Mixed modes in red-giant stars observed with CoRoT

By B. Mosser, C. Barban, J. Montalbán, P. Beck, A. Miglio, K. Belkacem, M. Goupil, S. Hekker, J. Ridder, M. Dupret and 8 more. 2011

158 citations recorded by the source corpus.

Context. The CoRoT mission has provided thousands of red-giant light curves. The analysis of their solar-like oscillations allows us to characterize their stellar properties. Aims. Up to now, the global seismic parameters of the pressure modes have been unable to distinguish red-clump giants from members of the red-giant branch. As recently done with Kepler red giants, we intend to analyze and use the so-called mixed modes to determine the evolutionary status of the red giants observed with CoRoT. We also aim at deriving different seismic characteristics depending on evolution. Methods. The complete identification of the pressure eigenmodes provided by the red-giant universal oscillation pattern allows us to aim at the mixed modes surrounding the l = 1 expected eigenfrequencies. A dedicated method based on the envelope autocorrelation function is proposed to analyze their period separation. Results. We have identified the mixed-mode signature separation thanks to their pattern that is compatible with the asymptotic law of gravity modes. We have shown that, independent of any modeling, the g-mode spacings help to distinguish the evolutionary status of a red-giant star. We then report the different seismic and fundamental properties of the stars, depending on their evolutionary status. In particular, we show that high-mass stars of the secondary clump present very specific seismic properties. We emphasize that stars belonging to the clump were affected by significant mass loss. We also note significant population and/or evolution differences in the different fields observed by CoRoT.

Subfields: Astronomy and Astrophysics, Education, Instrumentation

View Paper: https://www.semanticscholar.org/paper/daac34e88294fe850eac054db1b098e949358995

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Citations in the corpus

THE APOKASC CATALOG: AN ASTEROSEISMIC AND SPECTROSCOPIC JOINT SURVEY OF TARGETS IN THE KEPLER FIELDS (2014, methodology): “We associate a degree l to each extracted frequency based on a method similar to that provided by Mosser et al. (2011a).”
TESTING SCALING RELATIONS FOR SOLAR-LIKE OSCILLATIONS FROM THE MAIN SEQUENCE TO RED GIANTS USING KEPLER DATA (2011, methodology): “All amplitudes shown have been calculated using the method described by Kjeldsen et al. (2008) with c = 3.04 (Bedding et al. 2010) to convert to amplitude per radial mode.”
THE APOGEE RED-CLUMP CATALOG: PRECISE DISTANCES, VELOCITIES, AND HIGH-RESOLUTION ELEMENTAL ABUNDANCES OVER A LARGE AREA OF THE MILKY WAY'S DISK (2014, methodology): “Yellow and red points in the figure are stars in the APOKASC catalog for which the evolutionary state was measured by Stello et al. (2013) using the period spacings of gravity-mode stellar oscillations derived with two different methods (Bedding et al. 2011; Mosser et al. 2011).”
Asteroseismology of old open clusters with Kepler: direct estimate of the integrated red giant branch mass-loss in NGC 6791 and 6819 (2011, methodology): “Recent work by Montalbán et al. (2010), Bedding et al. (2011), and Mosser et al. (2011) has shown that the characteristics of the ℓ = 1 ridge in the échelle diagram can be used as an indicator of evolutionary state of low-mass giants.”
Mixed modes in red giants: a window on stellar evolution (2014, methodology): “These oscillations have been used to distinguish between stars that are burning only hydrogen in a thin shell around their cores and those that are additionally burning helium inside their cores (Bedding et al. 2011; Mosser et al. 2011a; Stello et al. 2013).”
Characterization of the power excess of solar-like oscillations in red giants with Kepler (2011, methodology): “(8) We have used the mean values e12 = −0.22, e20 = −0.065, e03 = 0.17, and e31 = 0.27 derived from the universal red giant oscillation pattern (Mosser et al. 2011b).”
Probing the core structure and evolution of red giants using gravity-dominated mixed modes observed with Kepler (2012, methodology): “Then, we used the so-called universal pattern to locate the short-lived radial and non-radial pressure modes very precisely (Mosser et al. 2011b).”
Galactic archaeology: mapping and dating stellar populations with asteroseismology of red-giant stars (2012, methodology): “For this work we adapted PARAM2 to include as additional observational constraints νmax, ∆ν and, when available, the evolutionary status of the star (core-Helium or hydrogen-shell burning phase), as determined by the period spacing of gravity-dominated modes (see Mosser et al. 2011).”
ASTEROSEISMIC CLASSIFICATION OF STELLAR POPULATIONS AMONG 13,000 RED GIANTS OBSERVED BY KEPLER (2013, methodology): “We associated the frequencies,ν, with radial or quadrupole (l = 0 and2) modes ifǫ − 0.3 < ν/∆ν mod1 < ǫ + 0.1, whereǫ was derived using the∆ν-ǫ relation fitted to red giant branch stars by Corsaro et al. (2012) based on the formula- tion by Mosser et al. (2011b) (Figure 1(b–d), shaded regions).”
Thermohaline instability and rotation-induced mixing - III. Grid of stellar models and asymptotic asteroseismic quantities from the pre-main sequence up to the AGB for low- and intermediate-mass stars of various metallicities (2012, background): “As proposed by Bedding et al. (2011) and Mosser et al. (2011), this quantity allows us to distinguish two stars that have the same luminosity, one being at the RGB bump and the other one being at the clump undergoing central He burning.”
Rotation and magnetism of Kepler pulsating solar-like stars : Towards asteroseismically calibrated age-rotation relations (2014, background): “With the advent of the detection of mixed modes in subgiant and giant stars (e.g. Beck et al. 2011; Bedding et al. 2011; Mosser et al. 2011; Stello et al. 2013; Benomar et al. 2013, 2014) – including some belonging to a few clusters (Stello et al. 2011; Basu et al. 2011) – it is now possible to…”
Asteroseismology of Solar-Type and Red-Giant Stars (2013, methodology): “Third, seismic data on RGB stars in principle provide robust ages that probe a wide age range: Once a star has evolved to the RGB its age is determined to a first approximation by the time spent in the core-hydrogen burning phase, which is predominantly a function of mass and metallicity.”
CALCULATING ASTEROSEISMIC DIAGRAMS FOR SOLAR-LIKE OSCILLATIONS (2011, methodology): “A similar analysis was done for CoRoT data by Mosser et al. (2011b).”
Spin down of the core rotation in red giants (2012, methodology): “With narrow filters centered on the expected ℓ = 1 pressure modes, it gives the spacing due to the mixed-mode pattern (Mosser et al. 2011a).”
The Updated BaSTI Stellar Evolution Models and Isochrones. I. Solar-scaled Calculations (2018, methodology): “This diagram have been used successfully to distinguish the shell hydrogen burning red giant stars with those that are fusing helium in the core along with the hydrogen in the shell (e.g., Bedding et al. 2011; Mosser et al. 2011).”