CoRoT Measures Solar-Like Oscillations and Granulation in Stars Hotter Than the Sun

Bibcode
2008Sci...322..558M
DOI
10.1126/science.1163004
Michel, Eric; Baglin, Annie; Auvergne, Michel; Catala, Claude; Samadi, Reza; Baudin, Frédéric; Appourchaux, Thierry; Barban, Caroline; Weiss, Werner W.; Berthomieu, Gabrielle; Boumier, Patrick; Dupret, Marc-Antoine; Garcia, Rafael A.; Fridlund, Malcolm; Garrido, Rafael; Goupil, Marie-Jo; Kjeldsen, Hans; Lebreton, Yveline; Mosser, Benoît; Grotsch-Noels, Arlette; Janot-Pacheco, Eduardo; Provost, Janine; Roxburgh, Ian W.; Thoul, Anne; Toutain, Thierry; Tiphène, Didier; Turck-Chieze, Sylvaine; Vauclair, Sylvie D.; Vauclair, Gérard P.; Aerts, Conny; Alecian, Georges; Ballot, Jérôme; Charpinet, Stéphane; Hubert, Anne-Marie; Lignières, François; Mathias, Philippe; Monteiro, Mario J. P. F. G.; Neiner, Coralie; Poretti, Ennio; Renan de Medeiros, José; Ribas, Ignasi; Rieutord, Michel L.; Roca Cortés, T.; Zwintz, Konstanze
Referencia bibliográfica

Science, Volume 322, Issue 5901, pp. 558- (2008).

Fecha de publicación:
10
2008
Revista
Science
Número de autores
44
Número de autores del IAC
1
Número de citas
244
Número de citas referidas
191
Descripción
Oscillations of the Sun have been used to understand its interior structure. The extension of similar studies to more distant stars has raised many difficulties despite the strong efforts of the international community over the past decades. The CoRoT (Convection Rotation and Planetary Transits) satellite, launched in December 2006, has now measured oscillations and the stellar granulation signature in three main sequence stars that are noticeably hotter than the sun. The oscillation amplitudes are about 1.5 times as large as those in the Sun; the stellar granulation is up to three times as high. The stellar amplitudes are about 25% below the theoretic values, providing a measurement of the nonadiabaticity of the process ruling the oscillations in the outer layers of the stars.
Proyectos relacionados
Helio y Astroseismología
Sismología Solar y Estelar y Búsqueda de Exoplanetas
Los objetivos principales de este proyecto son: 1) estudiar la estructura y la dinámica del interior solar, 2) ampliar este estudio a otros tipos de estrellas y 3) buqueda de planetas extrasolares utilizando métodos fotométricos y su caracterización con información complementaria (espectrometría). Para alcanzar el primer objetivo, utilizamos la
Savita
Mathur
En ejecución
Tipo
Con árbitro
Física estelar e interestelar (FEEI)

Te puede interesar

  • Con árbitro
    Ultralight dark matter simulations and stellar dynamics: Tension in dwarf galaxies for <inline-formula><mml:math><mml:mrow><mml:mi>m</mml:mi><mml:mo>&lt;</mml:mo><mml:mn>5</mml:mn><mml:mo>×</mml:mo><mml:msup><mml:mrow><mml:mn>10</mml:mn></mml:mrow><mml:mr
    We present numerical simulations of dark matter and stellar dynamics in ultralight dark matter halos tailored to mimic dwarf galaxies. An important effect we observe is the dynamical evolution of the stellar half-light radius and velocity dispersion, which makes previous equilibrium models significantly incomplete. Based on half-light radius
    Teodori, Luca et al.

    Fecha de publicación:

    1
    2026
    Bibcode
    2026PhRvD.113b3055T
    Número de citas
    0
  • Con árbitro
    The ALMA survey to Resolve exoKuiper belt Substructures (ARKS): VI. Asymmetries and offsets
    Context. Asymmetries in debris discs provide unique clues to understand the evolution and architecture of planetary systems. Previous studies of debris discs at (sub)millimetre wavelengths have suggested the presence of asymmetries in a wide variety of systems, yet the lack of sufficiently sensitive high-resolution observations means that the
    Lovell, J. B. et al.

    Fecha de publicación:

    1
    2026
    Bibcode
    2026A&A...705A.200L
    Número de citas
    10
  • Con árbitro
    The ALMA survey to Resolve exoKuiper belt Substructures (ARKS): VII. Optically thick gas with broad CO gaussian local line profiles in the HD 121617 disc
    Context. CO gas has been detected in ~20 debris discs, typically classified as CO-poor or CO-rich. We present observations of the CO-rich HD 121617 debris disc as part of the ALMA survey to Resolve exoKuiper belt Substructures (ARKS). Aims. We model local CO line profiles in the HD 121617 debris disc to investigate optical depth, CO mass, and
    Brennan, A. et al.

    Fecha de publicación:

    1
    2026
    Bibcode
    2026A&A...705A.201B
    Número de citas
    7