TESTING SCALING RELATIONS FOR SOLAR-LIKE OSCILLATIONS FROM THE MAIN SEQUENCE TO RED GIANTS USING KEPLER DATA

By D. Huber, T. Bedding, D. Stello, S. Hekker, S. Mathur, B. Mosser, G. Verner, Alfio M. Bonanno, D. Buzasi, T. Campante and 22 more. 2011

256 citations recorded by the source corpus.

We have analyzed solar-like oscillations in ∼1700 stars observed by the Kepler Mission, spanning from the main sequence to the red clump. Using evolutionary models, we test asteroseismic scaling relations for the frequency of maximum power (νmax), the large frequency separation (Δν), and oscillation amplitudes. We show that the difference of the Δν–νmax relation for unevolved and evolved stars can be explained by different distributions in effective temperature and stellar mass, in agreement with what is expected from scaling relations. For oscillation amplitudes, we show that neither (L/M)s scaling nor the revised scaling relation by Kjeldsen & Bedding is accurate for red-giant stars, and demonstrate that a revised scaling relation with a separate luminosity-mass dependence can be used to calculate amplitudes from the main sequence to red giants to a precision of ∼25%. The residuals show an offset particularly for unevolved stars, suggesting that an additional physical dependency is necessary to fully reproduce the observed amplitudes. We investigate correlations between amplitudes and stellar activity, and find evidence that the effect of amplitude suppression is most pronounced for subgiant stars. Finally, we test the location of the cool edge of the instability strip in the Hertzsprung–Russell diagram using solar-like oscillations and find the detections in the hottest stars compatible with a domain of hybrid stochastically excited and opacity driven pulsation.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/8b1664bcb2b9ce5bf8774d8ec071f94e21630e23

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In Astronomy and Astrophysics

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

In Instrumentation

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

Citations in the corpus

• THE APOKASC CATALOG: AN ASTEROSEISMIC AND SPECTROSCOPIC JOINT SURVEY OF TARGETS IN THE KEPLER FIELDS (2014, background): “Global properties of the oscillations, such as the large frequency spacing ∆ν and frequency of maximum oscillation power νmax, are naturally related to the stellar mean density and surface gravity, respectively (Kjeldsen & Bedding 1995); see also Stello et al. (2009b) and Huber et al. (2011).”
• THE AGE AND MASS OF THE α HERCULIS TRIPLE-STAR SYSTEM FROM A MESA GRID OF ROTATING STARS WITH 1.3 ⩽ M/M☉ ⩽ 8.0 (2013, methodology): “Based on this fact, we earlier estimated the mass of this star to be 2.5+1.6 −1.1M⊙ (Moravveji et al. 2011) using the asteroseismic mass and radius scaling laws (Huber et al. 2011).”
• FUNDAMENTAL PROPERTIES OF STARS USING ASTEROSEISMOLOGY FROM KEPLER AND CoRoT AND INTERFEROMETRY FROM THE CHARA ARRAY (2012, methodology): “The analysis by Huber et al. (2011) was based on data spanning from Q0-6, which in most cases was sufficient to resolve the modes and reliably estimate νmax and ∆ν (Hekker et al. 2012).”
• Ages and fundamental properties of Kepler exoplanet host stars from asteroseismology (2015, methodology): “The theoretical νmax value can only be obtained using equation 12, and we adopt for the reference solar value entering this equation νmax, = 3090±30 µHz given by Huber et al. (2011).”
• Standing on the Shoulders of Dwarfs: the Kepler Asteroseismic LEGACY Sample. I. Oscillation Mode Parameters (2016, methodology): “Overall we see a reasonable agreement with a scatter within approximately 25% as also found by Huber et al. (2011).”
• 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, methodology): “Finally, the value of maximum oscillation amplitude relative to that of the Sun (Amax/Amax, ) is computed using the relation (e.g. Huber et al. 2011) Amax/Amax, = (L/L )s (M/M )t ( Teff Teff, )−r , (10) for the solar value from Kepler Amax, = 2.5 ppm.”
• Asteroseismology of 16,000 Kepler Red Giants: Global Oscillation Parameters, Masses, and Radii (2018, methodology): “Our final sample thus includes 133 stars from Hekker et al. (2011a), 336 stars from Huber et al. (2011a), 12,975 stars from Stello et al. (2013), 705 stars from Huber et al. (2014), 606 stars from Mathur et al. (2016), and 1339 stars from Yu et al. (2016).”
• Characterization of the power excess of solar-like oscillations in red giants with Kepler (2011, background): “As a consequence, this theoretical relation largely overestimates the observed bolometric radial amplitudes, as also shown by Huber et al. (2011) and Stello et al. (2011).”
• 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).”
• Spin down of the core rotation in red giants (2012, background): “Previous work on field star asteroseismic surveys shows that is possible to define evolutionary sequences (e.g. Miglio et al. 2009; Huber et al. 2011).”
• The connection between stellar granulation and oscillation as seen by the Kepler mission (2014, methodology): “…that show a clear power excess due to pulsation and which have already been used for other studies, such as the investigation of different seismic (Huber et al. 2010, 2011; Mosser et al. 2012a) and granulation (Mathur et al. 2011) observables, the seismic determination of fundamental parameters…”
• The Updated BaSTI Stellar Evolution Models and Isochrones. I. Solar-scaled Calculations (2018, unknown): “We adopted νmax,⊙ = 3090 µHz from Huber et al. (2011), Teff,⊙ = 5777 K, and M⊙ = 1.9891×1033 gm and R⊙ = 6.9599×1010 cm as used in the corresponding stellar tracks.”
• Binary Companions of Evolved Stars in APOGEE DR14: Search Method and Catalog of ∼5000 Companions (2018, background): “However, for RGB stars with glog 1< , these modes would likely have frequencies of νmax≈ 0.5–5 μHz (Garcia & Stello 2018), corresponding to periods of P ≈ 20–2 days and amplitudes of ≈20–200 m s−1 (Huber et al. 2011; Huber 2017).”
• Asteroseismology of Solar-Type and Red-Giant Stars (2013, background): “Initial results have been obtained from peak-bagging (e.g., Baudin et al. 2011, Appourchaux et al. 2012) and from other techniques (Huber et al. 2011b, Mosser et al. 2012a) developed from ground-based analysis methods (e.g., Kjeldsen et al. 2008), including results on stars in open clusters (Stello…”
• SEISMIC EVIDENCE FOR A RAPIDLY ROTATING CORE IN A LOWER-GIANT-BRANCH STAR OBSERVED WITH KEPLER (2012, background): “…of the star (large separation of p modes and frequency of the maximum amplitude) provide a significantly more precise estimate of the surface gravity through well-established scaling laws (Kjeldsen & Bedding 1995) which have recently been further validated from observations (Huber et al. 2011).”
• Confirming chemical clocks: asteroseismic age dissection of the Milky Way disc(s) (2017, unknown): “For our adopted set of asteroseismic observables, they correspond to 〈 ν 〉 = 135.1 µHz and νmax, = 3090 µHz (Huber et al. 2011).”