Erratum: “Standing on the Shoulders of Dwarfs: The Kepler Asteroseismic LEGACY Sample. I. Oscillation Mode Parameters” (2017, ApJ, 835, 172)

Abstract

The advent of space-based missions like Kepler has revolutionized the study of solar-type stars, particularly through the measurement and modeling of their resonant modes of oscillation. Here we analyze a sample of 66 Kepler main-sequence stars showing solar-like oscillations as part of the Kepler seismic LEGACY project. We use Kepler short-cadence data, of which each star has at least 12 months, to create frequency power spectra optimized for asteroseismology. For each star we identify its modes of oscillation and extract parameters such as frequency, amplitude, and line width using a Bayesian Markov chain Monte Carlo 'peak-bagging' approach. We report the extracted mode parameters for all 66 stars, as well as derived quantities such as frequency difference ratios, the large and small separations ∆ν and δν 02 ; the behavior of line widths with frequency and line widths at ν max with T eff , for which we derive parametrizations; and behavior of mode visibilities. These average properties can be applied in future peak-bagging exercises to better constrain the parameters of the stellar oscillation spectra. The frequencies and frequency ratios can tightly constrain the fundamental parameters of these solar-type stars, and mode line widths and amplitudes can test models of mode damping and excitation.

Frequency dependence of p-mode frequency shifts induced by magnetic activity in Kepler solar-like stars

“…Our initial sample consists in the 61 solar-like oscillating stars observed by Kepler analyzed in Appourchaux et al (2012) complemented by 26 dwarfs from the LEGACY sample of 66 stars in Lund et al (2017) and not included in Appourchaux et al (2012). These 87 stars containing main sequence and slightly more evolved stars are listed in Table 1, where the total length of the observations and the associated duty cycles are given as well.…”

“…The objective here is to make progress in the understanding of the physical mechanisms responsible for the perturbations inducing the variability of the p-mode oscillations with magnetic activity. We started with a sample of 87 solar-like pulsating stars observed by Kepler and for which the peak-fitting analysis of the individual modes can be found in the literature (Appourchaux et al 2012;Lund et al 2017). The reason for selecting this sample is threefold: (1) it allowed us to study stars from the three following categories depending to their seismic and spectroscopic properties: the simple stars, the F-type stars, and the mixedmode stars (for more details, see Appourchaux et al 2012); (2) the characterization of the individual modes of these stars is already available and their fundamental stellar properties determined (Mathur et al 2012;Metcalfe et al 2014;Creevey et al 2017;Silva Aguirre et al 2017); and (3) these stars were observed in short cadence (SC; for more details, see Gilliland et al 2010) for at least 1 yr.…”

Pulsating white dwarfs: new insights

“…6 The sound of the bells (their eigenfrequencies) does not depend on how the bells are rung (Baade, 1992). 7 Note, however, that in many cases the studies of solar-type pulsators seem to be limited to using the frequency separations and frequency maximum to derive the astrophysical parameters of the stars, using the so-called "scaling relations" (Lund et al, 2017). 8 However, the dependence of the period spacing on the thickness of the outer envelope of DA and DB WDs is generally weaker than its dependence upon the effective temperature and the stellar mass (Tassoul et al, 1990).…”

Calibrating damping rates with LEGACY* linewidths

“…The agreement between observations and models is very satisfactorily. Moreover, all 1D models have global stellar parameters determined from minimizing the differences between observed and adiabatically computed oscillation frequencies [14], calibrated max(p t ) values, depth-dependent functional forms of the turbulent-velocity anisotropy Φ and T − τ relations as suggested by 3D simulations [15,16].…”

“…We use LEGACY [14] linewidths and frequencies of selected solar-type Kepler stars, together with 3D hydrodynamical simulation results [15,16], for calibrating the global stellar and nonlocal convection parameters in 1D stability computations. Additionally to exploiting the seismic diagnostic of observed oscillation frequencies, linewidth measurements provide further diagnostic information about the physical processes prevailing in the outer superadiabatic boundary layers where convective transport becomes inefficient.…”