ASTEROSEISMOLOGY OF RED GIANTS FROM THE FIRST FOUR MONTHS OF<i>KEPLER</i>DATA: GLOBAL OSCILLATION PARAMETERS FOR 800 STARS

Huber, Daniel; Bedding, Timothy R.; Stello, Dennis; Mosser, B.; Mathur, S.; Kallinger, T.; Hekker, S.; Elsworth, Y.; Buzasi, Derek L.; Ridder, J. De; Gilliland, Ronald L.; Kjeldsen, H.; Chaplin, W. J.; García, Rafael A.; Hale, Steven J.; Preston, H. L.; White, T. R.; Borucki, W. J.; Christensen‐Dalsgaard, J.; Clarke, Bruce; Jenkins, Jon M.; Koch, David

doi:10.1088/0004-637x/723/2/1607

Cited by 199 publications

(296 citation statements)

References 72 publications

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“…The comparison between this figure and Fig. 10 in Huber et al (2010) indicates that predictions from theory are in good agreement with the observed behavior of δ ν 02 in RGB and red clump stars. For main sequence stars, the frequency separation δ ν 01 = (ν n,0 −2 ν n1 +ν n+1,0 )/2 has also been suggested as a good indicator of the evolutionary state (e.g.…”

Section: Diagnostic Power Of Red Giant Oscillation Spectrasupporting

confidence: 80%

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Adiabatic Solar-Like Oscillations in Red Giant Stars

Montalbán

Miglio

Noels

et al. 2011

Red Giants as Probes of the Structure and Evolution of the Milky Way

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Since the detection of non-radial solar-like oscillation modes in red giants with the CoRoT satellite, the interest in the asteroseismic properties of red giants and the link with their global properties and internal structure is substantially increasing. Moreover, more and more precise data are being collected with the space-based telescopes CoRoT and Kepler. In this paper we present a survey of the most relevant theoretical and observational results obtained up to now concerning the potential of solar-like oscillations in red giants. Structure and oscillation spectra of red giant modelsRed giants are cool stars with an extended and diluted convective envelope surrounding a dense core, which makes their structure and therefore their pulsation properties very different from those of the Sun. As in solar-like stars, however, their convective envelope can stochastically excite oscillation modes. The properties of oscillation modes depend on the behavior of the Brunt-Väisälä (N) and Lamb (S ℓ ) frequencies. In a first approximation we can describe the radial displacement due to the perturbation as:

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Section: Diagnostic Power Of Red Giant Oscillation Spectrasupporting

confidence: 80%

“…observational works based on CoRoT and Kepler satellite data Huber et al, 2010;Mosser et al, 2010;Carrier et al, 2010). In the domain of validity of the asymptotic approximation for pressure modes, the spectrum of p modes can be described by (e.g.…”

Section: Diagnostic Power Of Red Giant Oscillation Spectramentioning

confidence: 99%

Adiabatic Solar-Like Oscillations in Red Giant Stars

Montalbán

Miglio

Noels

et al. 2011

Red Giants as Probes of the Structure and Evolution of the Milky Way

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“…The star we study here (KIC 12008916) exhibits a very high SNR (Corsaro et al 2015) for the best modes of oscillation (> 250), but detections of individual oscillations are possible at much lower SNR (typically 8). In the absence of instrumental noise (including shot noise), the SNR of the pulsation spectrum is typically determined by the properties of the star (for pulsations, see Huber et al 2010 and background see Kallinger et al 2014). Instrumental noise is somewhat specific to each space mission but is in general a function of stellar magnitude, so that brighter stars have lower instrumental noise and hence higher SNR.…”

Section: The Power Spectrummentioning

confidence: 99%

Asteroseismology of red giants: From analysing light curves to estimating ages

Davies

Miglio

2016

Astron Nachr

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Asteroseismology has started to provide constraints on stellar properties that will be essential to accurately reconstruct the history of the Milky Way. Here we look at the information content in data sets representing current and future space missions (CoRoT, Kepler, K2, TESS, and PLATO) for red giant stars. We describe techniques for extracting the information in the frequency power spectrum and apply these techniques to Kepler data sets of different observing length to represent the different space missions. We demonstrate that for KIC 12008916, a low-luminosity red giant branch star, we can extract useful information from all data sets, and for all but the shortest data set we obtain good constraint on the g-mode period spacing and core rotation rates. We discuss how the high precision in these parameters will constrain the stellar properties of stellar radius, distance, mass and age. We show that high precision can be achieved in mass and hence age when values of the g-mode period spacing are available. We caution that tests to establish the accuracy of asteroseismic masses and ages are still "work in progress".

