Stahn, Thorsten

[["dc.bibliographiccitation.artnumber","A96"],["dc.bibliographiccitation.journal","Astronomy & Astrophysics"],["dc.bibliographiccitation.volume","543"],["dc.contributor.author","Escobar, M. E."],["dc.contributor.author","Théado, S."],["dc.contributor.author","Vauclair, S."],["dc.contributor.author","Ballot, J."],["dc.contributor.author","Charpinet, S."],["dc.contributor.author","Dolez, N."],["dc.contributor.author","Hui-Bon-Hoa, A."],["dc.contributor.author","Vauclair, G."],["dc.contributor.author","Gizon, Laurent"],["dc.contributor.author","Mathur, Saurabh"],["dc.contributor.author","Quirion, P.-O."],["dc.contributor.author","Stahn, Thorsten"],["dc.date.accessioned","2017-09-07T11:48:39Z"],["dc.date.available","2017-09-07T11:48:39Z"],["dc.date.issued","2012"],["dc.identifier.doi","10.1051/0004-6361/201218969"],["dc.identifier.fs","596686"],["dc.identifier.gro","3146982"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9609"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/4736"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","chake"],["dc.relation.issn","0004-6361"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","Precise modeling of the exoplanet host star and CoRoT main target HD 52265"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","no"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","13267"],["dc.bibliographiccitation.issue","33"],["dc.bibliographiccitation.journal","Proceedings of the National Academy of Sciences"],["dc.bibliographiccitation.lastpage","13271"],["dc.bibliographiccitation.volume","110"],["dc.contributor.author","Gizon, Laurent"],["dc.contributor.author","Ballot, Jérome"],["dc.contributor.author","Michel, Eric"],["dc.contributor.author","Stahn, Thorsten"],["dc.contributor.author","Vauclair, Gérard"],["dc.contributor.author","Bruntt, Hans"],["dc.contributor.author","Quirion, Pierre-Olivier"],["dc.contributor.author","Benomar, Othman"],["dc.contributor.author","Vauclair, Sylvie"],["dc.contributor.author","Appourchaux, Thierry"],["dc.contributor.author","Auvergne, Michel"],["dc.contributor.author","Baglin, Annie"],["dc.contributor.author","Barban, Caroline"],["dc.contributor.author","Baudin, Fréderic"],["dc.contributor.author","Bazot, Michaël"],["dc.contributor.author","Campante, Tiago"],["dc.contributor.author","Catala, Claude"],["dc.contributor.author","Chaplin, William"],["dc.contributor.author","Creevey, Orlagh"],["dc.contributor.author","Deheuvels, Sébastien"],["dc.contributor.author","Dolez, Noël"],["dc.contributor.author","Elsworth, Yvonne"],["dc.contributor.author","García, Rafael"],["dc.contributor.author","Gaulme, Patrick"],["dc.contributor.author","Mathis, Stéphane"],["dc.contributor.author","Mathur, Savita"],["dc.contributor.author","Mosser, Benoît"],["dc.contributor.author","Régulo, Clara"],["dc.contributor.author","Roxburgh, Ian"],["dc.contributor.author","Salabert, David"],["dc.contributor.author","Samadi, Réza"],["dc.contributor.author","Sato, Kumiko"],["dc.contributor.author","Verner, Graham"],["dc.contributor.author","Hanasoge, Shravan"],["dc.contributor.author","Sreenivasan, Katepalli R."],["dc.date.accessioned","2017-09-07T11:49:44Z"],["dc.date.available","2017-09-07T11:49:44Z"],["dc.date.issued","2013"],["dc.description.abstract","Rotation is thought to drive cyclic magnetic activity in the Sun and Sun-like stars. Stellar dynamos, however, are poorly understood owing to the scarcity of observations of rotation and magnetic fields in stars. Here, inferences are drawn on the internal rotation of a distant Sun-like star by studying its global modes of oscillation. We report asteroseismic constraints imposed on the rotation rate and the inclination of the spin axis of the Sun-like star HD 52265, a principal target observed by the CoRoT satellite that is known to host a planetary companion. These seismic inferences are remarkably consistent with an independent spectroscopic observation (rotational line broadening) and with the observed rotation period of star spots. Furthermore, asteroseismology constrains the mass of exoplanet HD 52265b. Under the standard assumption that the stellar spin axis and the axis of the planetary orbit coincide, the minimum spectroscopic mass of the planet can be converted into