  To initiate the observational component of the MiMeS project,
  the collaboration was awarded a 640 hour Large Program (LP) with
  ESPaDOnS. This award was followed by LP allocations with Narval
  (137 nights, or 1213 hours), and with HARPSpol (30 nights , or 280
  hours). <P />The TC sample (summarized in Table 4) consists of stars
  that were established or suspected to be magnetic at the beginning
  of the project. The majority of these stars are confirmed period ic
  variables with periods ranging from approximately 1 d to 1.5 years,
  with the majority having a period of less than 10 days so that they
  are suitable candidates for observational monitoring and mapping. <P
  />(1 data file).

Title: The magnetic field of the double-lined spectroscopic binary
    system HD 5550
Authors: Alecian, E.; Tkachenko, A.; Neiner, C.; Folsom, C. P.;
   Leroy, B.
Bibcode: 2016A&A...589A..47A
Altcode: 2016arXiv160107762A
  Context. The origin of fossil fields in intermediate- and high-mass
  stars is poorly understood, as is the interplay between binarity and
  magnetism during stellar evolution. Thus we have begun a study of
  the magnetic properties of a sample of intermediate-mass and massive
  short-period binary systems as a function of binarity properties. <BR
  /> Aims: This paper specifically aims to characterise the magnetic
  field of HD 5550, a double-lined spectroscopic binary system of
  intermediate mass. <BR /> Methods: We gathered 25 high-resolution
  spectropolarimetric observations of HD 5550 using the instrument
  Narval. We first fitted the intensity spectra using Zeeman/ATLAS9
  LTE synthetic spectra to estimate the effective temperatures,
  microturbulent velocities, and the abundances of some elements of
  both components, as well as the light ratio of the system. We then
  applied the multi-line least-square deconvolution (LSD) technique to
  the intensity and circularly polarised spectra, which provided us with
  mean LSD I and V line profiles. We fitted the Stokes I line profiles
  to determine the radial and projected rotational velocities of both
  stars. We then analysed the shape and evolution of the V profiles using
  the oblique rotator model to characterise the magnetic fields of both
  stars. <BR /> Results: We confirm the Ap nature of the primary, which
  has previously been reported, and find that the secondary displays
  spectral characteristics typical of an Am star. While a magnetic field
  is clearly detected in the lines of the primary, no magnetic field
  is detected in the secondary in any of our observations. If a dipolar
  field were present at the surface of the Am star, its polar strength
  must be below 40 G. The faint variability observed in the Stokes V
  profiles of the Ap star allowed us to propose a rotation period of
  6.84<SUB>-0.39</SUB><SUP>+0.61</SUP> d, which is close to the orbital
  period (~6.82 d), suggesting that the star is synchronised with its
  orbit. By fitting the variability of the V profiles, we propose that
  the Ap component hosts a dipolar field inclined with the rotation
  axis at an angle β = 156 ± 17 ° and a polar strength B<SUB>d</SUB>
  = 65 ± 20 G. The field strength is the weakest known for an Ap
  star. <P />Based on the BinaMIcS Large Programme (PI: C. Neiner,
  runID: L131N02) obtained at the Telescope Bernard Lyot (USR5026)
  operated by the Observatoire Midi-Pyrénées, Université de Toulouse
  (Paul Sabatier), Centre National de la Recherche Scientifique of France.

Title: Weak magnetic field, solid-envelope rotation, and wave-induced
    N-enrichment in the SPB star ζ Cassiopeiae
Authors: Briquet, M.; Neiner, C.; Petit, P.; Leroy, B.; de Batz, B.
Bibcode: 2016A&A...587A.126B
Altcode: 2016arXiv160104517B
  <BR /> Aims: The main-sequence B-type star ζ Cassiopeiae is known
  as a N-rich star with a magnetic field discovered with the Musicos
  spectropolarimeter. We model the magnetic field of the star by means
  of 82 new spectropolarimetric observations of higher precision to
  investigate the field strength, topology, and effect. <BR /> Methods: We
  gathered data with the Narval spectropolarimeter installed at Télescope
  Bernard Lyot (TBL; Pic du Midi, France) and applied the least-squares
  deconvolution technique to measure the circular polarisation of the
  light emitted from ζ Cas. We used a dipole oblique rotator model to
  determine the field configuration by fitting the longitudinal field
  measurements and by synthesizing the measured Stokes V profiles. We
  also made use of the Zeeman-Doppler imaging technique to map the stellar
  surface and to deduce the difference in rotation rate between the pole
  and equator. <BR /> Results: ζ Cas exhibits a polar field strength
  B<SUB>pol</SUB> of 100-150 G, which is the weakest polar field observed
  so far in a massive main-sequence star. Surface differential rotation is
  ruled out by our observations and the field of ζ Cas is strong enough
  to enforce rigid internal rotation in the radiative zone according to
  theory. Thus, the star rotates as a solid body in the envelope. <BR />
  Conclusions: We therefore exclude rotationally induced mixing as the
  cause of the surface N-enrichment. We discuss that the transport of
  chemicals from the core to the surface by internal gravity waves is
  the most plausible explanation for the nitrogen overabundance at the
  surface of ζ Cas. <P />Based on observations obtained at the Télescope
  Bernard Lyot (USR5026) operated by the Observatoire Midi-Pyrénées,
  Université de Toulouse (Paul Sabatier), Centre National de la Recherche
  Scientifique (CNRS) of France.

Title: The MiMeS survey of magnetism in massive stars: introduction
    and overview
Authors: Wade, G. A.; Neiner, C.; Alecian, E.; Grunhut, J. H.; Petit,
   V.; Batz, B. de; Bohlender, D. A.; Cohen, D. H.; Henrichs, H. F.;
   Kochukhov, O.; Landstreet, J. D.; Manset, N.; Martins, F.; Mathis, S.;
   Oksala, M. E.; Owocki, S. P.; Rivinius, Th.; Shultz, M. E.; Sundqvist,
   J. O.; Townsend, R. H. D.; ud-Doula, A.; Bouret, J. -C.; Braithwaite,
   J.; Briquet, M.; Carciofi, A. C.; David-Uraz, A.; Folsom, C. P.;
   Fullerton, A. W.; Leroy, B.; Marcolino, W. L. F.; Moffat, A. F. J.;
   Nazé, Y.; Louis, N. St; Aurière, M.; Bagnulo, S.; Bailey, J. D.;
   Barbá, R. H.; Blazère, A.; Böhm, T.; Catala, C.; Donati, J. -F.;
   Ferrario, L.; Harrington, D.; Howarth, I. D.; Ignace, R.; Kaper, L.;
   Lüftinger, T.; Prinja, R.; Vink, J. S.; Weiss, W. W.; Yakunin, I.
Bibcode: 2016MNRAS.456....2W
Altcode: 2015arXiv151108425W
  The MiMeS (Magnetism in Massive Stars) project is a large-scale,
  high-resolution, sensitive spectropolarimetric investigation of the
  magnetic properties of O- and early B-type stars. Initiated in 2008 and
  completed in 2013, the project was supported by three Large Program
  allocations, as well as various programmes initiated by independent
  principal investigators, and archival resources. Ultimately, over 4800
  circularly polarized spectra of 560 O and B stars were collected with
  the instruments ESPaDOnS (Echelle SpectroPolarimetric Device for the
  Observation of Stars) at the Canada-France-Hawaii Telescope, Narval
  at the Télescope Bernard Lyot and HARPSpol at the European Southern
  Observatory La Silla 3.6 m telescope, making MiMeS by far the largest
  systematic investigation of massive star magnetism ever undertaken. In
  this paper, the first in a series reporting the general results of the
  survey, we introduce the scientific motivation and goals, describe
  the sample of targets, review the instrumentation and observational
  techniques used, explain the exposure time calculation designed to
  provide sensitivity to surface dipole fields above approximately 100
  G, discuss the polarimetric performance, stability and uncertainty
  of the instrumentation, and summarize the previous and forthcoming
  publications.

Title: Search for magnetic fields in particle-accelerating
    colliding-wind binaries
Authors: Neiner, C.; Grunhut, J.; Leroy, B.; De Becker, M.; Rauw, G.
Bibcode: 2015A&A...575A..66N
Altcode: 2014arXiv1412.5327N
  Context. Some colliding-wind massive binaries, called
  particle-accelerating colliding-wind binaries (PACWB), exhibit
  synchrotron radio emission, which is assumed to be generated by a
  stellar magnetic field. However, no measurement of magnetic fields in
  these stars has ever been performed. <BR /> Aims: We aim at quantifying
  the possible stellar magnetic fields present in PACWB to provide
  constraints for models. <BR /> Methods: We gathered 21 high-resolution
  spectropolarimetric observations of 9 PACWB available in the ESPaDOnS,
  Narval and HarpsPol archives. We analysed these observations with the
  least squares deconvolution method. We separated the binary spectral
  components when possible. <BR /> Results: No magnetic signature is
  detected in any of the 9 PACWB stars and all longitudinal field
  measurements are compatible with 0 G. We derived the upper field
  strength of a possible field that could have remained hidden in
  the noise of the data. While the data are not very constraining
  for some stars, for several stars we could derive an upper limit of
  the polar field strength of the order of 200 G. <BR /> Conclusions:
  We can therefore exclude the presence of strong or moderate stellar
  magnetic fields in PACWB, typical of the ones present in magnetic
  massive stars. Weak magnetic fields could however be present in these
  objects. These observational results provide the first quantitative
  constraints for future models of PACWB. <P />Based on archival
  observations obtained at the Télescope Bernard Lyot (USR5026)
  operated by the Observatoire Midi-Pyrénées, Université de Toulouse
  (Paul Sabatier), Centre National de la Recherche Scientifique (CNRS)
  of France, at the Canada-France-Hawaii Telescope (CFHT) operated by
  the National Research Council of Canada, the Institut National des
  Sciences de l'Univers of the CNRS of France, and the University of
  Hawaii, and at the European Southern Observatory (ESO), Chile.

