Red-giant seismic properties analyzed with CoRoT

By B. Mosser, K. Belkacem, M. Goupil, A. Miglio, T. Morel, C. Barban, F. Baudin, S. Hekker, R. Samadi, J. Ridder and 3 more. 2010

187 citations recorded by the source corpus.

Context. The CoRoT 5-month long observation runs provide us with the opportunity to analyze a large variety of red-giant stars and derive their fundamental parameters from their asteroseismic properties. Aims. We perform an analysis of more than 4600 CoRoT light curves to extract as much information as possible. We take into account the characteristics of both the star sample and the method to ensure that our asteroseismic results are as unbiased as possible. We also study and compare the properties of red giants in two opposite regions of the Galaxy. Methods. We analyze the time series using the envelope autocorrelation function to extract precise asteroseismic parameters with reliable error bars. We examine first the mean wide frequency separation of solar-like oscillations and the frequency of the maximum seismic amplitude, then the parameters of the excess power envelope. With the additional information of the effective temperature, we derive the stellar mass and radius. Results. We identify more than 1800 red giants among the 4600 light curves and obtain accurate distributions of the stellar parameters for about 930 targets. We are able to reliably measure the mass and radius of several hundred red giants. We derive precise information about the stellar population distribution and the red clump. By comparing the stars observed in two different fields, we find that the stellar asteroseismic properties are globally similar, but that the characteristics are different for red-clump stars. Conclusions. This study demonstrates the efficiency of statistical asteroseismology: validating scaling relations allows us to infer fundamental stellar parameters, derive precise information about red-giant evolution and interior structure, analyze and compare stellar populations from different fields.

Subfields: Astronomy and Astrophysics, Computational Mechanics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/21281d7372b45e388eea1ffb9fd9fc1f2b0f0cb3

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. D. Huber
2. I. Minchev
3. W. Chaplin
4. D. Stello
5. Joss Bland-Hawthorn
6. A. Miglio
7. A. Helmi
8. B. Mosser