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“…We can compare our identification to the ε-values found in large samples of red giant stars, observed with the Kepler space telescope (e.g. Huber et al 2010;Corsaro et al 2012b). For these stars, we have a solid mode identification from uninterrupted data.…”

Section: Solar-like Oscillations In γ Pscmentioning

confidence: 84%

Detection of solar-like oscillations in the bright red giant starsγPiscium andθ¹ Tauri from a 190-day high-precision spectroscopic multi-site campaign

Beck

Kambe²,

Hillen

et al. 2015

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Context. Red giants are evolved stars that exhibit solar-like oscillations. Although a multitude of stars have been observed with space telescopes, only a handful of red giant stars were targets of spectroscopic asteroseismic observing projects. Aims. We search for solar-like oscillations in the two bright red giant stars γ Psc and θ 1 Tau from a time series of ground-based spectroscopy and determine the frequency of the excess of oscillation power ν max and the mean large frequency separation Δν for both stars. Seismic constraints on the stellar mass and radius will provide robust input for stellar modelling. Methods. The radial velocities of γ Psc and θ 1 Tau were monitored for 120 and 190 days, respectively. Nearly 9000 spectra were obtained. To reach accurate radial velocities, we used simultaneous thorium-argon and iodine-cell calibration of our optical spectra. In addition to the spectroscopy, we acquired interferometric observations of γ Psc for an independent estimate of the radius. We also analysed 22 days of observations of θ 1 Tau with the MOST satellite.Results. The frequency analysis of the radial velocity data of γ Psc revealed an excess of oscillation power around 32 μHz and a large frequency separation of 4.1 ± 0.1 μHz. θ 1 Tau exhibits oscillation power around 90 μHz, with a large frequency separation of 6.9 ± 0.2 μHz. Scaling relations indicate that γ Psc is a star of about 1 M and 10 R . The object θ 1 Tau appears to be a massive star of about 2.7 M and 10 R . The radial velocities of both stars were found to be modulated on timescales much longer than the oscillation periods. Conclusions. The estimated radii from seismology are in agreement with interferometric observations and also with estimates based on photometric data. While the mass of θ 1 Tau is in agreement with results from dynamical parallaxes, we find a lower mass for γ Psc than is found in the literature. The long periodic variability agrees with the expected timescales of rotational modulation.Key words. asteroseismology -stars: rotation -techniques: interferometric -techniques: spectroscopic -stars: general Based on observations made with the HERMES spectrograph mounted on the 1.2 m Mercator Telescope at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofsica de Canarias; the CORALIE spectrograph mounted on the 1.2 m Swiss telescope at La Silla Observatory, the HIDES spectrograph, mounted on the 1.9 m telescope at Okayama Astrophysical Observatory, NAOJ, the MOST space telescope, and and observations made with ESO Telescopes at the La Silla Paranal Observatory under program ID 086.D-0101.

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ASTEROSEISMOLOGY OF RED GIANTS FROM THE FIRST FOUR MONTHS OFKEPLERDATA: GLOBAL OSCILLATION PARAMETERS FOR 800 STARS

Cited by 199 publications

References 72 publications

Adiabatic Solar-Like Oscillations in Red Giant Stars

Adiabatic Solar-Like Oscillations in Red Giant Stars

Asteroseismology of red giants: From analysing light curves to estimating ages

Detection of solar-like oscillations in the bright red giant starsγPiscium andθ¹ Tauri from a 190-day high-precision spectroscopic multi-site campaign

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ASTEROSEISMOLOGY OF RED GIANTS FROM THE FIRST FOUR MONTHS OFKEPLERDATA: GLOBAL OSCILLATION PARAMETERS FOR 800 STARS

Cited by 199 publications

References 72 publications

Adiabatic Solar-Like Oscillations in Red Giant Stars

Adiabatic Solar-Like Oscillations in Red Giant Stars

Asteroseismology of red giants: From analysing light curves to estimating ages

Detection of solar-like oscillations in the bright red giant starsγPiscium andθ1 Tauri from a 190-day high-precision spectroscopic multi-site campaign

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Product

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Detection of solar-like oscillations in the bright red giant starsγPiscium andθ¹ Tauri from a 190-day high-precision spectroscopic multi-site campaign