Title: γ Pegasi: testing Vega-like magnetic fields in B stars
Authors: Neiner, C.; Monin, D.; Leroy, B.; Mathis, S.; Bohlender, D.
Bibcode: 2014A&A...562A..59N
Altcode: 2013arXiv1312.3521N
  Context. The bright B pulsator γ Peg shows both p and g modes of β
  Cep and SPB types. It has also been claimed that it is a magnetic star,
  while others do not detect any magnetic field. <BR /> Aims: We check
  for the presence of a magnetic field, with the aim to characterise it if
  it exists, or else provide a firm upper limit of its strength if it is
  not detected. If γ Peg is magnetic as claimed, it would make an ideal
  asteroseismic target for testing various theoretical scenarios. If
  it is very weakly magnetic, it would be the first observation of
  an extension of Vega-like fields to early B stars. Finally, if it
  is not magnetic and we can provide a very low upper limit on its
  non-detected field, it would make an important result for stellar
  evolution models. <BR /> Methods: We acquired high resolution, high
  signal-to-noise spectropolarimetric Narval data at Telescope Bernard
  Lyot (TBL). We also gathered existing dimaPol spectropolarimetric
  data from the Dominion Astrophysical Observatory (DAO) and Musicos
  spectropolarimetric data from TBL. We analysed the Narval and Musicos
  observations using the least-squares deconvolution (LSD) technique
  to derive the longitudinal magnetic field and Zeeman signatures in
  lines. The longitudinal field strength was also extracted from the Hβ
  line observed with the DAO. With a Monte Carlo simulation we derived the
  maximum strength of the field possibly hosted by γ Peg. <BR /> Results:
  We find that no magnetic signatures are visible in the very high quality
  spectropolarimetric data. The average longitudinal field measured in
  the Narval data is B<SUB>l</SUB> = -0.1 ± 0.4 G. We derive a very
  strict upper limit of the dipolar field strength of B<SUB>pol</SUB> ~
  40 G. <BR /> Conclusions: We conclude that γ Peg is not magnetic: it
  hosts neither a strong stable fossil field as observed in a fraction
  of massive stars nor a very weak Vega-like field. There is therefore
  no evidence that Vega-like fields exist in B stars, contrary to the
  predictions by fossil field dichotomy scenarios. These scenarios should
  thus be revised. Our results also provide strong constraints for stellar
  evolution models. <P />Based on observations obtained at the Telescope
  Bernard Lyot (USR5026) operated by the Observatoire Midi-Pyrénées,
  Université de Toulouse (Paul Sabatier), Centre National de la
  Recherche Scientifique of France, and at the Dominion Astrophysical
  Observatory.Tables 1-3 are available in electronic form at <A
  href="http://www.aanda.org/10.1051/0004-6361/201323093/olm">http://www.aanda.org</A>

Title: Discovery of a magnetic field in the CoRoT hybrid B-type
    pulsator HD 43317
Authors: Briquet, M.; Neiner, C.; Leroy, B.; Pápics, P. I.; MiMeS
   Collaboration
Bibcode: 2013A&A...557L..16B
Altcode: 2013arXiv1308.4636B
  Context. A promising way of testing the impact of a magnetic field on
  internal mixing (core overshooting, internal rotation) in main-sequence
  B-type stars is to perform asteroseismic studies of a sample of magnetic
  pulsators. <BR /> Aims: The CoRoT satellite revealed that the B3IV
  star HD 43317 is a hybrid SPB/β Cep-type pulsator that has a wealth of
  pulsational constraints on which one can perform a seismic modelling,
  in particular, probing the extent of its convective core and mixing
  processes. Moreover, indirect indicators of a magnetic field in the star
  were observed: rotational modulation due to chemical or temperature
  spots and X-ray emission. Our goal was to directly investigate the
  field in HD 43317 and, if it is magnetic, to characterise it. <BR
  /> Methods: We collected data with the Narval spectropolarimeter
  installed at Télescope Bernard Lyot (TBL, Pic du Midi, France)
  and applied the least-squares deconvolution technique to measure the
  circular polarisation of the light emitted from HD 43317. We modelled
  the longitudinal field measurements directly with a dipole. <BR />
  Results: Zeeman signatures in the Stokes V profiles of HD 43317 are
  clearly detected and rotationally modulated, which proves that this star
  exhibits an oblique magnetic field. The modulation with the rotation
  period deduced from the CoRoT light curve is also confirmed, and we
  found a field strength at the poles of about 1 kG. Our result must be
  taken into account in future seismic modelling work of this star. <P
  />Based on observations obtained using the Narval spectropolarimeter
  at the Observatoire du Pic du Midi (France), which is operated by the
  Institut National des Sciences de l'Univers (INSU).

Title: Stochastic gravito-inertial modes discovered by CoRoT in the
    hot Be star HD 51452
Authors: Neiner, C.; Floquet, M.; Samadi, R.; Espinosa Lara, F.;
   Frémat, Y.; Mathis, S.; Leroy, B.; de Batz, B.; Rainer, M.; Poretti,
   E.; Mathias, P.; Guarro Fló, J.; Buil, C.; Ribeiro, J.; Alecian,
   E.; Andrade, L.; Briquet, M.; Diago, P. D.; Emilio, M.; Fabregat,
   J.; Gutiérrez-Soto, J.; Hubert, A. -M.; Janot-Pacheco, E.; Martayan,
   C.; Semaan, T.; Suso, J.; Zorec, J.
Bibcode: 2012A&A...546A..47N
Altcode:
  Context. Be stars are rapidly rotating stars with a circumstellar
  decretion disk. They usually undergo pressure and/or gravity pulsation
  modes excited by the κ-mechanism, i.e. an effect of the opacity of
  iron-peak elements in the envelope of the star. In the Milky Way,
  p-modes are observed in stars that are hotter than or equal to the
  B3 spectral type, while g-modes are observed at the B2 spectral
  type and cooler. <BR /> Aims: We observed a B0IVe star, HD 51452,
  with the high-precision, high-cadence photometric CoRoT satellite
  and high-resolution, ground-based HARPS and SOPHIE spectrographs to
  study its pulsations in great detail. We also used the lower resolution
  spectra available in the BeSS database. <BR /> Methods: We analyzed the
  CoRoT and spectroscopic data with several methods: Clean-NG, FreqFind,
  and a sliding window method. We also analyzed spectral quantities,
  such as the violet over red (V/R) emission variations, to obtain
  information about the variation in the circumstellar environment. We
  calculated a stellar structure model with the ESTER code to test
  the various interpretation of the results. <BR /> Results: We detect
  189 frequencies of variations in the CoRoT light curve in the range
  between 0 and 4.5 c d<SUP>-1</SUP>. The main frequencies are also
  recovered in the spectroscopic data. In particular we find that HD
  51452 undergoes gravito-inertial modes that are not in the domain of
  those excited by the κ-mechanism. We propose that these are stochastic
  modes excited in the convective zones and that at least some of them
  are a multiplet of r-modes (i.e. subinertial modes mainly driven by
  the Coriolis acceleration). Stochastically excited gravito-inertial
  modes had never been observed in any star, and theory predicted that
  their very low amplitudes would be undetectable even with CoRoT. We
  suggest that the amplitudes are enhanced in HD 51452 because of the
  very rapid stellar rotation. In addition, we find that the amplitude
  variations of these modes are related to the occurrence of minor
  outbursts. <BR /> Conclusions: Thanks to CoRoT data, we have detected
  a new kind of pulsations in HD 51452, which are stochastically excited
  gravito-inertial modes, probably due to its very rapid rotation. These
  modes are probably also present in other rapidly rotating hot Be
  stars. <P />The CoRoT space mission, launched on December 27, 2006,
  has been developed and is operated by CNES, with the contribution of
  Austria, Belgium, Brazil, ESA (RSSD, and Science Programs), Germany,
  and Spain. This work uses observations partly made with the HARPS
  instrument at the 3.6-m ESO telescope (La Silla, Chile) in the framework
  of the LP182.D-0356, as well as data obtained with Sophie at OHP and
  from the BeSS database.Table 3 is available in electronic form at <A
  href="http://www.aanda.org">http://www.aanda.org</A>

Title: Fast calculation of the Lomb-Scargle periodogram using
    nonequispaced fast Fourier transforms
Authors: Leroy, B.
Bibcode: 2012A&A...545A..50L
Altcode:
  We present a code for the fast computation of the Lomb-Scargle
  periodogram that uses nonequispaced fast Fourier transforms (FFTs). The
  computation time has the classical O(Nlog N) behaviour of FFTs,
  but is shorter by about one order of magnitude than the "classical"
  fast algorithm by Press and Rybicki, and is about five times shorter
  that the best GPU-based implementations of the usual O(N<SUP>2</SUP>)
  algorithm. This performance is achieved without sacrificing accuracy,
  as revealed by comparing the computations done with our FFT-based
  algorithm and a naïve one.

