Detection of Solar‐like Oscillations in the G5 Subgiant μ Her

Bonanno, A.; Benatti, S.; Claudi, R.; Desidera, S.; Gratton, R.; Leccia, S.; Paternò, L.

doi:10.1086/528946

Cited by 39 publications

(44 citation statements)

References 12 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…2), but observable from the northern hemisphere, can be found in the PASTEL catalogue. These are HD 73752 (HR 3430, [Fe/H] = 0.4, Luck & Heiter 2006), a close visual binary (5.4 and 6.8 mag, period of 123 yr, semi-major axis of 1.7 arcsec, Malkov et al 2012);HD 19994 (GJ 128) and HD 120136 (τ Boo, GJ 527), two planet-host visual binaries (semi-major axes 10 and 5 arcsec, Malkov et al 2012;Poveda et al 1994) Silva et al 2011), a star with asteroseismic data (Bonanno et al 2008), for which Baines et al (2014) measured an angular diameter of 1.96 ± 0.01 mas with the NPOI.…”

Section: Appendix A: Hr-diagrams For Individual Starsmentioning

confidence: 99%

GaiaFGK benchmark stars: Effective temperatures and surface gravities

Heiter

Jofré

Gustafsson

et al. 2015

A&A

282

414

View full text Add to dashboard Cite

Context. In the era of large Galactic stellar surveys, carefully calibrating and validating the data sets has become an important and integral part of the data analysis. Moreover, new generations of stellar atmosphere models and spectral line formation computations need to be subjected to benchmark tests to assess any progress in predicting stellar properties. Aims. We focus on cool stars and aim at establishing a sample of 34 Gaia FGK benchmark stars with a range of different metallicities. The goal was to determine the effective temperature and the surface gravity independently of spectroscopy and atmospheric models as far as possible. Most of the selected stars have been subjected to frequent spectroscopic investigations in the past, and almost all of them have previously been used as reference, calibration, or test objects. Methods. Fundamental determinations of T eff and log g were obtained in a systematic way from a compilation of angular diameter measurements and bolometric fluxes and from a homogeneous mass determination based on stellar evolution models. The derived parameters were compared to recent spectroscopic and photometric determinations and to gravity estimates based on seismic data. Results. Most of the adopted diameter measurements have formal uncertainties around 1%, which translate into uncertainties in effective temperature of 0.5%. The measurements of bolometric flux seem to be accurate to 5% or better, which contributes about 1% or less to the uncertainties in effective temperature. The comparisons of parameter determinations with the literature in general show good agreements with a few exceptions, most notably for the coolest stars and for metal-poor stars. Conclusions. The sample consists of 29 FGK-type stars and 5 M giants. Among the FGK stars, 21 have reliable parameters suitable for testing, validation, or calibration purposes. For four stars, future adjustments of the fundamental T eff are required, and for five stars the log g determination needs to be improved. Future extensions of the sample of Gaia FGK benchmark stars are required to fill gaps in parameter space, and we include a list of suggested candidates.

show abstract

Section: Appendix A: Hr-diagrams For Individual Starsmentioning

confidence: 99%

GaiaFGK benchmark stars: Effective temperatures and surface gravities

Heiter

Jofré

Gustafsson

et al. 2015

A&A

282

414

View full text Add to dashboard Cite

show abstract

“…Timeseries were prepared for asteroseismic analysis in the manner described by García et al (2011). Different teams attempted to detect, and then extract the basic properties of, the solar-like oscillations using automated analysis pipelines developed and extensively tested (e.g., see Bonanno et al 2008;Huber et al 2009;Mosser & Appourchaux 2009;Roxburgh 2009;Campante et al 2010;Hekker et al 2010;Mathur et al 2010) for application to the large ensemble of targets observed by Kepler. The basic results of this survey were presented in Chaplin et al (2011) and Verner et al (2011).…”

