Modeling of solar oscillation power spectra

Anderson, E.; Duvall, T. L.; Jefferies, S. M.

doi:10.1086/169452

Cited by 279 publications

(222 citation statements)

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“…nl . We choose the standard Lorentzian line profile (e.g., Anderson, Duvall, & Jefferies 1990) appropriate for describing an exponentially damped oscillator:…”

Section: Modeling Oscillation Power Spectramentioning

confidence: 99%

Determining the Inclination of the Rotation Axis of a Sun‐like Star

Gizon

Solanki

2003

ApJ

282

329

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Asteroseismology provides us with the possibility of determining the angle, i, between the direction of the rotation axis of a pulsating Sun-like star and the line of sight. A knowledge of i is important not just for obtaining improved stellar parameters, but also in order to determine the true masses of extrasolar planets detected from the radial velocity shifts of their central stars. By means of Monte Carlo simulations, we estimate the precision of the measurement of i and other stellar parameters. We find that the inclination angle can be retrieved accurately when ie30 for stars that rotate at least twice as fast as the Sun.

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“…nl . We choose the standard Lorentzian line profile (e.g., Anderson, Duvall, & Jefferies 1990) appropriate for describing an exponentially damped oscillator:…”

Section: Modeling Oscillation Power Spectramentioning

confidence: 99%

Determining the Inclination of the Rotation Axis of a Sun‐like Star

Gizon

Solanki

2003

ApJ

282

329

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“…In the limit of averaging over an infinite number of noise realizations, the peaks in the power spectrum tend toward Lorentzian profiles (Anderson et al 1990). This is typically known as the limit spectrum.…”

Section: Measuring Stellar Rotation With Keplermentioning

confidence: 99%

“…The likelihood was computed using a χ 2 probability density function as in Anderson et al (1990). We used the MCMC chains to compute the marginalized posterior distributions for each parameter, where we adopt the median of each distribution as a robust measure of the best-fit parameter value.…”

Section: Fittingmentioning

confidence: 99%

Differential Rotation in Sun-like Stars from Surface Variability and Asteroseismology

Nielsen

2017

Springer Theses

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“…Following, for example, the discussion in Anderson et al (1990), we relate these quantities to determine the solution, in the Fourier (frequency) domain, of the oscillator equation describing the behaviour of the p mode:…”

Section: Wwwan-journalorgmentioning

confidence: 99%

A framework for describing correlated excitation of solar p‐modes

2008

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In a previous paper we suggested that, for a given p mode, the excitation function is the same as the component of the solar background noise that has an identical surface spherical harmonic projection (over the corresponding range of temporal frequency). An important consequence of this surmise is that the excitation of overtones of a given angular degree and azimuthal order will be correlated in time. In this note, we introduce the basic principles and a mathematical description of correlated mode excitation. We use simple, illustrative examples, involving two modes. Our treatment suggests that in the real observations, any signatures of the correlation would not appear as a correlation of the output amplitudes of overtones, but rather as subtle modifications to the power spectral density at frequencies between the central frequencies of the overtones. These modifications give a contribution to the observed peak asymmetries.

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Modeling of solar oscillation power spectra

Cited by 279 publications

References 0 publications

Determining the Inclination of the Rotation Axis of a Sun‐like Star

Determining the Inclination of the Rotation Axis of a Sun‐like Star

Differential Rotation in Sun-like Stars from Surface Variability and Asteroseismology

A framework for describing correlated excitation of solar p‐modes

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