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A COMPREHENSIVE STATISTICAL ASSESSMENT OF STAR-PLANET INTERACTION

2015; IOP Publishing; Volume: 799; Issue: 2 Linguagem: Inglês

10.1088/0004-637x/799/2/163

1538-4357

Brendan P. Miller, Elena Gallo, Jason T. Wright, Elliott G. Pearson,

Astronomy and Astrophysical Research

We investigate whether magnetic interaction between close-in giant planets and their host stars produce observable statistical enhancements in stellar coronal or chromospheric activity. New Chandra observations of 12 nearby (d < 60 pc) planet-hosting solar analogs are combined with archival Chandra, XMM-Newton, and ROSAT coverage of 11 similar stars to construct a sample inoculated against inherent stellar class and planet-detection biases. Survival analysis and Bayesian regression methods (incorporating both measurements errors and X-ray upper limits; 13/23 stars have secure detections) are used to test whether "hot Jupiter" hosts are systematically more X-ray luminous than comparable stars with more distant or smaller planets. No significant correlations are present between common proxies for interaction strength (MP/a2 or 1/a) versus coronal activity (LX or LX/Lbol). In contrast, a sample of 198 FGK main-sequence stars does show a significant (∼99% confidence) increase in X-ray luminosity with MP/a2. While selection biases are incontrovertibly present within the main-sequence sample, we demonstrate that the effect is primarily driven by a handful of extreme hot-Jupiter systems with MP/a2 > 450 MJup AU−2, which here are all X-ray luminous but to a degree commensurate with their Ca ii H and K activity, in contrast to presented magnetic star–planet interaction scenarios that predict enhancements relatively larger in LX. We discuss these results in the context of cumulative tidal spin-up of stars hosting close-in gas giants (potentially followed by planetary infall and destruction). We also test our main-sequence sample for correlations between planetary properties and UV luminosity or Ca ii H and K emission, and find no significant dependence.