First Kepler results on compact pulsators – VII. Pulsating subdwarf B stars detected in the second half of the survey phase
Identifieur interne : 001201 ( Istex/Curation ); précédent : 001200; suivant : 001202First Kepler results on compact pulsators – VII. Pulsating subdwarf B stars detected in the second half of the survey phase
Auteurs : A. S. Baran [États-Unis, Pologne] ; S. D. Kawaler [États-Unis] ; M. D. Reed [États-Unis] ; A. C. Quint [États-Unis] ; S. J. O'Toole [Australie] ; R. H. Stensen [Belgique] ; J. H. Telting [Espagne] ; R. Silvotti [Italie] ; S. Charpinet [France] ; J. Christensen-Dalsgaard [Danemark] ; M. Still [États-Unis] ; J. R. Hall [États-Unis] ; K. Uddin [États-Unis]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011-07-11.
Descripteurs français
- Wicri :
- topic : Niveau sonore.
English descriptors
- KwdEn :
- Amplitude, Amplitude phase, Amplitude spectra, Amplitude spectrum, Artefact, Asymptotic, Asymptotic behaviour, Asymptotic signature, Baran, Binarity, Bottom panel, Class stars, Compact pulsators, Compact stars, Consecutive overtones, Data sets, Detection threshold, Ellipsoidal variation, Fourier, Fourier analysis, Frequency, Frequency range, Gravity modes, High frequencies, High frequency, Higher frequencies, Highest amplitudes, Horizontal line, Hybrid, Hybrid pulsators, Hybrid star, Hybrid stars, Instrumental issues, Kawaler, Kepler, Kepler data, Kepler mission, Kepler photometer, Kepler spacecraft, Last digits, Lower amplitude, Lower amplitudes, Middle panel, Minimum amplitude, Mnras, Moffett field, Monthly notices, More data, Multiplets, Noise level, Nyquist frequency, Original amplitude spectrum, Other hand, Other peaks, Other sdbv stars, Paper viii, Peak, Period spacings, Periodicity, Phase modulation, Phase variations, Photometric, Photometric data, Pressure modes, Pulsation, Pulsation amplitude, Pulsation modes, Pulsators, Residual, Residual amplitude spectrum, Residual peaks, Residual signal, Residual signals, Rich amplitude spectrum, Rotation period, Rotation periods, Rotational splitting, Same frequency, Sdbv, Sdbv stars, Second panel, Show evidence, Single peaks, Spectroscopic parameters, Split multiplets, Splittings, Star, Stensen, Strong peaks, Survey phase, Theoretical models, Thin hydrogen envelope, Third month, Third panel, Time resolution, Time series photometry, Transition region, Triplet.
- Teeft :
- Amplitude, Amplitude phase, Amplitude spectra, Amplitude spectrum, Artefact, Asymptotic, Asymptotic behaviour, Asymptotic signature, Baran, Binarity, Bottom panel, Class stars, Compact pulsators, Compact stars, Consecutive overtones, Data sets, Detection threshold, Ellipsoidal variation, Fourier, Fourier analysis, Frequency, Frequency range, Gravity modes, High frequencies, High frequency, Higher frequencies, Highest amplitudes, Horizontal line, Hybrid, Hybrid pulsators, Hybrid star, Hybrid stars, Instrumental issues, Kawaler, Kepler, Kepler data, Kepler mission, Kepler photometer, Kepler spacecraft, Last digits, Lower amplitude, Lower amplitudes, Middle panel, Minimum amplitude, Mnras, Moffett field, Monthly notices, More data, Multiplets, Noise level, Nyquist frequency, Original amplitude spectrum, Other hand, Other peaks, Other sdbv stars, Paper viii, Peak, Period spacings, Periodicity, Phase modulation, Phase variations, Photometric, Photometric data, Pressure modes, Pulsation, Pulsation amplitude, Pulsation modes, Pulsators, Residual, Residual amplitude spectrum, Residual peaks, Residual signal, Residual signals, Rich amplitude spectrum, Rotation period, Rotation periods, Rotational splitting, Same frequency, Sdbv, Sdbv stars, Second panel, Show evidence, Single peaks, Spectroscopic parameters, Split multiplets, Splittings, Star, Stensen, Strong peaks, Survey phase, Theoretical models, Thin hydrogen envelope, Third month, Third panel, Time resolution, Time series photometry, Transition region, Triplet.
