Baudin, Fréderic

[["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"]]