Title: The Kepler characterization of the variability among A-
    and F-type stars. I. General overview
Authors: Uytterhoeven, K.; Moya, A.; Grigahcène, A.; Guzik,
   J. A.; Gutiérrez-Soto, J.; Smalley, B.; Handler, G.; Balona,
   L. A.; Niemczura, E.; Fox Machado, L.; Benatti, S.; Chapellier, E.;
   Tkachenko, A.; Szabó, R.; Suárez, J. C.; Ripepi, V.; Pascual, J.;
   Mathias, P.; Martín-Ruíz, S.; Lehmann, H.; Jackiewicz, J.; Hekker,
   S.; Gruberbauer, M.; García, R. A.; Dumusque, X.; Díaz-Fraile, D.;
   Bradley, P.; Antoci, V.; Roth, M.; Leroy, B.; Murphy, S. J.; De Cat,
   P.; Cuypers, J.; Kjeldsen, H.; Christensen-Dalsgaard, J.; Breger, M.;
   Pigulski, A.; Kiss, L. L.; Still, M.; Thompson, S. E.; van Cleve, J.
Bibcode: 2011A&A...534A.125U
Altcode: 2011arXiv1107.0335U
  Context. The Kepler spacecraft is providing time series of photometric
  data with micromagnitude precision for hundreds of A-F type stars. <BR
  /> Aims: We present a first general characterization of the pulsational
  behaviour of A-F type stars as observed in the Kepler light curves
  of a sample of 750 candidate A-F type stars, and observationally
  investigate the relation between γ Doradus (γ Dor), δ Scuti
  (δ Sct), and hybrid stars. <BR /> Methods: We compile a database
  of physical parameters for the sample stars from the literature and
  new ground-based observations. We analyse the Kepler light curve of
  each star and extract the pulsational frequencies using different
  frequency analysis methods. We construct two new observables, "energy"
  and "efficiency", related to the driving energy of the pulsation
  mode and the convective efficiency of the outer convective zone,
  respectively. <BR /> Results: We propose three main groups to describe
  the observed variety in pulsating A-F type stars: γ Dor, δ Sct, and
  hybrid stars. We assign 63% of our sample to one of the three groups,
  and identify the remaining part as rotationally modulated/active stars,
  binaries, stars of different spectral type, or stars that show no clear
  periodic variability. 23% of the stars (171 stars) are hybrid stars,
  which is a much higher fraction than what has been observed before. We
  characterize for the first time a large number of A-F type stars (475
  stars) in terms of number of detected frequencies, frequency range,
  and typical pulsation amplitudes. The majority of hybrid stars show
  frequencies with all kinds of periodicities within the γ Dor and δ
  Sct range, also between 5 and 10 d<SUP>-1</SUP>, which is a challenge
  for the current models. We find indications for the existence of δ
  Sct and γ Dor stars beyond the edges of the current observational
  instability strips. The hybrid stars occupy the entire region within
  the δ Sct and γ Dor instability strips and beyond. Non-variable
  stars seem to exist within the instability strips. The location of
  γ Dor and δ Sct classes in the (T<SUB>eff</SUB>, log g)-diagram
  has been extended. We investigate two newly constructed variables,
  "efficiency" and "energy", as a means to explore the relation between
  γ Dor and δ Sct stars. <BR /> Conclusions: Our results suggest a
  revision of the current observational instability strips of δ Sct and
  γ Dor stars and imply an investigation of pulsation mechanisms to
  supplement the κ mechanism and convective blocking effect to drive
  hybrid pulsations. Accurate physical parameters for all stars are
  needed to confirm these findings.

Title: VizieR Online Data Catalog: Variability of A- and F-stars
    from Kepler (Uytterhoeven+ 2011)
Authors: Uytterhoeven, K.; Moya, A.; Grigahcene, A.; Guzik, J. A.;
   Gutierrez-Soto, J.; Smalley, B.; Handler, G.; Balona, L. A.; Niemczura,
   E.; Fox Machado, L.; Benatti, S.; Chapellier, E.; Tkachenko, A.; Szabo,
   R.; Suarez, J. C.; Ripepi, V.; Pascual, J.; Mathias, P.; Martin-Ruiz,
   S.; Lehmann, H.; Jackiewicz, J.; Hekker, S.; Gruberbauer, M.; Garcia,
   R. A.; Dumusque, X.; Diaz-Fraile, D.; Bradley, P.; Antoci, V.; Roth,
   M.; Leroy, B.; Murphy, S. J.; De Cat, P.; Cuypers, J.; Kjeldsen, H.;
   Christensen-Dalsgaard, J.; Breger, M.; Pigulski, A.; Kiss, L. L.;
   Still, M.; Thompson, S. E.; van Cleve, J.
Bibcode: 2011yCat..35340125U
Altcode: 2011yCat..35349125U
  We compile a database of physical parameters for the sample stars from
  the literature and new ground-based observations. We analyse the Kepler
  light curve of each star and extract the pulsational frequencies using
  different frequency analysis methods. We construct two new observables,
  'energy' and 'efficiency', related to the driving energy of the
  pulsation mode and the convective efficiency of the outer convective
  zone, respectively. <P />(5 data files).

Title: Kepler observations of the variability in B-type stars
Authors: Balona, L. A.; Pigulski, A.; De Cat, P.; Handler, G.;
   Gutiérrez-Soto, J.; Engelbrecht, C. A.; Frescura, F.; Briquet, M.;
   Cuypers, J.; Daszyńska-Daszkiewicz, J.; Degroote, P.; Dukes, R. J.;
   Garcia, R. A.; Green, E. M.; Heber, U.; Kawaler, S. D.; Lehmann,
   H.; Leroy, B.; Molenda-Żaaowicz, J.; Neiner, C.; Noels, A.; Nuspl,
   J.; Østensen, R.; Pricopi, D.; Roxburgh, I.; Salmon, S.; Smith,
   M. A.; Suárez, J. C.; Suran, M.; Szabó, R.; Uytterhoeven, K.;
   Christensen-Dalsgaard, J.; Kjeldsen, H.; Caldwell, D. A.; Girouard,
   F. R.; Sanderfer, D. T.
Bibcode: 2011MNRAS.413.2403B
Altcode: 2011MNRAS.tmp..298B; 2011arXiv1103.0644B
  The analysis of the light curves of 48 B-type stars observed by Kepler
  is presented. Among these are 15 pulsating stars, all of which show low
  frequencies, characteristic of slowly pulsating B (SPB) stars. Seven of
  these stars also show a few weak, isolated high frequencies and they
  could be considered as SPB/β Cephei (β Cep) hybrids. In all cases,
  the frequency spectra are quite different from what is seen from
  ground-based observations. We suggest that this is because most of
  the low frequencies are modes of high degree which are predicted to be
  unstable in models of mid-B stars. We find that there are non-pulsating
  stars within the β Cep and SPB instability strips. Apart from the
  pulsating stars, we can identify stars with frequency groupings similar
  to what is seen in Be stars but which are not Be stars. The origin of
  the groupings is not clear, but may be related to rotation. We find
  periodic variations in other stars which we attribute to proximity
  effects in binary systems or possibly rotational modulation. We find
  no evidence for pulsating stars between the cool edge of the SPB
  and the hot edge of the δ Sct instability strips. None of the stars
  shows the broad features which can be attributed to stochastically
  excited modes as recently proposed. Among our sample of B stars are
  two chemically peculiar stars, one of which is a HgMn star showing
  rotational modulation in the light curve.

Title: Asteroseismology of solar-type stars with Kepler I: Data
    analysis
Authors: Karoff, C.; Chaplin, W. J.; Appourchaux, T.; Elsworth, Y.;
   Garcia, R. A.; Houdek, G.; Metcalfe, T. S.; Molenda-Żakowicz, J.;
   Monteiro, M. J. P. F. G.; Thompson, M. J.; Christensen-Dalsgaard, J.;
   Gilliland, R. L.; Kjeldsen, H.; Basu, S.; Bedding, T. R.; Campante,
   T. L.; Eggenberger, P.; Fletcher, S. T.; Gaulme, P.; Handberg, R.;
   Hekker, S.; Martic, M.; Mathur, S.; Mosser, B.; Regulo, C.; Roxburgh,
   I. W.; Salabert, D.; Stello, D.; Verner, G. A.; Belkacem, K.; Biazzo,
   K.; Cunha, M. S.; Gruberbauer, M.; Guzik, J. A.; Kupka, F.; Leroy,
   B.; Ludwig, H. -G.; Mathis, S.; Noels, A.; Noyes, R. W.; Roca Cortes,
   T.; Roth, M.; Sato, K. H.; Schmitt, J.; Suran, M. D.; Trampedach,
   R.; Uytterhoeven, K.; Ventura, R.
Bibcode: 2010AN....331..972K
Altcode: 2010arXiv1005.0507K
  We report on the first asteroseismic analysis of solar-type stars
  observed by Kepler. Observations of three G-type stars, made at
  one-minute cadence during the first 33.5 days of science operations,
  reveal high signal-to-noise solar-like oscillation spectra in all three
  stars: About 20 modes of oscillation can clearly be distinguished
  in each star. We discuss the appearance of the oscillation spectra,
  including the presence of a possible signature of faculae, and the
  presence of mixed modes in one of the three stars.