Abstract
We present five new pulsating subdwarf B (sdB) stars discovered by the Kepler spacecraft during the asteroseismology survey phase. We perform time series analysis on the nearly continuous month‐long Kepler data sets of these five objects; these data sets provide nearly alias‐free time series photometry at unprecedented precision. Following an iterative pre‐whitening process, we derive the pulsational frequency spectra of these stars, separating out artefacts of known instrumental origin. We find that these new pulsating sdB stars are multiperiodic long‐period pulsators of the V1093 Her type, with the number of periodicities ranging from eight (KIC 8302197) to 53 (KIC 11558725). The frequencies and amplitudes are typical of g‐mode pulsators of this type. We do not find any evidence for binarity in the five stars from their observed pulsation frequencies. As these are g‐mode pulsators, we briefly looked for period spacings for mode identification and found average spacings of about 260 and 145 s. This may indicate l= 1 and 2 patterns. Some modes may show evidence of rotational splitting. These discoveries complete the list of compact pulsators found in the survey phase. Of the 13 compact pulsators, only one star was identified as a short‐period (p‐mode) V361 Hya pulsator, while all other new pulsators turned out to be V1093 Her class objects. Among the latter objects, two of them seemed to be pure V1093 Her while the others show additional low‐amplitude peaks in the p‐mode frequency range, suggesting their hybrid nature. Authenticity of these peaks will be tested with longer runs currently under analysis.
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DOI: 10.1111/j.1365-2966.2011.18486.x
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Pulsating subdwarf B stars detected in the second half of the survey phase</title><author><name sortKey="Baran, A S" sort="Baran, A S" uniqKey="Baran A" first="A. S." last="Baran">A. S. Baran</name><affiliation wicri:level="1"><mods:affiliation>Department of Physics and Astronomy, Iowa State University, 12 Physics Hall, Ames, IA 50011, USA</mods:affiliation><country xml:lang="fr">États-Unis</country><wicri:regionArea>Department of Physics and Astronomy, Iowa State University, 12 Physics Hall, Ames, IA 50011</wicri:regionArea></affiliation><affiliation wicri:level="1"><mods:affiliation>Mt Suhora Observatory, Cracow Pedagogical University, ul. Podchorazych 2, 30‐084 Krakow, Poland</mods:affiliation><country xml:lang="fr">Pologne</country><wicri:regionArea>Mt Suhora Observatory, Cracow Pedagogical University, ul. Podchorazych 2, 30‐084 Krakow</wicri:regionArea></affiliation><affiliation wicri:level="1"><mods:affiliation>E-mail: asb@iastate.edu</mods:affiliation><country wicri:rule="url">États-Unis</country></affiliation></author><author><name sortKey="Kawaler, S D" sort="Kawaler, S D" uniqKey="Kawaler S" first="S. D." last="Kawaler">S. D. Kawaler</name><affiliation wicri:level="1"><mods:affiliation>Department of Physics and Astronomy, Iowa State University, 12 Physics Hall, Ames, IA 50011, USA</mods:affiliation><country xml:lang="fr">États-Unis</country><wicri:regionArea>Department of Physics and Astronomy, Iowa State University, 12 Physics Hall, Ames, IA 50011</wicri:regionArea></affiliation></author><author><name sortKey="Reed, M D" sort="Reed, M D" uniqKey="Reed M" first="M. D." last="Reed">M. D. Reed</name><affiliation wicri:level="1"><mods:affiliation>Department of Physics, Astronomy, and Materials Science, Missouri State University, Springfield, MO 65897, USA</mods:affiliation><country xml:lang="fr">États-Unis</country><wicri:regionArea>Department of Physics, Astronomy, and Materials Science, Missouri State University, Springfield, MO 65897</wicri:regionArea></affiliation></author><author><name sortKey="Quint, A C" sort="Quint, A C" uniqKey="Quint A" first="A. C." last="Quint">A. C. Quint</name><affiliation wicri:level="1"><mods:affiliation>Department of Physics, Astronomy, and Materials Science, Missouri State University, Springfield, MO 65897, USA</mods:affiliation><country