In Computational Mechanics

1. D. Stello
2. Y. Elsworth
3. T. Bedding
4. D. Huber
5. S. Hekker
6. J. Ridder
7. T. Kallinger
8. K. Belkacem

In Instrumentation

1. D. Huber
2. D. Stello
3. W. Chaplin
4. B. Mosser
5. Joss Bland-Hawthorn
6. I. Minchev
7. T. Bedding
8. O. Gerhard

Citations in the corpus

• Asteroseismology of 16,000 Kepler Red Giants: Global Oscillation Parameters, Masses, and Radii (2018, methodology): “…Gilliland (2008) and Stello & Gilliland (2009) investigated the time series collected by the Hubble Space Telescope; Stello et al. (2008) worked with the star tracker of WIRE satellite; and Kallinger et al. (2010a) and Mosser et al. (2010) used data from the CoRoT telescope (Michel et al. 2008).”
• FUNDAMENTAL PROPERTIES OF STARS USING ASTEROSEISMOLOGY FROM KEPLER AND CoRoT AND INTERFEROMETRY FROM THE CHARA ARRAY (2012, background): “It is well known that the scaling relation for ∆ν is on more solid ground than the scaling relation for νmax, which only recently has been studied in more detail observationally (see, e.g., Stello et al. 2009a; Mosser et al. 2010; White et al. 2011) and theoretically (Belkacem et al. 2011).”
• Age determination for 269 Gaia DR2 open clusters (2019, background): “These quantities, combined with the effective temperature, can be used to derive stellar masses through the so-call scaling relations (see, e.g., Kallinger et al. 2010 and Mosser et al. 2010).”
• Asteroseismology of old open clusters with Kepler: direct estimate of the integrated red giant branch mass-loss in NGC 6791 and 6819 (2011, background): “1 and 2 may be solved to derive M and R (see e.g. Kallinger et al. 2010; Mosser et al. 2010): M M⊙ ≃ ( νmax νmax,⊙ )3 ( ∆ν ∆ν⊙ )−4 ( Teff Teff,⊙ )3/2 (3) R R⊙ ≃ ( νmax νmax,⊙ )( ∆ν ∆ν⊙ )−2( Teff Teff,⊙ )1/2 .”
• Characterization of the power excess of solar-like oscillations in red giants with Kepler (2011, background): “The role of the stellar mass is potentially important since the mass distribution is degenerate with νmax (Mosser et al. 2010).”
• FUNDAMENTAL PROPERTIES OF KEPLER PLANET-CANDIDATE HOST STARS USING ASTEROSEISMOLOGY (2013, unknown): “…of Kepler and CoRoT stars and by comparing derived radii and masses to evolutionary tracks and synthetic stellar populations (Hekker et al. 2009; Miglio et al. 2009; Kallinger et al. 2010a; Huber et al. 2010; Mosser et al. 2010; Huber et al. 2011; Silva Aguirre et al. 2011; Miglio et al. 2012b).”
• The universal red-giant oscillation pattern; an automated determination with CoRoT data (2010, methodology): “The new era of the spaceborne missions CoRoT andKepler has dramatically increased the amount and quality of the available asteroseismic data of red giants (Hekker et al. 2009; Bedding et al. 2010a; Mosser et al. 2010; Huber et al. 2010).”
• Mixed modes in red-giant stars observed with CoRoT (2011, methodology): “The number of detections of solar-like oscillation towardsthe anticenter direction is lower than towards the center, due to a lower red-giant density in the outer galactic regions and toimmer magnitudes (Mosser et al. 2010).”
• Probing the core structure and evolution of red giants using gravity-dominated mixed modes observed with Kepler (2012, methodology): “…we were also mindful of the need to include stars with a wide range of masses, the mass being estimated from the asteroseismic scaling relation, as in Mosser et al. (2010), and using the effective temperature given in the Kepler Input Catalog (Brown et al. 2011).150 As shown below in Fig.”
• The underlying physical meaning of the νmax νc relation (2011, background): “More recently, the space-missions CoRoT and Kepler confirmed those results by providing accurate and homogeneous measurements for a large sample of stars from red giants to main-sequence stars (e.g., Mosser et al. 2010).”
• Red giant masses and ages derived from carbon and nitrogen abundances (2015, unknown): “…et al. 2010), and now K2 space missions, solar-like oscillations have been detected in thousands of red giants (e.g. De Ridder et al. 2009; Hekker et al. 2009, 2011; Bedding et al. 2010; Mosser et al. 2010; Stello et al. 2013, 2015), for stars up to 8 kpc from the Sun (Miglio et al. 2013a).”
• THE APOKASC CATALOG: AN ASTEROSEISMIC AND SPECTROSCOPIC JOINT SURVEY OF TARGETS IN THE KEPLER FIELDS (2014, unknown): “We observed all Kepler Objects of Interest, or KOIs, that fit our magnitude and color cuts, all dwarfs within our magnitude range that had Teff < 5500 K, and selected targets observed by the CoRoT satellite (Mosser et al. 2010).”
• Ages and fundamental properties of Kepler exoplanet host stars from asteroseismology (2015, methodology): “These techniques have been extensively used in characterisation of the CoRoT and Kepler samples (e.g., Mosser et al. 2010; Huber et al. 2014), studies of open clusters (e.g., Basu et al. 2011; Stello et al. 2011), galactic archaeology (e.g., Miglio et al. 2013b; Casagrande et al. 2014), and will…”
• THE RADIAL VELOCITY EXPERIMENT (RAVE): FIFTH DATA RELEASE (2013, methodology): “ASTEROSEISMICALLY CALIBRATED RED GIANT CATALOG Asteroseismic data provide a very accurate way to determine surface gravities of red giant stars (e.g., Stello et al. 2008; Mosser et al. 2010; Bedding et al. 2011).”
• ASTEROSEISMOLOGY OF RED GIANTS FROM THE FIRST FOUR MONTHS OF KEPLER DATA: GLOBAL OSCILLATION PARAMETERS FOR 800 STARS (2010, methodology): “As can be seen in Table 1, there is good agreement between the results of different methods, as well as with the result by Mosser et al. (2010) that was based on CoRoT stars with νmax < 100µHz.”
• Spin down of the core rotation in red giants (2012, background): “Specific features of solar-like oscillations in red giants have been characterized (e.g. Bedding et al. 2010; Mosser et al. 2010; Huber et al. 2010).50 Mixed modes, which correspond to the coupling of gravity waves in the radiative core region and pressure waves in the envelope (Dziembowski et al.…”
• Asteroseismology of red giants from the first four months of Kepler data: Fundamental stellar parameters (2010, methodology): “We refer to Huber et al. (2010) who report on the signature of secondary-clump stars in the distributions of the seismic observables of red giants in theKepler field of view (see also Mosser et al. 2010 for CoRoT red giants).”
• Galactic archaeology: mapping and dating stellar populations with asteroseismology of red-giant stars (2012, methodology): “Moreover, as discussed in detail in Mosser et al. (2010), since no significant bias in the distribution of the targets is present in the νmax range between 6 µHz and 80 µHz, we only considered observed and simulated stars with νmax in this frequency range.”
• TESTING SCALING RELATIONS FOR SOLAR-LIKE OSCILLATIONS FROM THE MAIN SEQUENCE TO RED GIANTS USING KEPLER DATA (2011, methodology): “…et al. 1999a; Houdek 2006; Samadi et al. 2007), as well as observationally using red-giant stars (Gilliland 2008; Dziembowski & Soszyński 2010; Mosser et al. 2010; Stello et al. 2010), main-sequence stars (Verner et al. 2011a) and an ensemble of main-sequence and red-giant stars (Baudin et…”