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Radial dependence of line profile variability in seven 09-B0.5 stars

Identifieur interne : 000149 ( France/Analysis ); précédent : 000148; suivant : 000150

Radial dependence of line profile variability in seven 09-B0.5 stars

Auteurs : F. Martins [Belgique] ; W. Marcolino [France] ; D. J. Hillier [États-Unis] ; J. F. Donati [France] ; J. C. Bouret [France]

Source :

RBID : Hal:hal-01439992

Abstract

Context. Massive stars show a variety of spectral variabilities: discrete absorption components in UV P-Cygni profiles. optical line profile variability, X-ray variability, and radial velocity modulations. Aims. Our goal is to study the spectral variability of single OB stars to better understand the relation between photospheric and wind variability. For that, we rely on high spectral resolution and on high signal-to-noise ratio optical spectra collected with the spectrograph NARVAL on the Telescope Bernard Lyot at Pic du Midi. Methods. We investigated the variability of twelve spectral lines by means of the temporal variance spectrum. The selected lines probe the radial structure of the atmosphere from the photosphere to the outer wind. We also performed a spectroscopic analysis with atmosphere models to derive the stellar and wind properties and to constrain the formation region of the selected lines. Results. We show that variability is observed in the wind lines of all bright giants and superelants on a daily tiniescale. Lines formed in the photosphere are sometimes variable, sometimes not The dwarf stars do not show any sign of variability, If variability is observed on a daily timescale, it can also (but not always) be observed on hourly timescales, albeit with lower amplitude. There is a very clear correlation between amplitude of the variability and fraction of the fine formed in the wind. Strong anti-correlations between the different parts of the temporal variance spectrum are observed. Conclusions. Our results indicate that variability is stronger in lines formed in the wind. A link between photospheric and wind variability is not obvious from our study, since wind variability is observed regardless of the level of photospheric variability. Different photospheric lines also show different degrees of variability.

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DOI: 10.1051/0004-6361/201423882


