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

  title={CoRoT Measures Solar-Like Oscillations and Granulation in Stars Hotter Than the Sun},
  author={Eric Michel and Annie Baglin and Michel Auvergne and Claude Catal{\`a} and R'eza Samadi and Frédéric Baudin and Thierry Appourchaux and Caroline Barban and Werner W. Weiss and Gabrielle Berthomieu and Patrick Boumier and M-A. Dupret and Rafael A. Garc{\'i}a and Malcolm Fridlund and Rafael Garrido and Marie Jo Goupil and Hans Kjeldsen and Yveline Lebreton and Beno{\^i}t Mosser and Arlette Grotsch-Noels and Eduardo Janot-Pacheco and Janine Provost and Ian W. Roxburgh and Anne Thoul and Thierry Toutain and Didier Tiphène and S. Turck-chi{\`e}ze and Sylvie D. Vauclair and G{\'e}rard Vauclair and Conny Aerts and G Alecian and J{\'e}r{\^o}me Ballot and St{\'e}phane Charpinet and Anne Marie Hubert and François Lignières and Ph. Mathias and M{\'a}rio J. P. F. G. Monteiro and Coralie Neiner and Ennio Poretti and Jos{\'e} R. de Medeiros and Ignasi Ribas and Michel Rieutord and Teodoro Roca Cortés and Konstanze Zwintz},
  pages={558 - 560}
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… 

Some highlights of the latest CoRoT results on stellar physics

  • S. Deheuvels
  • Physics, Geology
    Proceedings of the International Astronomical Union
  • 2013
Abstract Since its launch in December 2006, the CoRoT satellite has provided photometric data precise down to the micro-magnitude level for about 150 bright stars and 150 000 fainter ones. These

Solar-Like Oscillations in a Massive Star

Using data gathered by the Convection Rotation and Planetary Transits mission, the detection of solar-like oscillations in a massive star, V1449 Aql, which is a known large-amplitude (β Cephei) pulsator.


Sun-like stars show intensity fluctuations on a number of timescales due to various physical phenomena on their surfaces. These phenomena can convincingly be studied in the frequency spectra of these

CoRoT and Kepler results: Solar-like oscillators

Connections Between Stellar Oscillations and Turbulent Convection

Since the advent of space asteroseismology, enabled by the CoRoT and Kepler space-craft, solar-like oscillations have appeared to be a common feature of low-mass stars from the main-sequence to the

Asteroseismology of Solar-Type and Red-Giant Stars

We are entering a golden era for stellar physics driven by satellite and telescope observations of unprecedented quality and scope. New insights on stellar evolution and stellar interiors physics are

What does the Sun suggest about global oscillation amplitudes in solar-like stars

Motivated by the results of CoRoT and based on the solar experience, we develop a new stellar scaling law for the intensity-velocity amplitude ratio (gain) of resonant oscillations, which is a

Mode lifetimes of stellar oscillations - Implications for asteroseismology

Context. Successful inference from asteroseismology relies on at least two factors: that the oscillations in the stars have amplitudes large enough to be clearly observable, and that the oscillations


A large fraction of cool, low-mass stars exhibit brightness fluctuations that arise from a combination of convective granulation, acoustic oscillations, magnetic activity, and stellar rotation. Much

Amplitudes of solar-like oscillations: a new scaling relation

Solar-like oscillations are excited by near-surface convection and are being observed in growing numbers of stars using ground- and space-based telescopes. We have previously suggested an empirical



Solar-like oscillations in δ

Model computations of δ Scuti stars, located in the vicinity of the red edge of the classical instability strip, suggest amplitudes of solar-like oscillations larger than in cooler models located

Excitation of solar-like oscillations across the HR diagram

Aims. We extend semi-analytical computations of excitation rates for solar oscillation modes to those of other solar-like oscillating stars to compare them with recent observations Methods. Numerical

Amplitudes of Stellar Oscillations: The Implications for Asteroseismology

There are no good predictions for the amplitudes expected from solar-like oscillations in other stars. In the absence of a definitive model for convection, which is thought to be the mechanism that

Evidence for Granulation and Oscillations in Procyon from Photometry with the WIRE Satellite

We report evidence for the granulation signal in the star Procyon A, based on two photometric time series from the star tracker on the WIRE satellite. The power spectra show evidence of excess power

Solar-like Oscillations in Α Centauri B

We have made velocity observations of the star α Cen B from two sites, allowing us to identify 37 oscillation modes with l = 0–3. Fitting to these modes gives the large and small frequency

Solar-like Oscillations in α Centauri B

We have made velocity observations of the star α Centauri B from two sites, allowing us to identify 37 oscillation modes with l = 0-3. Fitting to these modes gives the large and small frequency


First results from the VIRGO experiment (Variability of solar IRradiance and Gravity Oscillations) on the ESA/NASA Mission SOHO (Solar and Heliospheric Observatory) are reported. The observations

A spectroscopic study of southern (candidate) gamma Doradus stars. II. Detailed abundance analysis and fundamental parameters

Context. The γ Doradus stars are a recent class of variable main sequence F-type stars located on the red edge of the Cepheid instability strip. They pulsate in gravity modes, and this makes them

Stellar Model Analysis of the Oscillation Spectrum of η Bootis Obtained from MOST

Eight consecutive low-frequency radial p-modes are identified in the G0 IV star η Bootis based on 27 days of ultraprecise rapid photometry obtained by the MOST (Microvariability and Oscillations of

Solar structure from global studies of the 5-minute oscillation

High sensitivity Doppier spectroscopy of integral sunlight in the 769.9 nm line of neutral potassium reveals several equally spaced lines of Q > 1,000 centred on the well known period of 5 min. These