Title: Photometric variability of the Be star CoRoT-ID 102761769
Authors: Emilio, M.; Andrade, L.; Janot-Pacheco, E.; Baglin, A.;
   Gutiérrez-Soto, J.; Suárez, J. C.; de Batz, B.; Diago, P.; Fabregat,
   J.; Floquet, M.; Frémat, Y.; Huat, A. L.; Hubert, A. M.; Espinosa
   Lara, F.; Leroy, B.; Martayan, C.; Neiner, C.; Semaan, T.; Suso, J.
Bibcode: 2010A&A...522A..43E
Altcode: 2010arXiv1010.5576E
  Context. Classical Be stars are rapid rotators of spectral type
  late O to early A and luminosity class V-III, which exhibit Balmer
  emission lines and often a near infrared excess originating in an
  equatorially concentrated circumstellar envelope, both produced by
  sporadic mass ejection episodes. The causes of the abnormal mass
  loss (the so-called Be phenomenon) are as yet unknown. <BR /> Aims:
  For the first time, we can now study in detail Be stars outside the
  Earth's atmosphere with sufficient temporal resolution. We investigate
  the variability of the Be Star CoRoT-ID 102761769 observed with the
  CoRoT satellite in the exoplanet field during the initial run. <BR />
  Methods: One low-resolution spectrum of the star was obtained with
  the INT telescope at the Observatorio del Roque de los Muchachos. A
  time series analysis was performed using both cleanest and singular
  spectrum analysis algorithms to the CoRoT light curve. To identify
  the pulsation modes of the observed frequencies, we computed a
  set of models representative of CoRoT-ID 102761769 by varying its
  main physical parameters inside the uncertainties discussed. <BR />
  Results: We found two close frequencies related to the star. They
  are 2.465 c d<SUP>-1</SUP> (28.5 μHz) and 2.441 c d<SUP>-1</SUP>
  (28.2 μHz). The precision to which those frequencies were found is
  0.018 c d<SUP>-1</SUP> (0.2 μHz). The projected stellar rotation was
  estimated to be 120 km s<SUP>-1</SUP> from the Fourier transform of
  spectral lines. If CoRoT-ID 102761769 is a typical Galactic Be star it
  rotates near the critical velocity. The critical rotation frequency
  of a typical B5-6 star is about 3.5 c d<SUP>-1</SUP> (40.5 μHz),
  which implies that the above frequencies are really caused by stellar
  pulsations rather than star's rotation. <P />The CoRoT space mission
  was developed and is operated by the French space agency CNES, with
  participation of ESA's RSSD and Science Programmes, Austria, Belgium,
  Brazil, Germany, and Spain.

Title: The Asteroseismic Potential of Kepler: First Results for
    Solar-Type Stars
Authors: Chaplin, W. J.; Appourchaux, T.; Elsworth, Y.; García,
   R. A.; Houdek, G.; Karoff, C.; Metcalfe, T. S.; Molenda-Żakowicz,
   J.; Monteiro, M. J. P. F. G.; Thompson, M. J.; Brown, T. M.;
   Christensen-Dalsgaard, J.; Gilliland, R. L.; Kjeldsen, H.; Borucki,
   W. J.; Koch, D.; Jenkins, J. M.; Ballot, J.; Basu, S.; Bazot, M.;
   Bedding, T. R.; Benomar, O.; Bonanno, A.; Brandão, I. M.; Bruntt,
   H.; Campante, T. L.; Creevey, O. L.; Di Mauro, M. P.; Doǧan,
   G.; Dreizler, S.; Eggenberger, P.; Esch, L.; Fletcher, S. T.;
   Frandsen, S.; Gai, N.; Gaulme, P.; Handberg, R.; Hekker, S.; Howe,
   R.; Huber, D.; Korzennik, S. G.; Lebrun, J. C.; Leccia, S.; Martic,
   M.; Mathur, S.; Mosser, B.; New, R.; Quirion, P. -O.; Régulo, C.;
   Roxburgh, I. W.; Salabert, D.; Schou, J.; Sousa, S. G.; Stello, D.;
   Verner, G. A.; Arentoft, T.; Barban, C.; Belkacem, K.; Benatti, S.;
   Biazzo, K.; Boumier, P.; Bradley, P. A.; Broomhall, A. -M.; Buzasi,
   D. L.; Claudi, R. U.; Cunha, M. S.; D'Antona, F.; Deheuvels, S.;
   Derekas, A.; García Hernández, A.; Giampapa, M. S.; Goupil, M. J.;
   Gruberbauer, M.; Guzik, J. A.; Hale, S. J.; Ireland, M. J.; Kiss,
   L. L.; Kitiashvili, I. N.; Kolenberg, K.; Korhonen, H.; Kosovichev,
   A. G.; Kupka, F.; Lebreton, Y.; Leroy, B.; Ludwig, H. -G.; Mathis, S.;
   Michel, E.; Miglio, A.; Montalbán, J.; Moya, A.; Noels, A.; Noyes,
   R. W.; Pallé, P. L.; Piau, L.; Preston, H. L.; Roca Cortés, T.;
   Roth, M.; Sato, K. H.; Schmitt, J.; Serenelli, A. M.; Silva Aguirre,
   V.; Stevens, I. R.; Suárez, J. C.; Suran, M. D.; Trampedach, R.;
   Turck-Chièze, S.; Uytterhoeven, K.; Ventura, R.; Wilson, P. A.
Bibcode: 2010ApJ...713L.169C
Altcode: 2010arXiv1001.0506C
  We present preliminary asteroseismic results from Kepler on three G-type
  stars. The observations, made at one-minute cadence during the first
  33.5 days of science operations, reveal high signal-to-noise solar-like
  oscillation spectra in all three stars: about 20 modes of oscillation
  may be clearly distinguished in each star. We discuss the appearance of
  the oscillation spectra, use the frequencies and frequency separations
  to provide first results on the radii, masses, and ages of the stars,
  and comment in the light of these results on prospects for inference
  on other solar-type stars that Kepler will observe.

Title: The B0.5 IVe CoRoT target HD 49330. II. Spectroscopic
    ground-based observations
Authors: Floquet, M.; Hubert, A. -M.; Huat, A. -L.; Frémat, Y.;
   Janot-Pacheco, E.; Gutiérrez-Soto, J.; Neiner, C.; de Batz, B.;
   Leroy, B.; Poretti, E.; Amado, P.; Catala, C.; Rainer, M.; Diaz, D.;
   Uytterhoeven, K.; Andrade, L.; Diago, P. D.; Emilio, M.; Espinosa Lara,
   F.; Fabregat, J.; Martayan, C.; Semaan, T.; Suso, J.
Bibcode: 2009A&A...506..103F
Altcode:
  Context: We present spectroscopic ground-based observations of the early
  Be star HD 49330 obtained simultaneously with the CoRoT-LRA1 run just
  before the burst observed in the CoRoT data. <BR />Aims: Ground-based
  spectroscopic observations of the early Be star HD 49330 obtained
  during the precursor phase and just before the start of an outburst
  allow us to disantangle stellar and circumstellar contributions and
  identify modes of stellar pulsations in this rapidly rotating star. <BR
  />Methods: Time series analysis (TSA) is performed on photospheric line
  profiles of He I and Si III by means of the least squares method. <BR
  />Results: We find two main frequencies f1 = 11.86 c d<SUP>-1</SUP>
  and f2 = 16.89 c d<SUP>-1</SUP> which can be associated with high order
  p-mode pulsations. We also detect a frequency f3 = 1.51 c d<SUP>-1</SUP>
  which can be associated with a low order g-mode. Moreover we show that
  the stellar line profile variability changed over the spectroscopic
  run. These results are in agreement with the results of the CoRoT
  data analysis, as shown in Huat et al. (2009). <BR />Conclusions:
  Our study of mid- and short-term spectroscopic variability allows the
  identification of p- and g-modes in HD 49330. It also allows us to
  display changes in the line profile variability before the start of
  an outburst. This brings new constraints for the seimic modelling of
  this star. <P />Based on observations made with ESO Telescopes at La
  Silla Observatory under the ESO Large Programme: LP178.D-0361, and on
  data collected with the TBL at Pic du Midi Observatory (France).

Title: The B0.5IVe CoRoT target HD 49330. I. Photometric analysis
    from CoRoT data
Authors: Huat, A. -L.; Hubert, A. -M.; Baudin, F.; Floquet, M.; Neiner,
   C.; Frémat, Y.; Gutiérrez-Soto, J.; Andrade, L.; de Batz, B.; Diago,
   P. D.; Emilio, M.; Espinosa Lara, F.; Fabregat, J.; Janot-Pacheco,
   E.; Leroy, B.; Martayan, C.; Semaan, T.; Suso, J.; Auvergne, M.;
   Catala, C.; Michel, E.; Samadi, R.
Bibcode: 2009A&A...506...95H
Altcode:
  Context: Be stars undergo outbursts producing a circumstellar disk
  from the ejected material. The beating of non-radial pulsations has
  been put forward as a possible mechanism of ejection. <BR />Aims:
  We analyze the pulsational behavior of the early B0.5IVe star HD
  49330 observed during the first CoRoT long run towards the Galactical
  anticenter (LRA1). This Be star is located close to the lower edge of
  the β Cephei instability strip in the HR diagram and showed a 0.03
  mag outburst during the CoRoT observations. It is thus an ideal case
  for testing the aforementioned hypothesis. <BR />Methods: We analyze
  the CoRoT light curve of HD 49330 using Fourier methods and non-linear
  least square fitting. <BR />Results: In this star, we find pulsation
  modes typical of β Cep stars (p modes) and SPB stars (g modes)
  with amplitude variations along the run directly correlated with the
  outburst. These results provide new clues about the origin of the Be
  phenomenon as well as strong constraints on the seismic modelling of
  Be stars. <P />Tables 3 to 7 are only available in electronic form
  at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5)
  or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/506/95

