Oscillating red giants in the CoRoT exofield: asteroseismic mass and radius determination

By T. Kallinger, W. Weiss, C. Barban, F. Baudin, F. Carrier, C. Cameron, J. Ridder, M. Goupil, M. Gruberbauer, A. Hatzes and 3 more. 2008

141 citations recorded by the source corpus.

Context. Observations and analysis of solar-type oscillations in red-giant stars is an emerging aspect of asteroseismic analysis with a number of open questions yet to be explored. Although stochastic oscillations have previously been detected in red giants from both radial velocity and photometric measurements, those data were either too short or had sampling that was not complete enough to perform a detailed data analysis of the variability. The quality and quantity of photometric data as provided by the CoRoT satellite is necessary to provide a breakthrough in observing p-mode oscillations in red giants. We have analyzed continuous photometric time-series of about 11 400 relatively faint stars obtained in the exofield of CoRoT during the first 150 days long-run campaign from May to October 2007. We find several hundred stars showing a clear power excess in a frequency and amplitude range expected for red-giant pulsators. In this paper we present first results on a sub-sample of these stars. Aims. Knowing reliable fundamental parameters like mass and radius is essential for detailed asteroseismic studies of red-giant stars. As the CoRoT exofield targets are relatively faint (11−16 mag) there are no (or only weak) constraints on the stars’ location in the H-R diagram. We therefore aim to extract information about such fundamental parameters solely from the available time series. Methods. We model the convective background noise and the power excess hump due to pulsation with a global model fit and deduce reliable estimates for the stellar mass and radius from scaling relations for the frequency of maximum oscillation power and the characteristic frequency separation. Results. We provide a simple method to estimate stellar masses and radii for stars exhibiting solar-type oscillations. Our method is tested on a number of known solar-type pulsators.

Subfields: Astronomy and Astrophysics, Computational Mechanics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/7366f058559e40f0a0b17769a7b982c885be12d9

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In Astronomy and Astrophysics

1. D. Huber
2. D. Stello
3. W. Chaplin
4. D. Charbonneau
5. T. Bedding
6. B. Mosser
7. Timothy Morton
8. A. Miglio

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. T. Bedding
6. J. Southworth
7. A. Miglio
8. S. Hekker

Citations in the corpus

• TESTING SCALING RELATIONS FOR SOLAR-LIKE OSCILLATIONS FROM THE MAIN SEQUENCE TO RED GIANTS USING KEPLER DATA (2011, methodology): “…been used extensively both for the direct inference of stellar properties (e.g., Stello et al. 2009b; Kallinger et al. 2010a; Mosser et al. 2010; Kallinger et al. 2010b; Chaplin et al. 2011a; Hekker et al. 2011b,a; Silva Aguirre et al. 2011) as well as for calculating pulsation amplitudes of…”
• Asteroseismology of 16,000 Kepler Red Giants: Global Oscillation Parameters, Masses, and Radii (2018, methodology): “As pointed out by Kallinger et al. (2010b), we expect to see a small excess near R = 20.5 R , made up of stars in the AGB clump phase (Cassisi et al. 2001).”
• FUNDAMENTAL PROPERTIES OF KEPLER PLANET-CANDIDATE HOST STARS USING ASTEROSEISMOLOGY (2013, unknown): “Given an estimate of the effective temperature, Equations (1) and (2) can be used to calculate the mass and radius of a star (see, e.g., Kallinger et al. 2010b).”
• Gaia FGK benchmark stars: Effective temperatures and surface gravities (2015, methodology): “We compiled measurements of ∆ν for about half of our sample from the literature, starting from the references given in Bruntt et al. (2010) and Kallinger et al. (2010).”
• Red-giant seismic properties analyzed with CoRoT (2010, methodology): “From Table 1 of Kallinger et al. (2010) completed with a few other solar-targets benefitting from a precise modeling (HD 203608, Mosser et al. (2008); ι Hor, Teixeira et al. (2009); HD 52265, Ballot et al. (2010); HD 170987, Mathur et al. (2010a); HD 46375, Gaulme et al. (2010)), we can derive the e”
• The Updated BaSTI Stellar Evolution Models and Isochrones. I. Solar-scaled Calculations (2018, methodology): “…Teff , have been used to determine masses and radii of large samples of isolated stars, independent of modelling, thus providing strong constraints on stellar evolution models and on models of Galactic stellar populations (see, e.g., Kallinger et al. 2010; Chaplin et al. 2011; Miglio et al. 2012b).”
• Seismic diagnostics for transport of angular momentum in stars. I. Rotational splittings from the pre-main sequence to the red-giant branch. (2012, background): “Brown et al. 1991; Kallinger et al. 2010; Kjeldsen & Bedding 1995)”
• AN ANCIENT EXTRASOLAR SYSTEM WITH FIVE SUB-EARTH-SIZE PLANETS (2015, background): “Oscillation mode power is modulated by an envelope that generally assumes a Gaussian shape (Kallinger et al. 2010).”
• ASTEROSEISMOLOGY OF RED GIANTS FROM THE FIRST FOUR MONTHS OF KEPLER DATA: GLOBAL OSCILLATION PARAMETERS FOR 800 STARS (2010, methodology): “The effect is relatively small on the giant branch (Kallinger et al. 2010c), but more significant for less evolved stars.”
• The connection between stellar granulation and oscillation as seen by the Kepler mission (2014, methodology): “Whereas Kallinger et al. (2010b) fitted the same model to the same data, they did not arrive at the same νmax.”
• 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 .”
• SOLAR-LIKE OSCILLATIONS IN LOW-LUMINOSITY RED GIANTS: FIRST RESULTS FROM KEPLER (2010, background): “…(HST; Edmonds & Gilliland 1996; Gilliland 2008; Stello & Gilliland 2009), WIRE (Buzasi et al. 2000; Retter et al. 2003; Stello et al. 2008), Microvariability and Oscillations of Stars (MOST; Barban et al. 2007; Kallinger et al. 2008a,b), and Solar Mass Ejection Imager (SMEI; Tarrant et al. 2007).”
• KEPLER INPUT CATALOG: PHOTOMETRIC CALIBRATION AND STELLAR CLASSIFICATION (2011, methodology): “These authors used the method described by Kallinger et al. (2010) to estimate stellar masses and radii from the p-mode large frequency separation ∆ν, the frequency of maximum power νmax, and the KIC estimate of Teff .”
• Asteroseismology of red giants from the first four months of Kepler data: Fundamental stellar parameters (2010, methodology): “…long observations with the Convection, Rotation and planetary Transits satellite (CoRoT), which provided clear detections of radial and non- radial oscillation modes in numerous stars (De Ridder et al. 2009; Hekker et al. 2009; Carrier et al. 2010; Kallinger et al. 2010; Mosser et al. 2010).”
• FUNDAMENTAL PROPERTIES OF STARS USING ASTEROSEISMOLOGY FROM KEPLER AND CoRoT AND INTERFEROMETRY FROM THE CHARA ARRAY (2012, methodology): “Note that our PAVO campaign is also targeting solar-type oscillators in the CoRoT field in the galactic anti-center, such as the Fstar HD49933 (Appourchaux et al. 2008; Benomar et al. 2009; Kallinger et al. 2010a), which has already been subject to interferometric follow-up (Bigot et al. 2011).”
• Galactic archaeology: mapping and dating stellar populations with asteroseismology of red-giant stars (2012, methodology): “1 and 2 may be solved to derive M and R (see e.g. Stello et al. 2008; 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 .”