xml:lang="fr">États-Unis</country><wicri:regionArea>Department of Physics, Astronomy, and Materials Science, Missouri State University, Springfield, MO 65897</wicri:regionArea></affiliation></author><author><name sortKey="O Toole, S J" sort="O Toole, S J" uniqKey="O Toole S" first="S. J." last="O'Toole">S. J. O'Toole</name><affiliation wicri:level="1"><mods:affiliation>Anglo‐Australian Observatory, PO Box 296, Epping, NSW 1710, Australia</mods:affiliation><country xml:lang="fr">Australie</country><wicri:regionArea>Anglo‐Australian Observatory, PO Box 296, Epping, NSW 1710</wicri:regionArea></affiliation></author><author><name sortKey=" Stensen, R H" sort=" Stensen, R H" uniqKey=" Stensen R" first="R. H." last=" Stensen">R. H. Stensen</name><affiliation wicri:level="1"><mods:affiliation>Instituut voor Sterrenkunde, K. U. Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium</mods:affiliation><country xml:lang="fr">Belgique</country><wicri:regionArea>Instituut voor Sterrenkunde, K. U. Leuven, Celestijnenlaan 200D, 3001 Leuven</wicri:regionArea></affiliation></author><author><name sortKey="Telting, J H" sort="Telting, J H" uniqKey="Telting J" first="J. H." last="Telting">J. H. Telting</name><affiliation wicri:level="1"><mods:affiliation>Nordic Optical Telescope, 38700 Santa Cruz de La Palma, Spain</mods:affiliation><country xml:lang="fr">Espagne</country><wicri:regionArea>Nordic Optical Telescope, 38700 Santa Cruz de La Palma</wicri:regionArea></affiliation></author><author><name sortKey="Silvotti, R" sort="Silvotti, R" uniqKey="Silvotti R" first="R." last="Silvotti">R. Silvotti</name><affiliation wicri:level="1"><mods:affiliation>INAF‐Osservatorio Astronomico di Torino, Strada dell'Osservatorio 20, 10025 Pino Torinese, Italy</mods:affiliation><country xml:lang="fr">Italie</country><wicri:regionArea>INAF‐Osservatorio Astronomico di Torino, Strada dell'Osservatorio 20, 10025 Pino Torinese</wicri:regionArea></affiliation></author><author><name sortKey="Charpinet, S" sort="Charpinet, S" uniqKey="Charpinet S" first="S." last="Charpinet">S. Charpinet</name><affiliation wicri:level="1"><mods:affiliation>Laboratoire d'Astrophysique de Toulouse‐Tarbes, Université de Toulouse, CNRS, 14 Av. E. Belin, 31400 Toulouse, France</mods:affiliation><country xml:lang="fr">France</country><wicri:regionArea>Laboratoire d'Astrophysique de Toulouse‐Tarbes, Université de Toulouse, CNRS, 14 Av. E. Belin, 31400 Toulouse</wicri:regionArea></affiliation></author><author><name sortKey="Christensen Alsgaard, J" sort="Christensen Alsgaard, J" uniqKey="Christensen Alsgaard J" first="J." last="Christensen-Dalsgaard">J. Christensen-Dalsgaard</name><affiliation wicri:level="1"><mods:affiliation>Department of Physics and Astronomy, Aarhus University, 8000 Aarhus C, Denmark</mods:affiliation><country xml:lang="fr">Danemark</country><wicri:regionArea>Department of Physics and Astronomy, Aarhus University, 8000 Aarhus C</wicri:regionArea></affiliation></author><author><name sortKey="Still, M" sort="Still, M" uniqKey="Still M" first="M." last="Still">M. Still</name><affiliation wicri:level="1"><mods:affiliation>Bay Area Environmental Research Institute/NASA Ames Research Center, Moffett Field, CA 94035, USA</mods:affiliation><country xml:lang="fr">États-Unis</country><wicri:regionArea>Bay Area Environmental Research Institute/NASA Ames Research Center, Moffett Field, CA 94035</wicri:regionArea></affiliation></author><author><name sortKey="Hall, J R" sort="Hall, J R" uniqKey="Hall J" first="J. R." last="Hall">J. R. Hall</name><affiliation wicri:level="1"><mods:affiliation>Orbital Sciences Corporation/NASA Ames Research Center, Moffett Field, CA 94035, USA</mods:affiliation><country xml:lang="fr">États-Unis</country><wicri:regionArea>Orbital Sciences Corporation/NASA Ames Research Center, Moffett Field, CA 94035</wicri:regionArea></affiliation></author><author><name sortKey="Uddin, K" sort="Uddin, K" uniqKey="Uddin K" first="K." last="Uddin">K. Uddin</name><affiliation wicri:level="1"><mods:affiliation>Orbital Sciences Corporation/NASA Ames Research Center, Moffett