a true mass of 1:85+0:52 −0:42MJupiter, which implies that it is a planet, not a brown dwarf."],["dc.identifier.doi","10.1073/pnas.1303291110"],["dc.identifier.gro","3147422"],["dc.identifier.pmid","23898183"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/5005"],["dc.language.iso","en"],["dc.notes.status","final"],["dc.notes.submitter","chake"],["dc.relation.issn","0027-8424"],["dc.title","Seismic constraints on rotation of Sun-like star and mass of exoplanet"],["dc.type","journal_article"],["dc.type.internalPublication","unknown"],["dc.type.peerReviewed","no"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","231"],["dc.bibliographiccitation.issue","1-2"],["dc.bibliographiccitation.journal","Astrophysics and Space Science"],["dc.bibliographiccitation.lastpage","242"],["dc.bibliographiccitation.volume","329"],["dc.contributor.author","Schuh, Sonja"],["dc.contributor.author","Silvotti, Roberto"],["dc.contributor.author","Lutz, Ronny"],["dc.contributor.author","Loeptien, Bjoern"],["dc.contributor.author","Green, Elizabeth M."],["dc.contributor.author","Ostensen, Roy H."],["dc.contributor.author","Leccia, Silvio"],["dc.contributor.author","Kim, Seung-Lee"],["dc.contributor.author","Fontaine, Gilles"],["dc.contributor.author","Charpinet, Stephane"],["dc.contributor.author","Francoeur, Myriam"],["dc.contributor.author","Randall, Suzanna"],["dc.contributor.author","Rodriguez-Lopez, Cristina"],["dc.contributor.author","van Grootel, Valerie"],["dc.contributor.author","Odell, Andrew P."],["dc.contributor.author","Paparo, Margit"],["dc.contributor.author","Bognar, Zsofia"],["dc.contributor.author","Papics, Peter"],["dc.contributor.author","Nagel, Thorsten"],["dc.contributor.author","Beeck, Benjamin"],["dc.contributor.author","Hundertmark, Markus"],["dc.contributor.author","Stahn, Thorsten"],["dc.contributor.author","Dreizler, Stefan"],["dc.contributor.author","Hessman, Frederic V."],["dc.contributor.author","Dall'Ora, Massimo"],["dc.contributor.author","Mancini, Dario"],["dc.contributor.author","Cortecchia, Fausto"],["dc.contributor.author","Benatti, Serena"],["dc.contributor.author","Claudi, Riccardo"],["dc.contributor.author","Janulis, Rimvydas"],["dc.date.accessioned","2018-11-07T08:38:16Z"],["dc.date.available","2018-11-07T08:38:16Z"],["dc.date.issued","2010"],["dc.description.abstract","In 2007, a companion with planetary mass was found around the pulsating subdwarf B star V391 Pegasi with the timing method, indicating that a previously undiscovered population of substellar companions to apparently single subdwarf B stars might exist. Following this serendipitous discovery, the EXOTIME (http://www.na.astro.it/similar to silvotti/exotime/)) monitoring program has been set up to follow the pulsations of a number of selected rapidly pulsating subdwarf B stars on time scales of several years with two immediate observational goals: (1) determine (P)over dot of the pulsational periods P (2) search for signatures of substellar companions in O-C residuals due to periodic light travel time variations, which would be tracking the central star's companion-induced wobble around the centre of mass These sets of data should therefore, at the same time, on the one hand be useful to provide extra constraints for classical asteroseismological exercises from the P. ( comparison with \"local\" evolutionary models), and on the other hand allow one to investigate the preceding evolution of a target in terms of possible \"binary\" evolution by extending the otherwise unsuccessful search for companions to potentially very low masses. While timing pulsations may be an observationally expensive method to search for companions, it samples a different range of orbital parameters, inaccessible through orbital photometric effects or the radial velocity method: the latter favours massive close-in companions, whereas the timing method becomes increasingly more sensitive toward wider separations. In this paper we report on the status of the on-going observations and coherence analysis for two of the currently five targets, revealing very well-behaved pulsational characteristics in HS 0444+0458, while showing HS 0702+6043 to be more complex than previously