Title: Low-amplitude variations detected by CoRoT in the B8IIIe
    star HD 175869
Authors: Gutiérrez-Soto, J.; Floquet, M.; Samadi, R.; Neiner, C.;
   Garrido, R.; Fabregat, J.; Frémat, Y.; Diago, P. D.; Huat, A. -L.;
   Leroy, B.; Emilio, M.; Hubert, A. -M.; Andrade, O. Thizy L.; de Batz,
   B.; Janot-Pacheco, E.; Espinosa Lara, F.; Martayan, C.; Semaan, T.;
   Suso, J.; Auvergne, M.; Chaintreuil, S.; Michel, E.; Catala, C.
Bibcode: 2009A&A...506..133G
Altcode:
  Context: The origin of the short-term variability in Be stars remains
  a matter of controversy. Pulsations and rotational modulation are
  the components of the favored hypothesis. <BR />Aims: We present our
  analysis of CoRoT data of the B8IIIe star HD 175869 observed during
  the first short run in the center direction (SRC1). <BR />Methods:
  We review both the instrumental effects visible in the CoRoT light
  curve and the analysis methods used by the CoRoT Be team. We applied
  these methods to the CoRoT light curve of the star HD 175869. A
  search for line-profile variations in the spectroscopic data was also
  performed. We also searched for a magnetic field, by applying the LSD
  technique to spectropolarimetric data. <BR />Results: The light curve
  exhibits low-amplitude variations of the order of 300 μmag with a
  double wave shape. A frequency within the range determined for the
  rotational frequency and 6 of its harmonics are detected. The main
  frequency and its first harmonic exhibit amplitude variations of a few
  days. Other significant frequencies of low-amplitude from 25 to a few
  μmag are also found. The analysis of line profiles from ground-based
  spectroscopic data does not detect any variation. In addition, no
  Zeeman signature was found. <BR />Conclusions: Inhomogeneities caused
  by stellar activity in or just above the photosphere are proposed to
  produce the photometric variability detected by CoRoT in the Be star
  HD 175869. The hypothesis that non-radial pulsations are the origin
  of these variations cannot be excluded.

Title: Pulsations in the late-type Be star HD 50 209 detected by CoRoT
Authors: Diago, P. D.; Gutiérrez-Soto, J.; Auvergne, M.; Fabregat, J.;
   Hubert, A. -M.; Floquet, M.; Frémat, Y.; Garrido, R.; Andrade, L.; de
   Batz, B.; Emilio, M.; Espinosa Lara, F.; Huat, A. -L.; Janot-Pacheco,
   E.; Leroy, B.; Martayan, C.; Neiner, C.; Semaan, T.; Suso, J.; Catala,
   C.; Poretti, E.; Rainer, M.; Uytterhoeven, K.; Michel, E.; Samadi, R.
Bibcode: 2009A&A...506..125D
Altcode: 2009arXiv0909.4524D
  Context: The presence of pulsations in late-type Be stars is still a
  matter of controversy. It constitutes an important issue to establish
  the relationship between non-radial pulsations and the mass-loss
  mechanism in Be stars. <BR />Aims: To contribute to this discussion,
  we analyse the photometric time series of the B8IVe star HD 50 209
  observed by the CoRoT mission in the seismology field. <BR />Methods:
  We use standard Fourier techniques and linear and non-linear least
  squares fitting methods to analyse the CoRoT light curve. In addition,
  we applied detailed modelling of high-resolution spectra to obtain
  the fundamental physical parameters of the star. <BR />Results: We
  have found four frequencies which correspond to gravity modes with
  azimuthal order m=0,-1,-2,-3 with the same pulsational frequency in the
  co-rotating frame. We also found a rotational period with a frequency
  of 0.679 cd<SUP>-1</SUP> (7.754 μHz). <BR />Conclusions: HD 50 209 is
  a pulsating Be star as expected from its position in the HR diagram,
  close to the SPB instability strip. <P />Based on observations made
  with the CoRoT satellite, with FEROS at the 2.2 m telescope of the
  La Silla Observatory under the ESO Large Programme LP178.D-0361
  and with Narval at the Télescope Bernard Lyot of the Pic du Midi
  Observatory. Current address: Valencian International University (VIU),
  José Pradas Gallen s/n, 12006 Castellón, Spain. Current address:
  Laboratoire AIM, CEA/DSM-CNRS-Université Paris Diderot; CEA, IRFU,
  SAp, centre de Saclay, 91191 Gif-sur-Yvette, France.

Title: The pulsations of the B5IVe star HD 181231 observed with
    CoRoT and ground-based spectroscopy
Authors: Neiner, C.; Gutiérrez-Soto, J.; Baudin, F.; de Batz, B.;
   Frémat, Y.; Huat, A. L.; Floquet, M.; Hubert, A. -M.; Leroy, B.;
   Diago, P. D.; Poretti, E.; Carrier, F.; Rainer, M.; Catala, C.; Thizy,
   O.; Buil, C.; Ribeiro, J.; Andrade, L.; Emilio, M.; Espinosa Lara,
   F.; Fabregat, J.; Janot-Pacheco, E.; Martayan, C.; Semaan, T.; Suso,
   J.; Baglin, A.; Michel, E.; Samadi, R.
Bibcode: 2009A&A...506..143N
Altcode:
  Context: <ASTROBJ>H</ASTROBJ>D 181231 is a B5IVe star, which has
  been observed with the CoRoT satellite during ~5 consecutive
  months and simultaneously from the ground in spectroscopy and
  spectropolarimetry. <BR />Aims: By analysing these data, we aim to
  detect and characterize as many pulsation frequencies as possible, to
  search for the presence of beating effects possibly at the origin of
  the Be phenomenon. Our results will also provide a basis for seismic
  modelling. <BR />Methods: The fundamental parameters of the star are
  determined from spectral fitting and from the study of the circumstellar
  emission. The CoRoT photometric data and ground-based spectroscopy are
  analysed using several Fourier techniques: Clean-ng, Pasper, and Tisaft,
  as well as a time-frequency technique. A search for a magnetic field
  is performed by applying the LSD technique to the spectropolarimetric
  data. <BR />Results: We find that <ASTROBJ>H</ASTROBJ>D 181231 is
  a B5IVe star seen with an inclination of ~45 degrees. No magnetic
  field is detected in its photosphere. We detect at least 10 independent
  significant frequencies of variations among the 54 detected frequencies,
  interpreted in terms of non-radial pulsation modes and rotation. Two
  longer-term variations are also detected: one at ~14 days resulting
  from a beating effect between the two main frequencies of short-term
  variations, the other at ~116 days due either to a beating of
  frequencies or to a zonal pulsation mode. <BR />Conclusions: Our
  analysis of the CoRoT light curve and ground-based spectroscopic
  data of <ASTROBJ>H</ASTROBJ>D 181231 has led to the determination
  of the fundamental and pulsational parameters of the star, including
  beating effects. This will allow a precise seismic modelling of this
  star. <P />Based on observations obtained with the CoRoT satellite,
  with FEROS at the 2.2 m télescope of the La Silla Observatory under
  the ESO Large Programme LP178.D-0361, with Narval at the Télescope
  Bernard Lyot of the Pic du Midi Observatory, and collected from the
  BeSS database. Table 5 is only available in electronic form at the
  CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via
  http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/506/143

Title: VizieR Online Data Catalog: Pulsations of HD 181231 (Neiner+,
    2009)
Authors: Neiner, C.; Gutierrez-Soto, J.; Baudin, F.; de Batz, B.;
   Fremat, Y.; Huat, A. -L.; Floquet, M.; Hubert, A. -M.; Leroy, B.;
   Diago, P. D.; Poretti, E.; Carrier, F.; Rainer, M.; Catala, C.; Thizy,
   O.; Buil, C.; Ribeiro, J.; Andrade, L.; Emilio, M.; Espinosa, F. Lara;
   Fabregat, J.; Janot-Pacheco, E.; Martayan, C.; Semaan, T.; Suso, J.;
   Baglin, A.; Michel, E.; Samadi, R.
Bibcode: 2009yCat..35060143N
Altcode:
  Frequencies (in c/d and microHz) detected in the CoRoT data of HD181231
  with the TiSAFT, Clean-NG, and Pasper methods. The minimum detectable
  frequency is 1/T=0.0064 c/d, i.e., 0.075microHz, where T is the length
  of the run. The error bar of the frequencies is Delta_f=1/(4T)=0.0016
  c/d, i.e., 0.019 microHz. The amplitudes and phases calculated with
  Amphi for each of the three sets of frequencies are reported in
  Cols. 5 and 6 together with their error bars. The last column gives
  our interpretation of each frequency. <P />(1 data file).

Title: VizieR Online Data Catalog: Fourier analysis of HD 49330
    CoRoT light curve (Huat+, 2009)
Authors: Huat, A. -L.; Hubert, A. -M.; Baudin, F.; Floquet, M.; Neiner,
   C.; Fremat, Y.; Gutierrez-Soto, J.; Andrade, L.; de Batz, B.; Diago,
   P. D.; Emilio, M.; Espinosa, F. Lara; Fabregat, J.; Janot-Pacheco,
   E.; Leroy, B.; Martayan, C.; Semaan, T.; Suso, J.; Auvergne, M.;
   Catala, C.; Michel, E.; Samadi, R.
Bibcode: 2009yCat..35060095H
Altcode:
  This work analyses the high precision photometric light curve obtained
  for the CoRoT target HD49330 (B0.5 IVe) which was observed during
  136.886 days with a sample of 32s. During the CoRoT run the star
  underwent an outburst often observed in hot Be star. The CoRoT light
  curve was analysed using Fourier methods and non-linear least square
  fitting. <P />(5 data files).