Field, CA 94035, USA</mods:affiliation><country xml:lang="fr">États-Unis</country><wicri:regionArea>Orbital Sciences Corporation/NASA Ames Research Center, Moffett Field, CA 94035</wicri:regionArea></affiliation></author></analytic><monogr></monogr><series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="alt">MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY</title><idno type="ISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><imprint><biblScope unit="vol">414</biblScope><biblScope unit="issue">4</biblScope><biblScope unit="page" from="2871">2871</biblScope><biblScope unit="page" to="2884">2884</biblScope><biblScope unit="page-count">14</biblScope><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2011-07-11">2011-07-11</date></imprint><idno type="ISSN">0035-8711</idno></series></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Amplitude</term><term>Amplitude phase</term><term>Amplitude spectra</term><term>Amplitude spectrum</term><term>Artefact</term><term>Asymptotic</term><term>Asymptotic behaviour</term><term>Asymptotic signature</term><term>Baran</term><term>Binarity</term><term>Bottom panel</term><term>Class stars</term><term>Compact pulsators</term><term>Compact stars</term><term>Consecutive overtones</term><term>Data sets</term><term>Detection threshold</term><term>Ellipsoidal variation</term><term>Fourier</term><term>Fourier analysis</term><term>Frequency</term><term>Frequency range</term><term>Gravity modes</term><term>High frequencies</term><term>High frequency</term><term>Higher frequencies</term><term>Highest amplitudes</term><term>Horizontal line</term><term>Hybrid</term><term>Hybrid pulsators</term><term>Hybrid star</term><term>Hybrid stars</term><term>Instrumental issues</term><term>Kawaler</term><term>Kepler</term><term>Kepler data</term><term>Kepler mission</term><term>Kepler photometer</term><term>Kepler spacecraft</term><term>Last digits</term><term>Lower amplitude</term><term>Lower amplitudes</term><term>Middle panel</term><term>Minimum amplitude</term><term>Mnras</term><term>Moffett field</term><term>Monthly notices</term><term>More data</term><term>Multiplets</term><term>Noise level</term><term>Nyquist frequency</term><term>Original amplitude spectrum</term><term>Other hand</term><term>Other peaks</term><term>Other sdbv stars</term><term>Paper viii</term><term>Peak</term><term>Period spacings</term><term>Periodicity</term><term>Phase modulation</term><term>Phase variations</term><term>Photometric</term><term>Photometric data</term><term>Pressure modes</term><term>Pulsation</term><term>Pulsation amplitude</term><term>Pulsation modes</term><term>Pulsators</term><term>Residual</term><term>Residual amplitude spectrum</term><term>Residual peaks</term><term>Residual signal</term><term>Residual signals</term><term>Rich amplitude spectrum</term><term>Rotation period</term><term>Rotation periods</term><term>Rotational splitting</term><term>Same frequency</term><term>Sdbv</term><term>Sdbv stars</term><term>Second panel</term><term>Show evidence</term><term>Single peaks</term><term>Spectroscopic parameters</term><term>Split multiplets</term><term>Splittings</term><term>Star</term><term>Stensen</term><term>Strong peaks</term><term>Survey phase</term><term>Theoretical models</term><term>Thin hydrogen envelope</term><term>Third month</term><term>Third panel</term><term>Time resolution</term><term>Time series photometry</term><term>Transition region</term><term>Triplet</term></keywords><keywords scheme="Teeft" xml:lang="en"><term>Amplitude</term><term>Amplitude phase</term><term>Amplitude spectra</term><term>Amplitude spectrum</term><term>Artefact</term><term>Asymptotic</term><term>Asymptotic behaviour</term><term>Asymptotic signature</term><term>Baran</term><term>Binarity</term><term>Bottom panel</term><term>Class stars</term><term>Compact pulsators</term><term>Compact stars</term><term>Consecutive overtones</term><term>Data sets</term><term>Detection threshold</term><term>Ellipsoidal variation</term><term>Fourier</term><term>Fourier analysis</term><term>Frequency</term><term>Frequency