thought."],["dc.identifier.doi","10.1007/s10509-010-0356-4"],["dc.identifier.isi","000282823200038"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/7631"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/18728"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Springer"],["dc.relation.issn","0004-640X"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","EXOTIME: searching for planets around pulsating subdwarf B stars"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","L10"],["dc.bibliographiccitation.issue","1"],["dc.bibliographiccitation.journal","The Astrophysical Journal"],["dc.bibliographiccitation.volume","748"],["dc.contributor.author","Metcalfe, T. S."],["dc.contributor.author","Chaplin, W. J."],["dc.contributor.author","Appourchaux, Thierry"],["dc.contributor.author","García, R. A."],["dc.contributor.author","Basu, S."],["dc.contributor.author","Brandão, I. M."],["dc.contributor.author","Creevey, O. L."],["dc.contributor.author","Deheuvels, S."],["dc.contributor.author","Doğan, G."],["dc.contributor.author","Eggenberger, P."],["dc.contributor.author","Karoff, C."],["dc.contributor.author","Miglio, A."],["dc.contributor.author","Stello, D."],["dc.contributor.author","Yıldız, M."],["dc.contributor.author","Çelik, Z."],["dc.contributor.author","Antia, H. M."],["dc.contributor.author","Benomar, O."],["dc.contributor.author","Howe, R."],["dc.contributor.author","Régulo, C."],["dc.contributor.author","Salabert, D."],["dc.contributor.author","Stahn, Thorsten"],["dc.contributor.author","Bedding, T. R."],["dc.contributor.author","Davies, G. R."],["dc.contributor.author","Elsworth, Y."],["dc.contributor.author","Gizon, Laurent"],["dc.contributor.author","Hekker, S."],["dc.contributor.author","Mathur, Saurabh"],["dc.contributor.author","Mosser, B."],["dc.contributor.author","Bryson, S. T."],["dc.contributor.author","Still, M. D."],["dc.contributor.author","Christensen-Dalsgaard, J."],["dc.contributor.author","Gilliland, R. L."],["dc.contributor.author","Kawaler, S. D."],["dc.contributor.author","Kjeldsen, H."],["dc.contributor.author","Ibrahim, K. A."],["dc.contributor.author","Klaus, T. C."],["dc.contributor.author","Li, J."],["dc.date.accessioned","2017-09-07T11:49:58Z"],["dc.date.available","2017-09-07T11:49:58Z"],["dc.date.issued","2012"],["dc.description.abstract","The evolved solar-type stars 16 Cyg A and B have long been studied as solar analogs, yielding a glimpse into the future of our own Sun. The orbital period of the binary system is too long to provide meaningful dynamical constraints on the stellar properties, but asteroseismology can help because the stars are among the brightest in the Kepler field. We present an analysis of three months of nearly uninterrupted photometry of 16 Cyg A and B from the Kepler space telescope. We extract a total of 46 and 41 oscillation frequencies for the two components, respectively, including a clear detection of octupole (l = 3) modes in both stars. We derive the properties of each star independently using the Asteroseismic Modeling Portal, fitting the individual oscillation frequencies and other observational constraints simultaneously. We evaluate the systematic uncertainties from an ensemble of results generated by a variety of stellar evolution codes and fitting methods. The optimal models derived by fitting each component individually yield a common age (t = 6.8 ± 0.4 Gyr) and initial composition (Z i = 0.024 ± 0.002, Y i = 0.25 ± 0.01) within the uncertainties, as expected for the components of a binary system, bolstering our confidence in the reliability of asteroseismic techniques. The longer data sets that will ultimately become available will allow future studies of differential rotation, convection zone depths, and long-term changes due to stellar activity cycles."],["dc.identifier.doi","10.1088/2041-8205/748/1/l10"],["dc.identifier.gro","3147458"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/5016"],["dc.language.iso","en"],["dc.notes.status","public"],["dc.notes.submitter","chake"],["dc.relation.issn","2041-8205"],["dc.title","Asteroseismology of the Solar Aanalogs 16 Cyg A and B from Kepler Observations"],["dc.type","journal_article"],["dc.type.internalPublication","unknown"],["dc.type.peerReviewed","no"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","31"],["dc.bibliographiccitation.issue","1-2"],["dc.bibliographiccitation.journal","Solar