Title: Low-amplitude variations detected by CoRoT in the late type
    Be star HD 175869
Authors: Gutiérrez-Soto, J.; Floquet, M.; Neiner, C.; Hubert, A. -M.;
   Frémat, Y.; Andrade, L.; de Batz, B.; Diago, P. D.; Emilio, M.;
   Fabregat, J.; Facanha, W.; Huat, A. -L.; Janot-Pacheco, E.; Leroy,
   B.; Martayan, C.; Suso, J.; Garrido, R.
Bibcode: 2009CoAst.158..208G
Altcode:
  We present the analysis of the CoRoT data of the B8IIIe star HD
  175869 observed during a short run (27.3 days). The light curve shows
  low-amplitude variations of the order of 0.3 mmag. A frequency within
  the range determined for the rotational frequency and its 5 harmonics
  are detected. Other significant frequencies with a low amplitude of a
  few ppm are also found. The analysis of line profiles from ground-based
  spectroscopic data does not show any variation.

Title: Application of the TiSAFT code (Time Series Analysis with
    Fisher's Test)
Authors: Huat, A. -L.; Leroy, B.; Diago, P. D.
Bibcode: 2009CoAst.158..211H
Altcode:
  A new code for extracting frequencies, amplitudes and phases in a
  time series has been developed for the CoRoT data analysis: TiSAFT
  (Time Series Analysis with Fisher's Test of significance). We provide
  an application of the TiSAFT code on a simulated β Cephei light curve
  and on CoRoT data of a Be star, as well as a comparison with other
  codes already used in the CoRoT Be team.

Title: Preliminary results on the pulsations of Be stars with CoRoT
Authors: Neiner, C.; Gutiérrez-Soto, J.; Floquet, M.; Huat, A. -L.;
   Hubert, A. -M.; de Batz, B.; Leroy, B.; Frémat, Y.; Andrade, L.;
   Diago, P. D.; Emilio, M.; Fabregat, J.; Janot-Pacheco, E.; Martayan,
   C.; Semaan, T.; Suso, J.
Bibcode: 2009CoAst.158..319N
Altcode:
  We present preliminary results of the study of pulsations of Be stars
  from CoRoT observations. CoRoT detected many pulsation frequencies in
  all observed Be stars, usually interpreted in terms of g-modes but
  sometimes also corresponding to p-modes. Even in late Be stars, for
  which the detection of pulsation frequencies is very difficult from the
  ground, because of their very low amplitude, the quality and precision
  of the CoRoT data allows us to detect many frequencies. Seismic models
  have not yet been calculated but the calculations are ongoing.

Title: First results on the Be stars observed with the CoRoT satellite
Authors: Gutierrez-Soto, J.; Neiner, C.; Hubert, A. -M.; Floquet,
   M.; Huat, A. -L.; Diago, P. D.; Fabregat, J.; Leroy, B.; De Batz, B.;
   Andrade, L.; Emilio, M.; Facanha, W.; Fremat, Y.; Janot-Pacheco, E.;
   Martayan, C.; Suso, J.
Bibcode: 2008CoAst.157...70G
Altcode:
  In this paper we present an overview of the analysis of some of the
  Be stars observed with the CoRoT satellite up to this date. Be stars
  are very fast-rotating B-type stars which may pulsate as β Cephei
  or SPB stars. CoRoT has already observed 5 bright Be stars in the
  seismology fields and several tens of fainter ones in the exoplanet
  fields with an unprecedented quality and with a time duration from
  20 to 150 days. Multiple frequencies are detected in the majority
  of the stars. Pulsations, outbursts, beating phenomenon, possible
  transient modes, rotation, amplitude variability, etc. have been found
  in their light curves. In order to complement this study, ground-based
  spectroscopic data have also been analysed for the stars located in
  the seismology fields.

Title: The pulsations of the B5IVe star HD181231 revealed by CoRoT
Authors: Neiner, C.; Gutierrez-Soto, J.; Fremat, Y.; Floquet, M.;
   Hubert, A. -M.; Leroy, B.; de Batz, B.; Huat, A. -L.; Martayan, C.;
   Andrade, L.; Emilio, M.; Fabregat, J.; Facanha, W.; Janot-Pacheco,
   E.; Suso, J.
Bibcode: 2008CoAst.157..349N
Altcode:
  We present the first results of the analysis of the light curve of
  the B5IVe star HD 181231 obtained during a long run (5 months) of
  the CoRoT mission. The light curve shows clear pulsations and even
  beating effects. Several frequencies are detected. Ground-based spec-
  troscopic data have also been analyzed and help to determine the
  rotation frequency and identify pulsation modes.

Title: First asteroseismic results from CoRoT
Authors: Michel, E.; Baglin, A.; Weiss, W. W.; Auvergne, M.; Catala,
   C.; Aerts, C.; Appourchaux, T.; Barban, C.; Baudin, F.; Briquet, M.;
   Carrier, F.; Degroote, P.; De Ridder, J.; Garcia, R. A.; Garrido,
   R.; Gutiérrez-Soto, J.; Kallinger, T.; Lefevre, L.; Neiner,
   C.; Poretti, E.; Samadi, R.; Sarro, L.; Alecian, G.; Andrade, L.;
   Ballot, J.; Benomar, O.; Berthomieu, G.; Boumier, P.; Charpinet, S.;
   de Batz, B.; Deheuvels, S.; Dupret, M. -A.; Emilio, M.; Fabregat,
   J.; Facanha, W.; Floquet, M.; Frémat, Y.; Fridlund, M.; Goupil,
   M. -J.; Grotsch-Noels, A.; Handler, G.; Huat, A. -L.; Hubert, A. -M.;
   Janot-Pacheco, E.; Kjeldsen, H.; Lebreton, Y.; Leroy, B.; Martayan,
   C.; Mathias, P.; Miglio, A.; Montalban, J.; Monteiro, M. J. P. F. G.;
   Mosser, B.; Provost, J; Regulo, C.; Renan de Medeiros, J.; Ribas,
   I.; Roca Cortés, T.; Roxburgh, I.; Suso, J.; Thoul, A.; Toutain, T.;
   Tiphene, D.; Turck-Chieze, S.; Vauclair, S.; Vauclair, G.; Zwintz, K.
Bibcode: 2008CoAst.156...73M
Altcode:
  About one year after the end of the first observational run and
  six months after the first CoRoT data delivery, we comment the data
  exploitation progress for different types of stars. We consider first
  results to illustrate how these data of unprecedented quality shed a
  new light on the field of stellar seismology.

Title: First results on Be stars with CoRoT
Authors: Gutiérrez-Soto, J.; Neiner, C.; Hubert, A. -M.; Floquet,
   M.; Huat, A. -L.; Diago, P. D.; Fabregat, J.; Leroy, B.; de Batz,
   B.; Andrade, L.; Emilio, M.; Facanha, W.; Frémat, Y.; Janot-Pacheco,
   E.; Martayan, M.; Suso, J.; Garrido, R.
Bibcode: 2008sf2a.conf..475G
Altcode:
  In this paper we present an overview of the analysis of some of the
  Be stars observed with the CoRoT satellite up to this date. Be stars
  are very fast-rotating B-type stars which may pulsate as β Cephei
  or SPB stars. CoRoT has already observed 5 bright Be stars in the
  seismology fields and several tens of fainter ones in the exoplanet
  fields with an unprecedented quality and with a time duration from 20
  to 150 days. Multiple frequencies are detected in the majority of the
  stars. Pulsations, outbursts, beating phenomenon, rotation, amplitude
  variability, etc. have been found in their light curves. In order to
  complement this study, ground-based spectroscopic data have also been
  analysed for the stars located in the seismology fields.

Title: The Gaia satellite: a tool for Emission Line Stars and
    Hot Stars
Authors: Martayan, C.; Frémat, Y.; Blomme, R.; Jonckheere, A.; Borges,
   M.; de Batz, B.; Leroy, B.; Sordo, R.; Bouret, J. -C.; Martins, F.;
   Zorec, J.; Neiner, C.; Nazé, Y.; Alecian, E.; Floquet, M.; Hubert,
   A. -M.; Briot, D.; Miroshnichenko, A.; Kolka, I.; Stee, P.; Lanz,
   T.; Meynet, G.
Bibcode: 2008sf2a.conf..499M
Altcode: 2008arXiv0809.4417M
  The Gaia satellite will be launched at the end of 2011. It will
  observe at least 1 billion stars, and among them several million
  emission line stars and hot stars. Gaia will provide parallaxes for
  each star and spectra for stars till V magnitude equal to 17. After a
  general description of Gaia, we present the codes and methods, which
  are currently developed by our team. They will provide automatically
  the astrophysical parameters and spectral classification for the hot
  and emission line stars in the Milky Way and other close local group
  galaxies such as the Magellanic Clouds.