range</term><term>Gravity modes</term><term>High frequencies</term><term>High frequency</term><term>Higher frequencies</term><term>Highest amplitudes</term><term>Horizontal line</term><term>Hybrid</term><term>Hybrid pulsators</term><term>Hybrid star</term><term>Hybrid stars</term><term>Instrumental issues</term><term>Kawaler</term><term>Kepler</term><term>Kepler data</term><term>Kepler mission</term><term>Kepler photometer</term><term>Kepler spacecraft</term><term>Last digits</term><term>Lower amplitude</term><term>Lower amplitudes</term><term>Middle panel</term><term>Minimum amplitude</term><term>Mnras</term><term>Moffett field</term><term>Monthly notices</term><term>More data</term><term>Multiplets</term><term>Noise level</term><term>Nyquist frequency</term><term>Original amplitude spectrum</term><term>Other hand</term><term>Other peaks</term><term>Other sdbv stars</term><term>Paper viii</term><term>Peak</term><term>Period spacings</term><term>Periodicity</term><term>Phase modulation</term><term>Phase variations</term><term>Photometric</term><term>Photometric data</term><term>Pressure modes</term><term>Pulsation</term><term>Pulsation amplitude</term><term>Pulsation modes</term><term>Pulsators</term><term>Residual</term><term>Residual amplitude spectrum</term><term>Residual peaks</term><term>Residual signal</term><term>Residual signals</term><term>Rich amplitude spectrum</term><term>Rotation period</term><term>Rotation periods</term><term>Rotational splitting</term><term>Same frequency</term><term>Sdbv</term><term>Sdbv stars</term><term>Second panel</term><term>Show evidence</term><term>Single peaks</term><term>Spectroscopic parameters</term><term>Split multiplets</term><term>Splittings</term><term>Star</term><term>Stensen</term><term>Strong peaks</term><term>Survey phase</term><term>Theoretical models</term><term>Thin hydrogen envelope</term><term>Third month</term><term>Third panel</term><term>Time resolution</term><term>Time series photometry</term><term>Transition region</term><term>Triplet</term></keywords><keywords scheme="Wicri" type="topic" xml:lang="fr"><term>Niveau sonore</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We present five new pulsating subdwarf B (sdB) stars discovered by the Kepler spacecraft during the asteroseismology survey phase. We perform time series analysis on the nearly continuous month‐long Kepler data sets of these five objects; these data sets provide nearly alias‐free time series photometry at unprecedented precision. Following an iterative pre‐whitening process, we derive the pulsational frequency spectra of these stars, separating out artefacts of known instrumental origin. We find that these new pulsating sdB stars are multiperiodic long‐period pulsators of the V1093 Her type, with the number of periodicities ranging from eight (KIC 8302197) to 53 (KIC 11558725). The frequencies and amplitudes are typical of g‐mode pulsators of this type. We do not find any evidence for binarity in the five stars from their observed pulsation frequencies. As these are g‐mode pulsators, we briefly looked for period spacings for mode identification and found average spacings of about 260 and 145 s. This may indicate l= 1 and 2 patterns. Some modes may show evidence of rotational splitting. These discoveries complete the list of compact pulsators found in the survey phase. Of the 13 compact pulsators, only one star was identified as a short‐period (p‐mode) V361 Hya pulsator, while all other new pulsators turned out to be V1093 Her class objects. Among the latter objects, two of them seemed to be pure V1093 Her while the others show additional low‐amplitude peaks in the p‐mode frequency range, suggesting their hybrid nature. Authenticity of these peaks will be tested with longer runs currently under analysis.</div></front></TEI></record>Pour manipuler ce document sous Unix (Dilib)
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|texte= First Kepler results on compact pulsators – VII. Pulsating subdwarf B stars detected in the second half of the survey phase
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