Asteroseismic Investigation of Known Planet Hosts in the Kepler Field

Asteroseismic Investigation of Known Planet Hosts in the Kepler Field .a{background-color: #ffff88}.h{background-color: #ffff00}.b{background-color: #ccccff}.i{background-color: #3333ff}.c{background-color: #ffcccc}.j{background-color: #ff3333}.d{background-color: #bbffff}.k{background-color: #00ffff}.e{background-color: #ffdd77}.l{background-color: #ff6600}.f{background-color: #ccffaa}.m{background-color: #33ff00}.g{background-color: #ffccff}.n{background-color: #ff00ff} a:link {color: #0000ff} a.oa:link {color: #00a000} a:visited {color: #4000a0} a.oa:visited {color: #006666} a:hover {color: #ff0000} a.oa:hover {color: #cc33cc} In addition to its great potential for characterizing extra-solar planetary systems, the Kepler Mission is providing unique data on stellar oscillations. A key aspect of Kepler asteroseismology is the application to solar-like oscillations of main-sequence stars. As an example, we here consider an initial analysis of data for three stars in the Kepler field for which planetary transits were known from ground-based observations. For one of these, HAT-P-7, we obtain a detailed frequency spectrum and hence strong constraints on the stellar properties. The remaining two stars show definite evidence for solar-like oscillations, yielding a preliminary estimate of their mean densities.