Asteroseismology of red giants from the first four months of Kepler data: Fundamental stellar parameters

By T. Kallinger, B. Mosser, S. Hekker, D. Huber, D. Stello, S. Mathur, S. Basu, T. Bedding, W. Chaplin, J. Ridder and 11 more. 2010

201 citations recorded by the source corpus.

Context. Clear power excess in a frequency range typical for solar-type oscillations in red giants has been detected in more than 1000 stars, which have been observed during the first 138 days of the science operation of the NASA Kepler satellite. This sample includes stars in a wide mass and radius range with spectral types G and K, extending in luminosity from the bottom of the giant branch up to high-luminous red giants, including the red bump and clump. The high-precision asteroseismic observations with Kepler provide a perfect source for testing stellar structure and evolutionary models, as well as investigating the stellar population in our Galaxy. Aims. We aim to extract accurate seismic parameters from the Kepler time series and use them to infer asteroseismic fundamental parameters from scaling relations and a comparison with red-giant models. Methods. We fit a global model to the observed power density spectra, which allows us to accurately estimate the granulation background signal and the global oscillation parameters, such as the frequency of maximum oscillation power. We find regular patterns of radial and non-radial oscillation modes and use a new technique to automatically identify the mode degree and the characteristic frequency separations between consecutive modes of the same spherical degree. In most cases, we can also measure the small separation between l = 0, 1, and 2 modes. Subsequently, the seismic parameters are used to estimate stellar masses and radii and to place the stars in an H-R diagram by using an extensive grid of stellar models that covers a wide parameter range. Using Bayesian techniques throughout our entire analysis allows us to determine reliable uncertainties for all parameters. Results. We provide accurate seismic parameters and their uncertainties for a large sample of red giants and determine their astero

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/dc9d5ce9b2bb6ed9a2b96ec12c89cb496f41c91d

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. Hans-Walter Rix
3. Jo Bovy
4. W. Chaplin
5. D. Stello
6. T. Bedding
7. B. Mosser
8. A. Miglio

In Instrumentation

1. D. Huber
2. D. Stello
3. Hans-Walter Rix
4. W. Chaplin
5. B. Mosser
6. Jo Bovy
7. T. Bedding
8. E. Gaidos

Citations in the corpus

• 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).”
• GYRE: An open-source stellar oscillation code based on a new Magnus Multiple Shooting Scheme (2013, background): “In their presentation of initial Kepler observations, Kallinger et al. (2010) discuss a distinct subpopulation of RGB stars which they identify as bump stars.”
• The Second APOKASC Catalog: The Empirical Approach (2018, methodology): “The CAN pipeline is described in Kallinger et al. (2010); the COR pipeline is described in Mosser & Appourchaux (2009); the OCT pipeline is described in Hekker et al. (2010); and the SYD pipeline is described in Huber et al. (2009).”
• Spin down of the core rotation in red giants (2012, background): “Important scaling relations have then been shown45 (Hekker et al. 2009) for deriving crucial information on the stellar mass and radius from global seismic parameters (Kallinger et al. 2010).”
• THE K2 ECLIPTIC PLANE INPUT CATALOG (EPIC) AND STELLAR CLASSIFICATIONS OF 138,600 TARGETS IN CAMPAIGNS 1–8 (2015, background): “K2 Asteroseismic Giants Stellar oscillations can be used to precisely measure fundamental properties in red giants with long-cadence data (e.g. Kallinger et al. 2010) and hence test derived stellar properties in the catalog.”
• THE APOKASC CATALOG: AN ASTEROSEISMIC AND SPECTROSCOPIC JOINT SURVEY OF TARGETS IN THE KEPLER FIELDS (2014, methodology): “Huber et al. (2010) described how the basic seismic parameters were measured; Kallinger et al. (2010) provided the stellar parameters, such as mass and radius; and Hekker et al. (2011b) compared different analysis techniques.”
• 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.”
• 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).”
• Red giant masses and ages derived from carbon and nitrogen abundances (2015, unknown): “Agescan then be inferred by comparing the seismic data to theoretical isochrones (e.g. Stello et al. 2009; Basu, Chaplin, & Elsworth 2010; Kallinger et al. 2010; Quirion, Christensen-Dalsgaard & Arentoft 2010; Casagrande et al. 2014), which leads to typical age uncertainties of the order of 30…”
• 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 Solar-Type and Red-Giant Stars (2013, background): “…data have yielded asteroseismic data of unprecented quality on stars in the red-giant phase (e.g., see Bedding et al. 2010, Huber et al. 2010, Kallinger et al. 2010, Hekker et al. 2011b), including giants in the open clusters NGC6791, NGC6819 and NGC6811 (Stello et al. 2011b; the clusters…”
• Mixed modes in red-giant stars observed with CoRoT (2011, background): “Thanks to the dramatic increase of information recently made available (De Ridder et al. 2009; Hekker et al. 2009; Mosser et al. 2010; Kallinger et al. 2010; Huber et al. 2010), we have now a precise view of pressure modes (p modes) corresponding to oscillations propagatingessentially in the large…”
• The universal red-giant oscillation pattern; an automated determination with CoRoT data (2010, background): “This accuracy, achieved without the need of stellar modeling (Kallinger et al. 2010), constitutes an important progress compared to the current photometric determination and demonstrates the power of asteroseismology.”
• 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).”
• REVISED STELLAR PROPERTIES OF KEPLER TARGETS FOR THE QUARTER 1–16 TRANSIT DETECTION RUN (2013, methodology): “We adopted an approach following Kallinger et al. (2010) and calculated for each star: LX = 1√ 2πσX exp (−(Xobs −Xmodel)2 2σ2X ) (2) where X = {Teff , log g, [Fe/H]} are assumed to be independent Gaussian observables.”
• 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): “This catalog contains stars in the Kepler field which have stellar parameters (mass, radius, and log g) determined from asteroseismology (e.g., Kallinger et al. 2010) and Teff and elemental abundances determined by APOGEE.”
• Probing the core structure and evolution of red giants using gravity-dominated mixed modes observed with Kepler (2012, methodology): “The data used are mainly Kepler long-cadence data that have been described in previous papers (e.g. 85 Jenkins et al. 2010; Bedding et al. 2010; Kallinger et al. 2010; Huber et al. 2010; Mathur et al. 2011b; Mosser et al. 2012, and references therein).”