Oscillation mode linewidths and heights of 23 main-sequence stars observed by Kepler

T. Appourchaux, H. M. Antia, Othman Benomar, T. L. Campante, G. R. Davies, R. Handberg, R. Howe, C. Régulo, K. Belkacem, G. Houdek, R. A. García, W. J. Chaplin

Research output: Contribution to journalArticle

Abstract

Context. Solar-like oscillations have been observed by Kepler and CoRoT in many solar-type stars, thereby providing a way to probe the stars using asteroseismology. Aims. We provide the mode linewidths and mode heights of the oscillations of various stars as a function of frequency and of effective temperature. Methods. We used a time series of nearly two years of data for each star. The 23 stars observed belong to the simple or F-like category. The power spectra of the 23 main-sequence stars were analysed using both maximum likelihood estimators and Bayesian estimators, providing individual mode characteristics such as frequencies, linewidths, and mode heights. We study the source of systematic errors in the mode linewidths and mode heights, and we present a way to correct these errors with respect to a common reference fit. Results. Using the correction, we can explain all sources of systematic errors, which could be reduced to less than ±15% for mode linewidths and heights, and less than ±5% for amplitude, when compared to the reference fit. The effect of a different estimated stellar background and a different estimated splitting will provide frequency-dependent systematic errors that might affect the comparison with theoretical mode linewidth and mode height, therefore affecting the understanding of the physical nature of these parameters. All other sources of relative systematic errors are less dependent upon frequency. We also provide the dependence of the so-called linewidth dip in the middle of the observed frequency range as a function of effective temperature. We show that the depth of the dip decreases with increasing effective temperature. The dependence of the dip on effective temperature may imply that the mixing length parameter α or the convective flux may increase with effective temperature.

Original languageEnglish (US)
Article numberA20
JournalAstronomy and Astrophysics
Volume566
DOIs
StatePublished - Jan 1 2014

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main sequence stars
oscillation
oscillations
dip
systematic errors
temperature
stars
estimators
solar oscillations
probe
asteroseismology
time series
power spectra
frequency ranges
probes
parameter

Keywords

  • Asteroseismology
  • Methods: data analysis
  • Stars: interiors

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Appourchaux, T., Antia, H. M., Benomar, O., Campante, T. L., Davies, G. R., Handberg, R., ... Chaplin, W. J. (2014). Oscillation mode linewidths and heights of 23 main-sequence stars observed by Kepler. Astronomy and Astrophysics, 566, [A20]. https://doi.org/10.1051/0004-6361/201323317

Oscillation mode linewidths and heights of 23 main-sequence stars observed by Kepler. / Appourchaux, T.; Antia, H. M.; Benomar, Othman; Campante, T. L.; Davies, G. R.; Handberg, R.; Howe, R.; Régulo, C.; Belkacem, K.; Houdek, G.; García, R. A.; Chaplin, W. J.

In: Astronomy and Astrophysics, Vol. 566, A20, 01.01.2014.

Research output: Contribution to journalArticle

Appourchaux, T, Antia, HM, Benomar, O, Campante, TL, Davies, GR, Handberg, R, Howe, R, Régulo, C, Belkacem, K, Houdek, G, García, RA & Chaplin, WJ 2014, 'Oscillation mode linewidths and heights of 23 main-sequence stars observed by Kepler', Astronomy and Astrophysics, vol. 566, A20. https://doi.org/10.1051/0004-6361/201323317
Appourchaux T, Antia HM, Benomar O, Campante TL, Davies GR, Handberg R et al. Oscillation mode linewidths and heights of 23 main-sequence stars observed by Kepler. Astronomy and Astrophysics. 2014 Jan 1;566. A20. https://doi.org/10.1051/0004-6361/201323317
Appourchaux, T. ; Antia, H. M. ; Benomar, Othman ; Campante, T. L. ; Davies, G. R. ; Handberg, R. ; Howe, R. ; Régulo, C. ; Belkacem, K. ; Houdek, G. ; García, R. A. ; Chaplin, W. J. / Oscillation mode linewidths and heights of 23 main-sequence stars observed by Kepler. In: Astronomy and Astrophysics. 2014 ; Vol. 566.
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abstract = "Context. Solar-like oscillations have been observed by Kepler and CoRoT in many solar-type stars, thereby providing a way to probe the stars using asteroseismology. Aims. We provide the mode linewidths and mode heights of the oscillations of various stars as a function of frequency and of effective temperature. Methods. We used a time series of nearly two years of data for each star. The 23 stars observed belong to the simple or F-like category. The power spectra of the 23 main-sequence stars were analysed using both maximum likelihood estimators and Bayesian estimators, providing individual mode characteristics such as frequencies, linewidths, and mode heights. We study the source of systematic errors in the mode linewidths and mode heights, and we present a way to correct these errors with respect to a common reference fit. Results. Using the correction, we can explain all sources of systematic errors, which could be reduced to less than ±15{\%} for mode linewidths and heights, and less than ±5{\%} for amplitude, when compared to the reference fit. The effect of a different estimated stellar background and a different estimated splitting will provide frequency-dependent systematic errors that might affect the comparison with theoretical mode linewidth and mode height, therefore affecting the understanding of the physical nature of these parameters. All other sources of relative systematic errors are less dependent upon frequency. We also provide the dependence of the so-called linewidth dip in the middle of the observed frequency range as a function of effective temperature. We show that the depth of the dip decreases with increasing effective temperature. The dependence of the dip on effective temperature may imply that the mixing length parameter α or the convective flux may increase with effective temperature.",
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AU - Appourchaux, T.