Section: δν δνmentioning

confidence: 99%

ASTEROSEISMIC FUNDAMENTAL PROPERTIES OF SOLAR-TYPE STARS OBSERVED BY THE NASA KEPLER MISSION

Chaplin

Basu

Huber

et al. 2013

ApJS

337

380

View full text Add to dashboard Cite

We use asteroseismic data obtained by the NASA Kepler mission to estimate the fundamental properties of more than 500 main-sequence and sub-giant stars. Data obtained during the first 10 months of Kepler science operations were used for this work, when these solar-type targets were observed for one month each in survey mode. Stellar properties have been estimated using two global asteroseismic parameters and complementary photometric and spectroscopic data. Homogeneous sets of effective temperatures, T eff , were available for the entire ensemble from complementary photometry; spectroscopic estimates of T eff and [Fe/H] were available from a homogeneous analysis of ground-based data on a subset of 87 stars. We adopt a grid-based analysis, coupling six pipeline codes to 11 stellar evolutionary grids. Through use of these different grid-pipeline combinations we allow implicitly for the impact on the results of stellar model dependencies from commonly used grids, and differences in adopted pipeline methodologies. By using just two global parameters as the seismic inputs we are able to perform a homogenous analysis of all solar-type stars in the asteroseismic cohort, including many targets for which it would not be possible to provide robust estimates of individual oscillation frequencies (due to a combination of low signal-to-noise ratio and short dataset lengths). The median final quoted uncertainties from consolidation of the grid-based analyses are for the full ensemble (spectroscopic subset) approximately 10.8% (5.4%) in mass, 4.4% (2.2%) in radius, 0.017 dex (0.010 dex) in log g, and 4.3% (2.8%) in mean density. Around 36% (57%) of the stars have final age uncertainties smaller than 1 Gyr. These ages will be useful for ensemble studies, but should be treated carefully on a star-bystar basis. Future analyses using individual oscillation frequencies will offer significant improvements on up to 150 stars, in particular for estimates of the ages, where having the individual frequency data is most important.

show abstract

“…ORK applied a procedure known as iterative sine-wave fitting (ISWF; e.g., Bedding et al 2007;Bonanno et al 2008;White et al 2010): it iteratively removes sinusoidal components from the data, which are identified as the maxima of the Fourier spectrum of the residuals. Since the number of oscillation modes present in the data is unknown a priori, the algorithm requires a stopping rule that associates some degree of confidence to the amplitude of each extracted sinusoidal component.…”

Section: Overview Of the Different Fitting Strategiesmentioning

confidence: 99%

Asteroseismology from multi-monthKeplerphotometry: the evolved Sun-like stars KIC 10273246 and KIC 10920273

Campante

Handberg

Mathur

et al. 2011

A&A

101

View full text Add to dashboard Cite

Context. The evolved main-sequence Sun-like stars KIC 10273246 (F-type) and KIC 10920273 (G-type) were observed with the NASA Kepler satellite for approximately ten months with a duty cycle in excess of 90%. Such continuous and long observations are unprecedented for solar-type stars other than the Sun. Aims. We aimed mainly at extracting estimates of p-mode frequencies -as well as of other individual mode parameters -from the power spectra of the light curves of both stars, thus providing scope for a full seismic characterization. Methods. The light curves were corrected for instrumental effects in a manner independent of the Kepler science pipeline. Estimation of individual mode parameters was based both on the maximization of the likelihood of a model describing the power spectrum and on a classic prewhitening method. Finally, we employed a procedure for selecting frequency lists to be used in stellar modeling. Results. A total of 30 and 21 modes of degree l = 0, 1, 2 -spanning at least eight radial orders -have been identified for KIC 10273246 and KIC 10920273, respectively. Two avoided crossings (l = 1 ridge) have been identified for KIC 10273246, whereas one avoided crossing plus another likely one have been identified for KIC 10920273. Good agreement is found between observed and predicted mode amplitudes for the F-type star KIC 10273246, based on a revised scaling relation. Estimates are given of the rotational periods, the parameters describing stellar granulation and the global asteroseismic parameters Δν and ν max .

show abstract

Detection of Solar‐like Oscillations in the G5 Subgiant μ Her

Cited by 39 publications

References 12 publications

GaiaFGK benchmark stars: Effective temperatures and surface gravities

GaiaFGK benchmark stars: Effective temperatures and surface gravities

ASTEROSEISMIC FUNDAMENTAL PROPERTIES OF SOLAR-TYPE STARS OBSERVED BY THE NASA KEPLER MISSION

Asteroseismology from multi-monthKeplerphotometry: the evolved Sun-like stars KIC 10273246 and KIC 10920273

Contact Info

Product

Resources

About