Physics"],["dc.bibliographiccitation.lastpage","52"],["dc.bibliographiccitation.volume","251"],["dc.contributor.author","Stahn, Thorsten"],["dc.contributor.author","Gizon, Laurent"],["dc.date.accessioned","2017-09-07T11:48:42Z"],["dc.date.available","2017-09-07T11:48:42Z"],["dc.date.issued","2008"],["dc.description.abstract","Quantitative helioseismology and asteroseismology require very precise measurements of the frequencies, amplitudes, and lifetimes of the global modes of stellar oscillation. The precision of these measurements depends on the total length (T), quality, and completeness of the observations. Except in a few simple cases, the effect of gaps in the data on measurement precision is poorly understood, in particular in Fourier space where the convolution of the observable with the observation window introduces correlations between different frequencies. Here we describe and implement a rather general method to retrieve maximum likelihood estimates of the oscillation parameters, taking into account the proper statistics of the observations. Our fitting method applies in complex Fourier space and exploits the phase information. We consider both solar-like stochastic oscillations and long-lived harmonic oscillations, plus random noise. Using numerical simulations, we demonstrate the existence of cases for which our improved fitting method is less biased and has a greater precision than when the frequency correlations are ignored. This is especially true of low signal-to-noise solar-like oscillations. For example, we discuss a case where the precision of the mode frequency estimate is increased by a factor of five, for a duty cycle of 15%. In the case of long-lived sinusoidal oscillations, a proper treatment of the frequency correlations does not provide any significant improvement; nevertheless, we confirm that the mode frequency can be measured from gapped data with a much better precision than the 1/T Rayleigh resolution."],["dc.identifier.doi","10.1007/s11207-008-9181-0"],["dc.identifier.gro","3147044"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/4776"],["dc.language.iso","en"],["dc.notes.status","final"],["dc.notes.submitter","chake"],["dc.relation.issn","0038-0938"],["dc.title","Fourier Analysis of Gapped Time Series: Improved Estimates of Solar and Stellar Oscillation Parameters"],["dc.type","journal_article"],["dc.type.internalPublication","unknown"],["dc.type.peerReviewed","no"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","A34"],["dc.bibliographiccitation.journal","Astronomy & Astrophysics"],["dc.bibliographiccitation.volume","564"],["dc.contributor.author","Boumier, P."],["dc.contributor.author","Benomar, O."],["dc.contributor.author","Baudin, F."],["dc.contributor.author","Verner, G. A."],["dc.contributor.author","Appourchaux, T."],["dc.contributor.author","Lebreton, Y."],["dc.contributor.author","Gaulme, P."],["dc.contributor.author","Chaplin, W. J."],["dc.contributor.author","García, R. A."],["dc.contributor.author","Hekker, S."],["dc.contributor.author","Regulo, C."],["dc.contributor.author","Salabert, D."],["dc.contributor.author","Stahn, T."],["dc.contributor.author","Elsworth, Y."],["dc.contributor.author","Gizon, L."],["dc.contributor.author","Hall, M."],["dc.contributor.author","Mathur, S."],["dc.contributor.author","Michel, E."],["dc.contributor.author","Morel, T."],["dc.contributor.author","Mosser, B."],["dc.contributor.author","Poretti, E."],["dc.contributor.author","Rainer, M."],["dc.contributor.author","Roxburgh, I. W."],["dc.contributor.author","Nascimento, J.