2015/05/22 by H. R. Coelho, Coelho, H. R., W. J. Chaplin +9
Physics and Astronomy · #FOS: Physical sciences #Solar and Stellar Astrophysics (astro-ph.SR) #astro-ph.SR
paper · pdf · doi:10.48550/arxiv.1505.06087
11 pages, 6 figures; accepted for publication in MNRAS
arxiv created 2015/05/22 · arxiv updated 2015/05/25
Large-scale analyses of stellar samples comprised of cool, solar-like oscillators now commonly utilize the so-called asteroseismic scaling relations to estimate fundamental stellar properties. In this paper we present a test of the scaling relation for the global asteroseismic parameter ν\rm max, the frequency at which a solar-like oscillator presents its strongest observed pulsation amplitude. The classic relation assumes that this characteristic frequency scales with a particular combination of surface gravity and effective temperature that also describes the dependence of the cut-off frequency for acoustic waves in an isothermal atmosphere, i.e., ν\rm max ∝ gT\rm eff-1/2. We test how well the oscillations of cool main-sequence and sub-giant stars adhere to this relation, using a sample of asteroseismic targets observed by the NASA Kepler Mission. Our results, which come from a grid-based analysis, rule out departures from the classic gT\rm eff-1/2 scaling dependence at the level of ≃ 1.5 \rm per cent over the full ≃ 1560 \rm K range in T\rm eff that we tested. There is some uncertainty over the absolute calibration of the scaling. However, any variation with T\rm eff is evidently small, with limits similar to those above.