On model predictions of the power spectral density of radial solar p modes

Chaplin, W. J.; Houdek, G.; Elsworth, Y.; Gough, D. O.; Isaak, G. R.; New, R.

doi:10.1111/j.1365-2966.2005.09041.x

Cited by 113 publications

(214 citation statements)

References 30 publications

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“…A detailed derivation of the solution can be found in Samadi & Goupil (2001, SG herefater) or in Chaplin et al (2005). We recall below the main steps.…”

Section: The Inhomogeneous Wave Equationmentioning

confidence: 99%

“…As an alternative to comparing theoretical results and observational data, Chaplin et al (2005) proposed to derive H from the theoretical excitation rates, P, and the observed mode line width, Γ , according to the relation:…”

Section: Seismic Constraintsmentioning

confidence: 99%

“…A few years later, Goldreich & Keeley (1977b, GK hereafter) have proposed the first theoretical model of stochastic excitation of acoustic modes by the Reynolds stress. Since this pioneering work, different improved models have been developed (Dolginov & Muslimov 1984;Balmforth 1992a;Goldreich et al 1994;Chaplin et al 2005;Samadi et al 2003a;Belkacem et al 2006bBelkacem et al , 2008. These approaches differ from each other either in the way turbulent convection is described or by the excitation process.…”

Section: Introductionmentioning

confidence: 99%

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Stochastic Excitation of Acoustic Modes in Stars

Samadi

2011

The Pulsations of the Sun and the Stars

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Abstract. For more than ten years, solar-like oscillations have been detected and frequencies measured for a growing number of stars with various characteristics (e.g. different evolutionary stages, effective temperatures, gravities, metal abundances ...).Excitation of such oscillations is attributed to turbulent convection and takes place in the uppermost part of the convective envelope. Since the pioneering work of Goldreich & Keely (1977), more sophisticated theoretical models of stochastic excitation were developed, which differ from each other both by the way turbulent convection is modelled and by the assumed sources of excitation. We review here these different models and their underlying approximations and assumptions.We emphasize how the computed mode excitation rates crucially depend on the way turbulent convection is described but also on the stratification and the metal abundance of the upper layers of the star. In turn we will show how the seismic measurements collected so far allow us to infer properties of turbulent convection in stars.

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“…A detailed derivation of the solution can be found in Samadi & Goupil (2001, SG herefater) or in Chaplin et al (2005). We recall below the main steps.…”

Section: The Inhomogeneous Wave Equationmentioning

confidence: 99%

Section: Seismic Constraintsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Stochastic Excitation of Acoustic Modes in Stars

Samadi

2011

The Pulsations of the Sun and the Stars

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“…Goldreich and Keeley 1977;Balmforth 1992;Houdek et al 1999;Chaplin et al 2005;Belkacem et al 2008;Houdek 2010). We refer to stars exhibiting such an oscillation pattern as solar-type stars hereafter.…”

Section: New Asteroseismic Diagnostics Of Global Stellar Convection mentioning

confidence: 99%

“…Goldreich and Keeley 1977;Balmforth 1992;Houdek et al 1999;Chaplin et al 2005;Belkacem et al 2008). The first observations of granulation are quite old (Herschel 1801), but it is not until 1933 that their turbulent origin was unveiled (Siedentopf 1933).…”

Section: Stellar Convection and The Background Signal In Oscillation mentioning

confidence: 99%

The Solar-Stellar Connection

Brun¹,

García²,

Houdek³

et al. 2017

Space Sciences Series of ISSI

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We discuss how recent advances in observations, theory and numerical simulations have allowed the stellar community to progress in its understanding of stellar convection, rotation and magnetism and to assess the degree to which the Sun and other stars share similar dynamical properties. Ensemble asteroseismology has become a reality with the advent of large time domain studies, especially from space missions. This new capability has provided improved constraints on stellar rotation and activity, over and above that obtained via traditional techniques such as spectropolarimetry or CaII H&K observations. New data and surveys covering large mass and age ranges have provided a wide parameter space to confront theories of stellar magnetism. These new empirical databases are complemented by theoretical advances and improved multi-D simulations of stellar dynamos. We trace these pathways through which a lucid and more detailed picture of magnetohydrodynamics of solar-like stars is beginning to emerge and discuss future prospects.

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The visibility of low‐frequency solar acoustic modes

et al. 2008

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We make predictions of the detectability of low-frequency p modes. Estimates of the powers and damping times of these low-frequency modes are found by extrapolating the observed powers and widths of higher-frequency modes with large observed signal-to-noise ratios. The extrapolations predict that the low-frequency modes will have small signal-to-noise ratios and narrow widths in a frequency-power spectrum. Monte Carlo simulations were then performed where timeseries containing mode signals and normally distributed Gaussian noise were produced. The mode signals were simulated to have the powers and damping times predicted by the extrapolations. Various statistical tests were then performed on the frequency-amplitude spectra formed from these timeseries to investigate the fraction of spectra in which the modes could be detected. The results of these simulations were then compared to the number of p-modes candidates observed in real Sun-as-a-star data at low frequencies. The fraction of simulated spectra in which modes were detected decreases rapidly as the frequency of modes decreases and so the fraction of simulations in which the low-frequency modes were detected was very small. However, increasing the signal-to-noise (S/N) ratio of the low-frequency modes by a factor of 2 above the extrapolated values led to significantly more detections. Therefore efforts should continue to further improve the quality of solar data that is currently available.Comment: 9 pages, 6 figures, accepted for publication in Astronomische Nachrichte

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On model predictions of the power spectral density of radial solar p modes

Cited by 113 publications

References 30 publications

Stochastic Excitation of Acoustic Modes in Stars

Stochastic Excitation of Acoustic Modes in Stars

The Solar-Stellar Connection

The visibility of low‐frequency solar acoustic modes

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