-D. Do"],["dc.contributor.author","Samadi, R."],["dc.contributor.author","Auvergne, M."],["dc.contributor.author","Chaintreuil, S."],["dc.contributor.author","Baglin, A."],["dc.contributor.author","Catala, C."],["dc.date.accessioned","2017-09-07T11:49:43Z"],["dc.date.available","2017-09-07T11:49:43Z"],["dc.date.issued","2014"],["dc.description.abstract","Context. The object HD 43587Aa is a G0V star observed during the 145-day LRa03 run of the COnvection, ROtation and planetary Transits space mission (CoRoT), for which complementary High Accuracy Radial velocity Planet Searcher (HARPS) spectra with S/N > 300 were also obtained. Its visual magnitude is 5.71, and its effective temperature is close to 5950 K. It has a known companion in a highly eccentric orbit and is also coupled with two more distant companions. Aims. We undertake a preliminary investigation of the internal structure of HD 43587Aa. Methods. We carried out a seismic analysis of the star, using maximum likelihood estimators and Markov chain Monte Carlo methods. Results. We established the first table of the eigenmode frequencies, widths, and heights for HD 43587Aa. The star appears to have a mass and a radius slightly larger than the Sun, and is slightly older (5.6 Gyr). Two scenarios are suggested for the geometry of the star: either its inclination angle is very low, or the rotation velocity of the star is very low. Conclusions. A more detailed study of the rotation and of the magnetic and chromospheric activity for this star is needed, and will be the subject of a further study. New high resolution spectrometric observations should be performed for at least several months in duration."],["dc.identifier.doi","10.1051/0004-6361/201322478"],["dc.identifier.gro","3147406"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/10917"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/4995"],["dc.language.iso","en"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","chake"],["dc.relation.issn","0004-6361"],["dc.title","Seismic analysis of HD 43587Aa, a solar-like oscillator in a multiple system"],["dc.type","journal_article"],["dc.type.internalPublication","unknown"],["dc.type.peerReviewed","no"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","A97"],["dc.bibliographiccitation.journal","Astronomy & Astrophysics"],["dc.bibliographiccitation.volume","530"],["dc.contributor.author","Ballot, J."],["dc.contributor.author","Gizon, L."],["dc.contributor.author","Samadi, R."],["dc.contributor.author","Vauclair, G."],["dc.contributor.author","Benomar, O."],["dc.contributor.author","Bruntt, H."],["dc.contributor.author","Mosser, B."],["dc.contributor.author","Stahn, T."],["dc.contributor.author","Verner, G. A."],["dc.contributor.author","Campante, T. L."],["dc.contributor.author","García, R. A."],["dc.contributor.author","Mathur, S."],["dc.contributor.author","Salabert, D."],["dc.contributor.author","Gaulme, P."],["dc.contributor.author","Régulo, C."],["dc.contributor.author","Roxburgh, I. W."],["dc.contributor.author","Appourchaux, T."],["dc.contributor.author","Baudin, F."],["dc.contributor.author","Catala, C."],["dc.contributor.author","Chaplin, W. J."],["dc.contributor.author","Deheuvels, S."],["dc.contributor.author","Michel, E."],["dc.contributor.author","Bazot, M."],["dc.contributor.author","Creevey, O. L."],["dc.contributor.author","Dolez, N."],["dc.contributor.author","Elsworth, Y."],["dc.contributor.author","Sato, K. H."],["dc.contributor.author","Vauclair, S."],["dc.contributor.author","Auvergne, M."],["dc.contributor.author","Baglin, A."],["dc.date.accessioned","2017-09-07T11:48:38Z"],["dc.date.available","2017-09-07T11:48:38Z"],["dc.date.issued","2011"],["dc.description.abstract","Context. The star HD 52265 is a G0V metal-rich exoplanet-host star observed in the seismology field of the CoRoT space telescope from November 2008 to March 2009. The satellite collected 117 days of high-precision photometric data on this star, showing that it presents solar-like oscillations. HD 52265 was also observed in spectroscopy with the Narval spectrograph at the same epoch.Aims. We characterise HD 52265 using both spectroscopic and seismic data.Methods. The fundamental stellar parameters of HD 52265 were derived with the semi-automatic software VWA, and the projected rotational velocity was estimated by fitting synthetic profiles to isolated lines in the observed spectrum. The parameters of the observed p modes were determined with a maximum-likelihood estimation. We performed a global fit of the oscillation spectrum, over about ten radial orders, for degrees l = 0 to 2. We also derived the properties of the granulation, and analysed a signature of the rotation induced by the photospheric magnetic activity.Results. Precise determinations of fundamental parameters have been obtained: Teff = 6100   ±   60   K, log g = 4.35   ±   0.09, [M/H] = 0.19   ±   0.05, as well as . We have measured a mean rotation period Prot = 12.3   ±   0.15 days, and find a signature of differential rotation. The frequencies of 31 modes are reported in the range 1500–2550   μHz. The large separation exhibits a clear modulation around the mean value . Mode widths vary with frequency along an S-shape with a clear local maximum around 1800   μHz. We deduce lifetimes ranging between 0.5 and 3 days for these modes. Finally, we find a maximal bolometric amplitude of about 3.96   ±   0.24 ppm for radial modes."],["dc.identifier.doi","10.1051/0004-6361/201116547"],["dc.identifier.gro","3146960"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/4726"],["dc.language.iso","en"],["dc.notes.status","final"],["dc.notes.submitter","chake"],["dc.relation.issn","0004-6361"],["dc.title","Accurate p-mode measurements of the G0V metal-rich CoRoT target HD 52265"],["dc.type","journal_article"],["dc.type.internalPublication","unknown"],["dc.type.peerReviewed","no"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","A82"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","601"],["dc.contributor.author","White, Timothy R."],["dc.contributor.author","Benomar, O."],["dc.contributor.author","Aguirre, Victor Silva"],["dc.contributor.author","Ball, Warrick H."],["dc.contributor.author","Bedding, Timothy R."],["dc.contributor.author","Chaplin, W. J."],["dc.contributor.author","Christensen-Dalsgaard, Joergen"],["dc.contributor.author","Garcia, R. A."],["dc.contributor.author","Gizon, Laurent"],["dc.contributor.author","Stello, Dennis"],["dc.contributor.author","Aigrain, S."],["dc.contributor.author","Antia, H. M."],["dc.contributor.author","Appourchaux, T."],["dc.contributor.author","Bazot, M."],["dc.contributor.author","Campante, Tiago L."],["dc.contributor.author","Creevey, O. L."],["dc.contributor.author","Davies, G. R."],["dc.contributor.author","Elsworth, Yvonne P."],["dc.contributor.author","Gaulme, P."],["dc.contributor.author","Handberg, Rasmus"],["dc.contributor.author","Hekker, Saskia"],["dc.contributor.author","Houdek, Gunter"],["dc.contributor.author","Howe, R."],["dc.contributor.author","Huber, D."],["dc.contributor.author","Karoff, Christoffer"],["dc.contributor.author","Marques, J. P."],["dc.contributor.author","Mathur, S."],["dc.contributor.author","McQuillan, A."],["dc.contributor.author","Metcalfe, T. S."],["dc.contributor.author","Mosser, B."],["dc.contributor.author","Nielsen, M. B."],["dc.contributor.author","Regulo, C."],["dc.contributor.author","Salabert, D."],["dc.contributor.author","Stahn, Thorsten"],["dc.date.accessioned","2018-11-07T10:24:05Z"],["dc.date.available","2018-11-07T10:24:05Z"],["dc.date.issued","2017"],["dc.description.abstract","Binary star systems are important for understanding stellar structure and evolution, and are especially useful when oscillations can be detected and analysed with asteroseismology. However, only four systems are known in which solar-like oscillations are detected in both components. Here, we analyse the fifth such system, HD 176465, which was observed by Kepler. We carefully analysed the system's power spectrum to measure individual mode frequencies, adapting our methods where necessary to accommodate the fact that both stars oscillate in a similar frequency range. We also modelled the two stars independently by fitting stellar models to the frequencies and complementary parameters. We are able to cleanly separate the oscillation modes in both systems. The stellar models produce compatible ages and initial compositions for the stars, as is expected from their common and contemporaneous origin. Combining the individual ages, the system is about 3.0 +/- 0.5 Gyr old. The two components of HD 176465 are young physically-similar oscillating solar analogues, the first such system to be found, and provide important constraints for stellar evolution and asteroseismology."],["dc.identifier.doi","10.1051/0004-6361/201628706"],["dc.identifier.isi","000402313500082"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/15004"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/42591"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","PUB_WoS_Import"],["dc.publisher","Edp Sciences S