S. Mathis
University of Paris
9 Papers
70 Citations
S. Mathis is an academic researcher from University of Paris. The author has contributed to research in topics: Asteroseismology & Magnetic field. The author has an hindex of 7, co-authored 9 publications. Previous affiliations of S. Mathis include Paris Diderot University & Janssen Pharmaceutica.
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Papers
On magnetic instabilities and dynamo action in stellar radiation zones
TL;DR: In this article, the authors examined the MHD instabilities arising in the radiation zone of a differentially rotating star, in which a poloidal field of fossil origin is sheared into a toroidal field.
Constraining the efficiency of angular momentum transport with asteroseismology of red giants: the effect of stellar mass
Patrick Eggenberger,Nadège Lagarde,Andrea Miglio,Josefina Montalbán,Sylvia Ekström,Cyril Georgy,Georges Meynet,Sébastien Salmon,T. Ceillier,Rafael A. García,S. Mathis,S. Deheuvels,André Maeder,J. W. den Hartogh,Raphael Hirschi,Raphael Hirschi +15 more
TL;DR: In this article, the authors investigate how asteroseismic measurements of red giants can help to characterize the additional transport mechanism and determine the efficiency of the missing transport mechanism for the low-mass red giant KIC 7341231 by computing rotating models that include an additional viscosity corresponding to this process.
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Constraining the efficiency of angular momentum transport with asteroseismology of red giants: the effect of stellar mass
Patrick Eggenberger,Nadège Lagarde,Andrea Miglio,Josefina Montalbán,Sylvia Ekström,Cyril Georgy,Georges Meynet,Sébastien Salmon,T. Ceillier,Rafael A. García,S. Mathis,S. Deheuvels,André Maeder,J. W. den Hartogh,Raphael Hirschi,Raphael Hirschi +15 more
TL;DR: In this paper, the authors investigate how asteroseismic measurements of red giants can help to characterize the additional transport mechanism and find that the viscosity corresponding to the additional mechanism is constrained to the range 1 x 10^3 - 1.3 × 10^4 cm^2/s.
Period spacings of gravity modes in rapidly rotating magnetic stars - II. The case of an oblique dipolar fossil magnetic field
Vincent Prat,S. Mathis,S. Mathis,Coralie Neiner,J. Van Beeck,Dominic M. Bowman,Conny Aerts,Conny Aerts,Conny Aerts +8 more
TL;DR: In this paper, the effect of the obliquity of a mixed (poloidal and toroidal) dipolar internal fossil magnetic field with respect to the rotation axis on the frequency of gravity modes in rapidly rotating stars was investigated.
New insights on the solar core
Rafael A. García,David Salabert,David Salabert,Jérôme Ballot,Antonio Eff-Darwich,Antonio Eff-Darwich,R. Garrido,Antonio Jiménez,Antonio Jiménez,S. Mathis,Savita Mathur,A. Moya,P. L. Pallé,P. L. Pallé,C. Régulo,C. Régulo,K. H. Sato,Juan Carlos Suárez,Sylvaine Turck-Chièze +18 more
- 01 Jan 2011
Abstract: Since the detection of the asymptotic properties of the dipole gravity modes in the Sun, the quest to find individual gravity modes has continued. An extensive and deeper analysis of 14 years of continuous GOLF/SoHO observational data, unveils the presence of a pattern of peaks that could be interpreted as individual dipole gravity modes in the frequency range between 60 and 140 microHz, with amplitudes compatible with the latest theoretical predictions. By collapsing the power spectrum we have obtained a quite constant splitting for these patterns in comparison to regions where no g modes were expected. Moreover, the same technique applied to simultaneous VIRGO/SoHO data unveils some common signals between the power spectra of both instruments. Thus, we are able to identify and characterize individual g modes with their central frequencies, amplitudes and splittings allowing to do seismic inversions of the rotation profile inside the solar core. These results open a new ligh t on the physics and dynamics of the solar deep core.
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