Title: New Methods for the Simulation of Ablative Thermal Protections
Authors: Nguyen-Bui, N. T. H.; Duffa, G.; Dubroca, B.; Leroy, B.
Bibcode: 2006ESASP.631E..13N
Altcode: 2006tpsh.confE..13N
  No abstract at ADS

Title: Inversion of line profiles using principal component analysis:
    some practical guidelines
Authors: Leroy, B.
Bibcode: 2003EAS.....9..117L
Altcode:
  Modern spectro-polarimeters produce huge amounts of data, and the <P
  />computing time needed to achieve data inversion is then becoming an
  <P />important bottleneck for the modelling activity. Recently, an <P
  />alternative to the traditional non-linear least squares technique <P
  />has been proposed; it relies on an old technique in multivariate <P
  />analysis, principal component analysis (PCA), and proves to be <P
  />much faster than traditional techniques (a gain of two <P />orders
  of magnitude in computation time is not unusual). We will <P />briefly
  recall this technique and discuss some means of making it <P />still
  more robust.

Title: Lockheed Martin Team's Next Generation Space Telescope (NGST)
    Reference Architecture
Authors: Martin, F.; Lesyna, L.; LeRoy, B.; Menzel, M.; Andersen,
   G.; Hyatt, B.; Triebes, K.; Rudiger, C.; Stier, M.; Cox, C.; Delp,
   C.; Hachkowski, R.; Hardman, G.; Keane, M.; MacFarlane, M.; Mordino,
   A.; Krim, M.
Bibcode: 2000ASPC..207...46M
Altcode: 2000ngst.conf...46M
  No abstract at ADS

Title: Improvements in Ablation Predictions for Reentry-Vehicles
    Nosetip
Authors: Couzi, J.; de Winne, J.; Leroy, B.
Bibcode: 1999ESASP.426..493C
Altcode: 1999asv..conf..493C
  No abstract at ADS

Title: Zeeman splitting in interstellar molecules. II. The ethynyl
    radical
Authors: Bel, N.; Leroy, B.
Bibcode: 1998A&A...335.1025B
Altcode:
  The Zeeman splitting that a longitudinal magnetic field would produce on
  the ethynyl radical is calculated for the transitions typical of those
  observed in the interstellar clouds. It turns out that the ubiquitous
  CCH radical adds to the list of the few interstellar molecules that
  could be used to determine magnetic fields in molecular clouds.

Title: Electrical properties of the gas within molecular clouds.
Authors: Bel, N.; Leroy, B.
Bibcode: 1996A&A...305..598B
Altcode:
  The electrical properties of the matter within a molecular cloud are
  examined. It is verified that, whilst the MHD approximation is still
  valid, the dominating presence of neutrals is the source of a very large
  anisotropy of the electrical conductivity; indeed, the latter differs in
  the directions parallel and perpendicular to the magnetic field by many
  orders of magnitude. The implication of this result for the dissipative
  processes (e.g., wave dissipation) cannot be underestimated. This
  anisotropy prevails during a large part of the evolution of a cloud.

Title: The dynamics of the solar convective zone by means of magnetic
    tracers
Authors: Collin, B.; Nesme-Ribes, E.; Leroy, B.; Meunier, N.;
   Sokoloff, D.
Bibcode: 1995CRASB.321..111C
Altcode: 1995CRASM.321..111C
  The rotation of the sun's convective zone can be studied by using
  the motions of magnetic features observed in the solar atmosphere but
  deeply rooted. It becomes possible to assign a depth of anchorage to
  these magnetic tracers, by helioseismology, which probes solar rotation
  layer by layer.

Title: Presumptive evidence for a low value of the total ozone
    content above Antarctica in September, 1958
Authors: Rigaud, P.; Leroy, B.
Bibcode: 1990AnGeo...8..791R
Altcode:
  No abstract at ADS

Title: Observability of the Magnetic Field in Molecular Clouds
Authors: Bel, N.; Leroy, B.
Bibcode: 1990IAUS..140..304B
Altcode:
  No abstract at ADS

Title: Zeeman splitting in interstellar molecules.
Authors: Bel, N.; Leroy, B.
Bibcode: 1989A&A...224..206B
Altcode:
  The Zeeman splitting due to a longitudinal magnetic field on some
  transitions of diatomic molecules observed in the interstellar clouds
  are calculated. Only CN and SO exhibit effects comparable to that of
  OH. Their observability in the mm range is discussed. In the same
  wavelength range, O2 would exhibit Zeeman effects even larger than
  that of OH, but must be observed from space radiotelescopes.

Title: Visible absorption cross-sections of NO2 at 298 K and 235 K
Authors: Leroy, B.; Rigaud, P.; Hicks, E.
Bibcode: 1987AnGeo...5..247L
Altcode:
  The absorption cross-sections of NO2 are measured between 426.8 nm
  and 449.9 nm in increments of 0.1 nm at temperatures of 298 K and 235
  K. The present results are applied to the C.M.S. (Composes Minoritaires
  Stratospheriques) spectrometer of the Geneva Observatory.

Title: Résolution analytique approchée des équations
    différentielles (ordinaires et aux dérivées partielles).
Authors: Leroy, B.
Bibcode: 1986mma..conf...33L
Altcode:
  No abstract at ADS

Title: Caractère quasi-universel des équations asymptotiques.
Authors: Leroy, B.
Bibcode: 1986mma..conf..439L
Altcode:
  No abstract at ADS

Title: On the derivation of the energy flux of linear
    magnetohydrodynamic waves
Authors: Leroy, B.
Bibcode: 1985GApFD..32..123L
Altcode:
  New light is shed on the derivation of the energy flux of the linear
  MHD waves. It is shown that, according to a suggestion of Lighthill,
  the usual perturbation procedure, which starts from the general
  expression for the energy flux, need not be supplemented by an
  averaging procedure. As a result, it is shown that to second order in
  the wave amplitude, a quantity identifiable as the wave energy flux
  is conserved. Some of the subtleties inherent in the derivation of
  the perturbation energy equation are discussed.

Title: Phase Mixing of Propagating Alfven Waves
Authors: Nocera, L.; Leroy, B.; Priest, E. R.
Bibcode: 1985IAUS..107..365N
Altcode:
  Among MHD waves, Alfvén waves have been proved to be the best
  candidates to reach the solar corona and, eventually, to be responsible
  for the heating of this outer part of the solar atmosphere. The problem
  concerning the mechanism able to transform the energy stored in the
  waves into heat is considered.

Title: Phase mixing of propagating Alfven waves
Authors: Nocera, L.; Priest, E. R.; Leroy, B.
Bibcode: 1984A&A...133..387N
Altcode:
  The fundamental wave solution found by Heyvaerts and Priest
  (1983) for the propagation and damping of shear Alfven waves in an
  inhomogeneous medium is checked against their assumptions, and a range
  of self-consistency is provided. By analyzing wave behavior outside
  this range, novel wave propagation properties are discovered. In the
  limit of weak damping, a uniformly valid solution is obtained by the
  method of multiple scales. For long wavelengths, the diffusion of
  energy in the direction transverse to the wave propagation is found
  to be important, and leads to weaker damping laws than those found by
  Heyvaerts and Priest.

Title: Introduction à la magnétohydrodynamique.
Authors: Leroy, B.
Bibcode: 1984cms..conf..123L
Altcode:
  No abstract at ADS

Title: Magnetoacoustic Gravity Waves and the Heating of the Solar
    Corona
Authors: Leroy, B.
Bibcode: 1984apoa.conf..326L
Altcode:
  No abstract at ADS

Title: Spectres d'absorption dans le proche ultraviolet de
    CS<SUB>2</SUB> et SO<SUB>2</SUB> entre 200 et 300K
Authors: Leroy, B.; Rigaud, P.; Jourdain, J. L.; Le Bras, G.
Bibcode: 1983M&P....29..177L
Altcode:
  Spectres d'absorption dans le proche ultraviolet de CS<SUB>2</SUB>
  et SO<SUB>2</SUB> entre 200 et 300K

Title: Propagation of Alfven waves in an isothermal atmosphere when
    the displacement current is not neglected
Authors: Leroy, B.
Bibcode: 1983A&A...125..371L
Altcode:
  If the solar atmosphere is modelled by a medium with a (possibly
  piece-wise) exponentially decreasing density, permeated by a
  uniform magnetic field, for MHD waves with a period ranging between
  a few seconds and several hours the WKBJ approximation is nowhere
  valid. Consequently, the concept of travelling wave is no longer
  meaningful and difficulties arise concerning the boundary condition
  that there be no incoming wave from infinity. In the past, these have
  been circumvented by confining arbitrarily the inhomogeneous medium to a
  region of finite extension. In the present paper the author proposes an
  alternative solution devoid of this free parameter; it simply consists
  in not discarding the displacement current in Maxwell's equations.

Title: Notions générales d'hydrodynamique.
Authors: Leroy, B.
Bibcode: 1983ihaa.conf....3L
Altcode:
  Contents: Introduction. Equations fondamentales. Similitude dynamique
  - analyse dimensionnelle. Approximation de Boussinesq - critères de
  similitude de la convection. Linéarisation - instabilité.

Title: Propagation of Waves in an Atmosphere in the Presence of a
    Magnetic Field - Part Six - Application of Magneto-Acoustic Mode
    Theory to the Solar Atmosphere
Authors: Schwartz, S. J.; Leroy, B.
Bibcode: 1982A&A...112...93S
Altcode:
  The theory of magneto-acoustic-gravity oscillations in an exponential
  atmosphere permeated by a uniform vertical magnetic field, presented by
  us in a companion paper, is applied to the solar atmosphere. Numerical
  parameters typical of both sunspots and coronal hole regions are used
  in our investigations over a wide frequency range of the energy flux
  carried by such oscillations from the photosphere to the corona. We
  conclude that the combined effects of stratification, partially
  transverse propagation and the transition region make it unlikely that
  such modes dominate coronal energetics.