A"],["dc.relation","info:eu-repo/grantAgreement/EC/FP7/338251/EU//STELLARAGES"],["dc.relation.issn","1432-0746"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","Kepler observations of the asteroseismic binary HD 176465"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","L25"],["dc.bibliographiccitation.issue","2"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","L28"],["dc.bibliographiccitation.volume","448"],["dc.contributor.author","Nagel, T."],["dc.contributor.author","Schuh, Sonja"],["dc.contributor.author","Kusterer, D. J."],["dc.contributor.author","Stahn, Thorsten"],["dc.contributor.author","Hugelmeyer, S. D."],["dc.contributor.author","Dreizler, Stefan"],["dc.contributor.author","Gansicke, B. T."],["dc.contributor.author","Schreiber, M. R."],["dc.date.accessioned","2018-11-07T10:09:39Z"],["dc.date.available","2018-11-07T10:09:39Z"],["dc.date.issued","2006"],["dc.description.abstract","Aims. The archival spectrum of SDSS J212531.92- 010745.9 shows not only the typical signature of a PG1159 star, but also indicates the presence of a companion. Our aim was the proof of the binary nature of this object and the determination of its orbital period. Methods. We performed time-series photometry of SDSS J212531.92-010745.9. We observed the object during 10 nights, spread over one month, with the Tubingen 80 cm and the Gottingen 50 cm telescopes. We fitted the observed light curve with a sine and simulated the light curve of this system with the nightfall program. Furthermore, we compared the spectrum of SDSS J212531.92-010745.9 with NLTE models, the results of which also constrain the light curve solution. Results. An orbital period of 6.95616(33) h with an amplitude of 0.354(3) mag is derived from our observations. A pulsation period could not be detected. For the PG1159 star we found, as preliminary results from comparison with our NLTE models, T-eff similar to 90 000 K, log g similar to 7.60, and the abundance ratio C C/He similar to 0.05 by number fraction. For the companion we obtained with a mean radius of 0.4 +/- 0.1 R-., amass of 0.4 +/- 0.1 M-., and a temperature of 8200 K on the irradiated side, good agreement between the observed light curve and the, nightfall simulation, but we do not regard those values as final."],["dc.identifier.doi","10.1051/0004-6361:200600009"],["dc.identifier.isi","000235777700005"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/7679"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/39691"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Edp Sciences S A"],["dc.relation.issn","0004-6361"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","SDSS J212531.92-010745.9 - the first definite PG 1159 close binary system"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","257"],["dc.bibliographiccitation.issue","1-4"],["dc.bibliographiccitation.journal","Space Science Reviews"],["dc.bibliographiccitation.lastpage","258"],["dc.bibliographiccitation.volume","156"],["dc.contributor.author","Gizon, L."],["dc.contributor.author","Schunker, H."],["dc.contributor.author","Baldner, C. S."],["dc.contributor.author","Basu, S."],["dc.contributor.author","Birch, A. C."],["dc.contributor.author","Bogart, R. S."],["dc.contributor.author","Braun, D. C."],["dc.contributor.author","Cameron, R. H."],["dc.contributor.author","Duvall Jr., T. L."],["dc.contributor.author","Hanasoge, S. M."],["dc.contributor.author","Jackiewicz, J."],["dc.contributor.author","Roth, M."],["dc.contributor.author","Stahn, T."],["dc.contributor.author","Thompson, M. J."],["dc.contributor.author","Zharkov, S."],["dc.date.accessioned","2017-09-07T11:48:39Z"],["dc.date.available","2017-09-07T11:48:39Z"],["dc.date.issued","2010"],["dc.identifier.doi","10.1007/s11214-010-9688-1"],["dc.identifier.gro","3146992"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/4741"],["dc.language.iso","en"],["dc.notes.status","final"],["dc.notes.submitter","chake"],["dc.relation.eissn","1572-9672"],["dc.relation.iserratumof","/handle/2/4740"],["dc.relation.issn","0038-6308"],["dc.title","Erratum to: Helioseismology of Sunspots: A Case Study of NOAA Region 9787"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","no"],["dc.type.subtype","erratum_ja"],["dspace.entity.type","Publication"]]