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

Huber, Daniel; Bedding, Timothy R.; Stello, Dennis; Hekker, S.; Mathur, S.; Mosser, B.; Verner, G. A.; Bonanno, A.; Buzasi, Derek L.; Campante, Tiago L.; Elsworth, Y.; Hale, Steven J.; Kallinger, T.; Aguirre, V. Silva; Chaplin, W. J.; Ridder, J. De; García, R. A.; Appourchaux, T.; Frandsen, S.; Houdek, G.; Molenda-Żakowicz, J.; Monteiro, M. J. P. F. G.; Christensen‐Dalsgaard, J.; Gilliland, Ronald L.; Kawaler, S. D.; Kjeldsen, H.; Broomhall, Anne-Marie; Corsaro, E.; Salabert, D.; Sanderfer, Dwight T.; Seader, S.; Smith, J. C.

doi:10.1088/0004-637x/743/2/143

Cited by 340 publications

(295 citation statements)

References 84 publications

(122 reference statements)

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“…Huber et al 2011;Hekker et al 2011;Kallinger et al 2010b;Mosser et al 2012a), studies of individual stars in a close binary grant us additional insight into the structure of the primary as well as the interaction between the binary system components. As a proof-ofconcept of what such objects have to offer compared to single pulsators, we organised a spectroscopic campaign on the heartbeat star with the richest oscillation pattern, KIC 5006817.…”

Section: Case Study Of Kic 5006817mentioning

confidence: 99%

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Pulsating red giant stars in eccentric binary systems discovered fromKeplerspace-based photometry

Beck

Hambleton

Vos

et al. 2014

A&A

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133

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Context. The unparalleled photometric data obtained by NASA's Kepler Space Telescope has led to improved understanding of red giant stars and binary stars. Seismology allows us to constrain the properties of red giants. In addition to eclipsing binaries, eccentric non-eclipsing binaries that exhibit ellipsoidal modulations have been detected with Kepler. Aims. We aim to study the properties of eccentric binary systems containing a red giant star and to derive the parameters of the primary giant component. Methods. We applied asteroseismic techniques to determine the masses and radii of the primary component of each system. For a selected target, light and radial velocity curve modelling techniques were applied to extract the parameters of the system and its primary component. Stellar evolution and its effects on the evolution of the binary system were studied from theoretical models. Results. The paper presents the asteroseismic analysis of 18 pulsating red giants in eccentric binary systems, for which masses and radii were constrained. The orbital periods of these systems range from 20 to 440 days. The results of our ongoing radial velocity monitoring programme with the Hermes spectrograph reveal an eccentricity range of e = 0.2 to 0.76. As a case study we present a detailed analysis of KIC 5006817, whose rich oscillation spectrum allows for detailed seismic analysis. From seismology we constrain the rotational period of the envelope to be at least 165 d, which is roughly twice the orbital period. The stellar core rotates 13 times faster than the surface. From the spectrum and radial velocities we expect that the Doppler beaming signal should have a maximum amplitude of 300 ppm in the light curve. Fixing the mass and radius to the asteroseismically determined values, we find from our binary modelling a value of the gravity darkening exponent that is significantly larger than expected. Through binary modelling, we determine the mass of the secondary component to be 0.29 ± 0.03 M . Conclusions. For KIC 5006817 we exclude pseudo-synchronous rotation of the red giant with the orbit. The comparison of the results from seismology and modelling of the light curve shows a possible alignment of the rotational and orbital axis at the 2σ level. Red giant eccentric systems could be progenitors of cataclysmic variables and hot subdwarf B stars.

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Section: Case Study Of Kic 5006817mentioning

confidence: 99%

“…These relations have been applied in numerous papers since then (e.g. Kallinger et al 2010b;Huber et al 2011;Corsaro et al 2013). Results from scaling relations have recently been compared with results of independent methods.…”

Section: Fig 1 Five Examples Ofmentioning

confidence: 99%

Pulsating red giant stars in eccentric binary systems discovered fromKeplerspace-based photometry

Beck

Hambleton

Vos

et al. 2014

A&A

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133

151

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“…with solar reference values from Huber et al (2011). Here r 1 and r 2 are the lower and upper boundaries of the evanescent zone,…”

Section: Red Giant Branchmentioning

confidence: 99%

“…We calculate n D and the frequency of maximum power n max using the scaling relations of Kjeldsen & Bedding (1995) with solar reference values from Huber et al (2011).…”

Section: Red Giant Branchmentioning

confidence: 99%

Asteroseismic Signatures of Evolving Internal Stellar Magnetic Fields

Cantiello

Fuller

Bildsten

2016

ApJ

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Recent asteroseismic analyses indicate the presence of strong (B  10 5 G) magnetic fields in the cores of many red giant stars. Here, we examine the implications of these results for the evolution of stellar magnetic fields, and we make predictions for future observations. Those stars with suppressed dipole modes indicative of strong core fields should exhibit moderate but detectable quadrupole mode suppression. The long magnetic diffusion times within stellar cores ensure that dynamo-generated fields are confined to mass coordinates within the main-sequence (MS) convective core, and the observed sharp increase in dipole mode suppression rates above 1.5 M e is likely explained by the larger convective core masses and faster rotation of these more massive stars. In clump stars, core fields of ∼10 5 G can suppress dipole modes, whose visibility should be equal to or less than the visibility of suppressed modes in ascending red giants. High dipole mode suppression rates in low-mass (M  2 M e ) clump stars would indicate that magnetic fields generated during the MS can withstand subsequent convective phases and survive into the compact remnant phase. Finally, we discuss implications for observed magnetic fields in white dwarfs and neutron stars, as well as the effects of magnetic fields in various types of pulsating stars.

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“…For low-mass stars, they are found in all evolutionary states, between the main sequence and horizontal branch of helium-core burning stars (e.g. Leighton et al 1962;Frandsen et al 2002;Carrier et al 2003;Hekker et al 2009;Chaplin et al 2011;Huber et al 2011;Kallinger et al 2012;Mosser et al 2013) and were even detected in the M5 A&A 573, A138 (2015) super giant α Her (Moravveji et al 2013). These very characteristic oscillations lead to a nearly regular spaced comb-like pattern in the power spectrum.…”

Section: Introductionmentioning

confidence: 99%

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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TESTING SCALING RELATIONS FOR SOLAR-LIKE OSCILLATIONS FROM THE MAIN SEQUENCE TO RED GIANTS USINGKEPLERDATA

Cited by 340 publications

References 84 publications

Pulsating red giant stars in eccentric binary systems discovered fromKeplerspace-based photometry

Pulsating red giant stars in eccentric binary systems discovered fromKeplerspace-based photometry

Asteroseismic Signatures of Evolving Internal Stellar Magnetic Fields

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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TESTING SCALING RELATIONS FOR SOLAR-LIKE OSCILLATIONS FROM THE MAIN SEQUENCE TO RED GIANTS USINGKEPLERDATA

Cited by 340 publications

References 84 publications

Pulsating red giant stars in eccentric binary systems discovered fromKeplerspace-based photometry

Pulsating red giant stars in eccentric binary systems discovered fromKeplerspace-based photometry

Asteroseismic Signatures of Evolving Internal Stellar Magnetic Fields

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