Title: Propagation of waves in an atmosphere in the presence
    of a magnetic field. V - The theory of magneto-acoustic-gravity
    oscillations. VI - Application of magneto-acoustic-gravity mode
    theory to the solar atmosphere
Authors: Leroy, B.; Schwartz, S. J.
Bibcode: 1982A&A...112...84L
Altcode:
  The study concerns the oscillations and associated energy flux in a
  horizontally stratified medium permeated by a uniform vertical magnetic
  field parallel to a uniform gravitational field. Particular attention
  is given to the obvious applications to sunspots and the corona. In
  addition to the Alfven mode, the inhomogeneous analogs of the fast and
  slow MHD waves which propagate in a homogeneous medium are found. The
  boundary conditions and energy flux calculations that are appropriate
  for these modes are discussed, as are some general considerations
  of the series solutions themselves. The theory is then applied to
  the solar atmosphere. Numerical parameters typical of both sunspots
  and coronal hole regions are used in the investigations over a wide
  frequency range of the energy flux carried by such oscillations from
  the photosphere to the corona. It is concluded that the combined effects
  of stratification, partially transverse propagation, and the transition
  region make it unlikely that such modes dominate coronal energetics.

Title: Coronal oscillations - Energy transport in the sun by
    magneto-atmospheric modes
Authors: Leroy, B.
Bibcode: 1982PhDT.........1L
Altcode:
  Errors are demonstrated to exist in an eikonal approximation of the
  wave propagation in the solar atmosphere, and possible models for
  wave heating of the corona are considered. Consideration is given to
  data from the ATM instruments on board Skylab, from the OSO series
  satellites, and to studies of other stellar coronas with the IUE and
  Einstein Observatory. It is shown that Alfven waves propagating from
  the convection zone are not strong enough to heat the solar corona
  to the observed levels, which are actually hotter than those in the
  photosphere, although the corona has a less dense composition. A zone
  is argued to exist where magnetogravitosonic waves emerge in relatively
  stable condition, and have been detected in the solar wind. A linear
  analysis is presented to identify the region of origin of the upcoming
  waves, showing that slow vertical oscillations emerge above sunspots
  while slow magnetohydrodynamic waves do not.

Title: Propagation of waves in an atmosphere in the presence of a
    magnetic field. IV - Alfven waves in sunspot umbrae
Authors: Bel, N.; Leroy, B.
Bibcode: 1981A&A...104..203B
Altcode:
  The propagation of Alfven waves in a sunspot is studied without
  the aid of the eikonal approximation. It is found that the outgoing
  energy flux density reaching the corona is less than 10 to the -5 of
  the input energy flux density. This shows clearly that the cooling
  of sunspots by ascending Alfven waves is not possible. In the study,
  special attention is given to the transmittance of the atmosphere.

Title: Propagation of waves in an atmosphere in the presence of a
    magnetic field. III - Alfven waves in the solar atmosphere
Authors: Leroy, B.
Bibcode: 1981A&A....97..245L
Altcode:
  The propagation of Alfven waves is treated within the framework of a
  realistic model of the solar atmosphere without recourse to the eikonal
  approximation. The very low value of the transmittance (less than 1
  percent) indicates that Alfven waves observed in the interplanetary
  medium have not been generated in the sun's convection zone. This
  conclusion is supported by Pioneer 6 data.

Title: Propagation of waves in an atmosphere in the presence of a
    magnetic field. II - The reflection of Alfven waves
Authors: Leroy, B.
Bibcode: 1980A&A....91..136L
Altcode:
  The propagation of linear Alfven waves in an isothermal atmosphere is
  investigated without the use of the WKBJ approximation. Wave reflection
  induced by the density gradient is studied in detail, and special
  emphasis is placed on the coupled-modes representation. As an example,
  attention is given to the reflectance and transmittance of a slab of
  isothermal atmosphere with respect to Alfven waves.

Title: Determination of the total content of atmospheric nitrogen
    dioxide from ground-based measurements of stellar spectra
Authors: Leroy, B.; Hicks, E.; Vassy, A.
Bibcode: 1980AnG....36..205L
Altcode:
  From the experimental work of A. and E. Vassy (1937) on atmospheric
  absorption which was carried out in Morocco, the total atmospheric
  content of nitrogen dioxide was determined. The results obtained from
  stellar spectra, taken from the ground, vary according to the season
  and outline a night decay of NO2. The average value of the total
  atmospheric content of NO2 ranges from 5 x 10 to the 16th to 1 x 10
  to the 17th molecules/sq cm.

Title: Some Comments on the Propagation of Alfven Waves in an
    Atmosphere
Authors: Leroy, B.
Bibcode: 1980jfss.conf..251L
Altcode:
  No abstract at ADS

Title: Reflexion and Transmission of Alfven Waves in an Atmosphere
Authors: Bel, N.; Leroy, B.
Bibcode: 1980IAUS...91..131B
Altcode:
  No abstract at ADS

Title: Propagation of waves in an atmosphere in the presence of a
    magnetic field. I. The method.
Authors: Leroy, B.; Bel, N.
Bibcode: 1979A&A....78..129L
Altcode:
  A method is developed for studying MHD-wave propagation in an
  isothermal atmosphere permeated by a uniform magnetic field. The
  hydrodynamic Lagrangian for an infinitely conducting and isothermal
  atmosphere permeated by an arbitrary magnetic field is examined, the
  Euler-Lagrange equations are obtained, and some physical insight into
  the terms involved is given. Whitman's (1965) averaged Lagrangian method
  is reviewed and applied to magnetoacoustic gravity waves propagating
  in an isothermal atmosphere permeated by a uniform magnetic field
  arbitrarily oriented with respect to the (constant) gravity field. The
  general equations of motion are derived in the linear approximation,
  and an analytical method is outlined for solving these equations.

Title: A four-filter photometer for the measurement of total ozone
    in the atmosphere.
Authors: Leroy, B.
Bibcode: 1977JApMe..16.1082L
Altcode:
  The paper examines the design (optical and electronic), operating
  principle and calibration of a photometer which, using four interference
  filters and a photocell, is designed for the measurement of total
  ozone in the atmosphere from solar light scattered by the zenith
  sky. In a 1974 field test the four-filter photometer was compared
  to other instruments, particularly the Dobson spectrophotometer. It
  was determined that to avoid errors, the photometer data should be
  supplemented with a study of the effects of cloud cover, bandwidth
  and aerosols on total ozone measurements.

Title: Etude statistique des relations entre la radiation X solaire,
    les renforcements soudains d'atmosphériques et les plages d'activité
    solaire
Authors: Leroy, B.
Bibcode: 1977C&T....93..215L
Altcode:
  A statistical study correlating low-frequency electromagnetic wave
  propagation in the ionosphere, solar X-ray radiation and ranges of solar
  activity is reported. The level of solar X-ray radiation is found to
  correlate with the energetics of the electromagnetic wave propagation;
  a background level of Sudden Enhancement of Atmospherics (SEA) and a
  higher degree of enhancement are distinguished. Solar activity ranges
  determined from Solar Geophysical Data are also correlated to the
  SEA levels.

Title: Analytical Study of Magnetoacoustic Gravity Waves
Authors: Bel, N.; Leroy, B.
Bibcode: 1977A&A....55..239B
Altcode:
  Summary. An analytical study of magneto-acoustic gravity waves
  propagating in an isothermal atmosphere along the gravity field has
  been done; we obtain the equation giving the cut-off frequency and
  we establish the conditions for the existence of a cross-over in the
  dispersion equation. Key words: waves linear coupling magnetic field
  gravity solar atmosphere

Title: On the Possibility of Nucleosynthesis in Any Matter-Antimatter
    Symmetric Cosmology
Authors: Combes, F.; Fassi-Fehri, O.; Leroy, B.
Bibcode: 1975Ap&SS..37..151C
Altcode:
  In any matter-antimatter symmetric cosmology the primeval
  nucleosynthesis imposes a typical size of a region of
  matter (antimatter) much larger than the diffusion length of
  neutrons. Observational results on the abundances of cosmic deuterium
  and helium are used to evaluate how large it has to be. As a result
  we find that a minimal sizeL <SUB>1</SUB>∼1.5×10<SUP>8</SUP> cm at
  the temperatureT=1 MeV is compatible with the standard abundances of
  primeval helium and deuterium.

Title: Nucleosynthesis in a Symmetrical Universe
Authors: Combes, F.; Fassi-Fehri, O.; Leroy, B.
Bibcode: 1975hea..conf..155C
Altcode:
  No abstract at ADS

Title: Nucleosynthesis and matter-antimatter cosmologies
Authors: Combes, F.; Fassi-Fehri, O.; Leroy, B.
Bibcode: 1975Natur.253...25C
Altcode:
  IF light elements are of cosmological origin, then a
  given cosmological model should be able to reproduce the
  observed abundances<SUP>1</SUP>. Symmetric matter-antimatter
  cosmologies<SUP>2-4</SUP> do not stand up to this test too well,
  and encounter problems whose basis is the annihilation process itself.

Title: The Deuterium Puzzle in the Symmetric Universe
Authors: Leroy, B.; Nicolle, J. P.; Schatzman, E.
Bibcode: 1973NASSP.339..351L
Altcode: 1973gra..conf..351L
  No abstract at ADS