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Hal:hal-01439992

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<orgName>Laboratoire d'Astrophysique de Marseille</orgName>
<orgName type="acronym">LAM</orgName>
<date type="start">2012</date>
<desc>
<address>
<addrLine>Pôle de l'Étoile Site de Château-Gombert 38, rue Frédéric Joliot-Curie 13388 Marseille cedex 13</addrLine>
<country key="FR"></country>
</address>
<ref type="url">http://www.lam.fr/</ref>
</desc>
<listRelation>
<relation name="UMR7326" active="#struct-198056" type="direct"></relation>
<relation active="#struct-300045" type="direct"></relation>
<relation name="UMR7326" active="#struct-441569" type="direct"></relation>
</listRelation>
<tutelles>
<tutelle name="UMR7326" active="#struct-198056" type="direct">
<org type="institution" xml:id="struct-198056" status="VALID">
<idno type="IdRef">15863621X</idno>
<idno type="ISNI">0000 0001 2176 4817</idno>
<orgName>Aix Marseille Université</orgName>
<orgName type="acronym">AMU</orgName>
<date type="start">2012-01-01</date>
<desc>
<address>
<addrLine>Aix-Marseille UniversitéJardins du Pharo58 Boulevard Charles Livon13284 Marseille cedex 7</addrLine>
<country key="FR"></country>
</address>
<ref type="url">http://www.univ-amu.fr/</ref>
</desc>
</org>
</tutelle>
<tutelle active="#struct-300045" type="direct">
<org type="institution" xml:id="struct-300045" status="VALID">
<orgName>Institut national des sciences de l'Univers </orgName>
<orgName type="acronym">INSU - CNRS</orgName>
<date type="start">2007-04-19</date>
<desc>
<address>
<addrLine>INSU-CNRS3 rue Michel-Ange, 75794 Paris Cedex 16</addrLine>
<country key="FR"></country>
</address>
<ref type="url">http://www.insu.cnrs.fr/</ref>
</desc>
</org>
</tutelle>
<tutelle name="UMR7326" active="#struct-441569" type="direct">
<org type="institution" xml:id="struct-441569" status="VALID">
<idno type="IdRef">02636817X</idno>
<idno type="ISNI">0000000122597504</idno>
<orgName>Centre National de la Recherche Scientifique</orgName>
<orgName type="acronym">CNRS</orgName>
<date type="start">1939-10-19</date>
<desc>
<address>
<country key="FR"></country>
</address>
<ref type="url">http://www.cnrs.fr/</ref>
</desc>
</org>
</tutelle>
</tutelles>
</hal:affiliation>
<country>France</country>
<placeName>
<settlement type="city">Marseille</settlement>
<region type="region" nuts="2">Provence-Alpes-Côte d'Azur</region>
</placeName>
<orgName type="university">Université d'Aix-Marseille</orgName>
</affiliation>
</author>
</analytic>
<idno type="DOI">10.1051/0004-6361/201423882</idno>
<series>
<title level="j">Astronomy and Astrophysics - A&A</title>
<idno type="ISSN">0004-6361</idno>
<imprint>
<date type="datePub">2015-02</date>
</imprint>
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<front>
<div type="abstract" xml:lang="en">Context. Massive stars show a variety of spectral variabilities: discrete absorption components in UV P-Cygni profiles. optical line profile variability, X-ray variability, and radial velocity modulations. Aims. Our goal is to study the spectral variability of single OB stars to better understand the relation between photospheric and wind variability. For that, we rely on high spectral resolution and on high signal-to-noise ratio optical spectra collected with the spectrograph NARVAL on the Telescope Bernard Lyot at Pic du Midi. Methods. We investigated the variability of twelve spectral lines by means of the temporal variance spectrum. The selected lines probe the radial structure of the atmosphere from the photosphere to the outer wind. We also performed a spectroscopic analysis with atmosphere models to derive the stellar and wind properties and to constrain the formation region of the selected lines. Results. We show that variability is observed in the wind lines of all bright giants and superelants on a daily tiniescale. Lines formed in the photosphere are sometimes variable, sometimes not The dwarf stars do not show any sign of variability, If variability is observed on a daily timescale, it can also (but not always) be observed on hourly timescales, albeit with lower amplitude. There is a very clear correlation between amplitude of the variability and fraction of the fine formed in the wind. Strong anti-correlations between the different parts of the temporal variance spectrum are observed. Conclusions. Our results indicate that variability is stronger in lines formed in the wind. A link between photospheric and wind variability is not obvious from our study, since wind variability is observed regardless of the level of photospheric variability. Different photospheric lines also show different degrees of variability.</div>
</front>
</TEI>
<affiliations>
<list>
<country>
<li>Belgique</li>
<li>France</li>
<li>États-Unis</li>
</country>
<region>
<li>Pennsylvanie</li>
<li>Provence-Alpes-Côte d'Azur</li>
<li>Province du Brabant wallon</li>
<li>Région wallonne</li>
</region>
<settlement>
<li>Louvain-la-Neuve</li>
<li>Marseille</li>
<li>Pittsburgh</li>
</settlement>
<orgName>
<li>Université catholique de Louvain</li>
<li>Université d'Aix-Marseille</li>
<li>Université de Pittsburgh</li>
</orgName>
</list>
<tree>
<country name="Belgique">
<region name="Région wallonne">
<name sortKey="Martins, F" sort="Martins, F" uniqKey="Martins F" first="F." last="Martins">F. Martins</name>
</region>
</country>
<country name="France">
<region name="Provence-Alpes-Côte d'Azur">
<name sortKey="Marcolino, W" sort="Marcolino, W" uniqKey="Marcolino W" first="W." last="Marcolino">W. Marcolino</name>
</region>
<name sortKey="Bouret, J C" sort="Bouret, J C" uniqKey="Bouret J" first="J. C." last="Bouret">J. C. Bouret</name>
<name sortKey="Donati, J F" sort="Donati, J F" uniqKey="Donati J" first="J. F." last="Donati">J. F. Donati</name>
</country>
<country name="États-Unis">
<region name="Pennsylvanie">
<name sortKey="Hillier, D J" sort="Hillier, D J" uniqKey="Hillier D" first="D. J." last="Hillier">D. J. Hillier</name>
</region>
</country>
</tree>
</affiliations>
</record>

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