Baudin, Fréderic

[["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.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.journal","Experimental Astronomy"],["dc.contributor.author","Harra, Louise"],["dc.contributor.author","Andretta, Vincenzo"],["dc.contributor.author","Appourchaux, Thierry"],["dc.contributor.author","Baudin, Frédéric"],["dc.contributor.author","Bellot-Rubio, Luis"],["dc.contributor.author","Birch, Aaron C."],["dc.contributor.author","Boumier, Patrick"],["dc.contributor.author","Cameron, Robert H."],["dc.contributor.author","Carlsson, Matts"],["dc.contributor.author","Corbard, Thierry"],["dc.contributor.author","Schmutz, W."],["dc.date.accessioned","2021-09-01T06:42:39Z"],["dc.date.available","2021-09-01T06:42:39Z"],["dc.date.issued","2021"],["dc.description.abstract","Abstract A mission to view the solar poles from high helio-latitudes (above 60°) will build on the experience of Solar Orbiter as well as a long heritage of successful solar missions and instrumentation (e.g. SOHO Domingo et al. (Solar Phys. 162 (1-2), 1–37 1995), STEREO Howard et al. (Space Sci. Rev. 136 (1-4), 67–115 2008), Hinode Kosugi et al. (Solar Phys. 243 (1), 3–17 2007), Pesnell et al. Solar Phys. 275 (1–2), 3–15 2012), but will focus for the first time on the solar poles, enabling scientific investigations that cannot be done by any other mission. One of the major mysteries of the Sun is the solar cycle. The activity cycle of the Sun drives the structure and behaviour of the heliosphere and of course, the driver of space weather. In addition, solar activity and variability provides fluctuating input into the Earth climate models, and these same physical processes are applicable to stellar systems hosting exoplanets. One of the main obstructions to understanding the solar cycle, and hence all solar activity, is our current lack of understanding of the polar regions. In this White Paper, submitted to the European Space Agency in response to the Voyage 2050 call, we describe a mission concept that aims to address this fundamental issue. In parallel, we recognise that viewing the Sun from above the polar regions enables further scientific advantages, beyond those related to the solar cycle, such as unique and powerful studies of coronal mass ejection processes, from a global perspective, and studies of coronal structure and activity in polar regions. Not only will these provide important scientific advances for fundamental stellar physics research, they will feed into our understanding of impacts on the Earth and other planets’ space environment."],["dc.description.abstract","Abstract A mission to view the solar poles from high helio-latitudes (above 60°) will build on the experience of Solar Orbiter as well as a long heritage of successful solar missions and instrumentation (e.g. SOHO Domingo et al. (Solar Phys. 162 (1-2), 1–37 1995), STEREO Howard et al. (Space Sci. Rev. 136 (1-4), 67–115 2008), Hinode Kosugi et al. (Solar Phys. 243 (1), 3–17 2007), Pesnell et al. Solar Phys. 275 (1–2), 3–15 2012), but will focus for the first time on the solar poles, enabling scientific investigations that cannot be done by any other mission. One of the major mysteries of the Sun is the solar cycle. The activity cycle of the Sun drives the structure and behaviour of the heliosphere and of course, the driver of space weather. In addition, solar activity and variability provides fluctuating input into the Earth climate models, and these same physical processes are applicable to stellar systems hosting exoplanets. One of the main obstructions to understanding the solar cycle, and hence all solar activity, is our current lack of understanding of the polar regions. In this White Paper, submitted to the European Space Agency in response to the Voyage 2050 call, we describe a mission concept that aims to address this fundamental issue. In parallel, we recognise that viewing the Sun from above the polar regions enables further scientific advantages, beyond those related to the solar cycle, such as unique and powerful studies of coronal mass ejection processes, from a global perspective, and studies of coronal structure and activity in polar regions. Not only will these provide important scientific advances for fundamental stellar physics research, they will feed into our understanding of impacts on the Earth and other planets’ space environment."],["dc.identifier.doi","10.1007/s10686-021-09769-x"],["dc.identifier.pii","9769"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/89113"],["dc.language.iso","en"],["dc.notes.intern","DOI-Import GROB-455"],["dc.relation.eissn","1572-9508"],["dc.relation.issn","0922-6435"],["dc.title","A journey of exploration to the polar regions of a star: probing the solar poles and the heliosphere from high helio-latitude"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","L7"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","540"],["dc.contributor.author","Belkacem, K."],["dc.contributor.author","Dupret, M. A."],["dc.contributor.author","Baudin, F."],["dc.contributor.author","Appourchaux, T."],["dc.contributor.author","Marques, J. P."],["dc.contributor.author","Samadi, R."],["dc.date.accessioned","2018-11-07T09:11:26Z"],["dc.date.available","2018-11-07T09:11:26Z"],["dc.date.issued","2012"],["dc.description.abstract","The space-borne missions CoRoT and Kepler are providing a rich harvest of high-quality constraints on solar-like pulsators. Among the seismic parameters, mode damping rates remains poorly understood and are thus barely used to infer the physical properties of stars. Nevertheless, thanks to the CoRoT and Kepler spacecrafts it is now possible to measure damping rates for hundreds of main-sequence and thousands of red-giant stars with unprecedented precision. By using a non-adiabatic pulsation code including a time-dependent convection treatment, we compute damping rates for stellar models that are representative of solar-like pulsators from the main-sequence to the red-giant phase. This allows us to reproduce the observations of both CoRoT and Kepler, which validates our modeling of mode damping rates and thus the underlying physical mechanisms included in the modeling. By considering the perturbations of turbulent pressure and entropy (including the perturbation of the dissipation rate of turbulent energy into heat) by the oscillation in our computation, we succeed in reproducing the observed relation between damping rates and effective temperature. Moreover, we discuss the physical reasons for mode damping rates to scale with effective temperature, as observationally exhibited. Finally, this opens the way for the use of mode damping rates to probe turbulent convection in solar-like stars."],["dc.identifier.doi","10.1051/0004-6361/201218890"],["dc.identifier.fs","596719"],["dc.identifier.isi","000303315400008"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9593"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/26722"],["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","Damping rates of solar-like oscillations across the HR diagram Theoretical calculations confronted to CoRoT and Kepler observations"],["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"]]