AU - Antia, H. M.

AU - Benomar, Othman

AU - Campante, T. L.

AU - Davies, G. R.

AU - Handberg, R.

AU - Howe, R.

AU - Régulo, C.

AU - Belkacem, K.

AU - Houdek, G.

AU - García, R. A.

AU - Chaplin, W. J.

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N2 - Context. Solar-like oscillations have been observed by Kepler and CoRoT in many solar-type stars, thereby providing a way to probe the stars using asteroseismology. Aims. We provide the mode linewidths and mode heights of the oscillations of various stars as a function of frequency and of effective temperature. Methods. We used a time series of nearly two years of data for each star. The 23 stars observed belong to the simple or F-like category. The power spectra of the 23 main-sequence stars were analysed using both maximum likelihood estimators and Bayesian estimators, providing individual mode characteristics such as frequencies, linewidths, and mode heights. We study the source of systematic errors in the mode linewidths and mode heights, and we present a way to correct these errors with respect to a common reference fit. Results. Using the correction, we can explain all sources of systematic errors, which could be reduced to less than ±15% for mode linewidths and heights, and less than ±5% for amplitude, when compared to the reference fit. The effect of a different estimated stellar background and a different estimated splitting will provide frequency-dependent systematic errors that might affect the comparison with theoretical mode linewidth and mode height, therefore affecting the understanding of the physical nature of these parameters. All other sources of relative systematic errors are less dependent upon frequency. We also provide the dependence of the so-called linewidth dip in the middle of the observed frequency range as a function of effective temperature. We show that the depth of the dip decreases with increasing effective temperature. The dependence of the dip on effective temperature may imply that the mixing length parameter α or the convective flux may increase with effective temperature.

AB - Context. Solar-like oscillations have been observed by Kepler and CoRoT in many solar-type stars, thereby providing a way to probe the stars using asteroseismology. Aims. We provide the mode linewidths and mode heights of the oscillations of various stars as a function of frequency and of effective temperature. Methods. We used a time series of nearly two years of data for each star. The 23 stars observed belong to the simple or F-like category. The power spectra of the 23 main-sequence stars were analysed using both maximum likelihood estimators and Bayesian estimators, providing individual mode characteristics such as frequencies, linewidths, and mode heights. We study the source of systematic errors in the mode linewidths and mode heights, and we present a way to correct these errors with respect to a common reference fit. Results. Using the correction, we can explain all sources of systematic errors, which could be reduced to less than ±15% for mode linewidths and heights, and less than ±5% for amplitude, when compared to the reference fit. The effect of a different estimated stellar background and a different estimated splitting will provide frequency-dependent systematic errors that might affect the comparison with theoretical mode linewidth and mode height, therefore affecting the understanding of the physical nature of these parameters. All other sources of relative systematic errors are less dependent upon frequency. We also provide the dependence of the so-called linewidth dip in the middle of the observed frequency range as a function of effective temperature. We show that the depth of the dip decreases with increasing effective temperature. The dependence of the dip on effective temperature may imply that the mixing length parameter α or the convective flux may increase with effective temperature.

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