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X-ray Activity Variations and Coronal Abundances of the Star-Planet Interaction candidate HD 179949
Anshuman Acharya, Vinay L. Kashyap, Steven H. Saar, Kulinder Pal Singh, Manfred Cuntz
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We carry out detailed spectral and timing analyses of the Chandra X-ray data of HD 179949, a prototypical example of a star with a close-in giant planet with possible star-planet interaction (SPI) effects. We find a low coronal abundance A(Fe)/A(H)≈0.2 relative to the solar photospheric baseline of Anders & Grevesse (1989), and significantly lower than the stellar photosphere as well. We further find low abundances of high First Ionization Potential (FIP) elements A(O)/A(Fe)≲1, A(Ne)/A(Fe)≲0.1, but with indications of higher abundances of A(N)/A(Fe)≫1, A(Al)/A(Fe)≲10. We estimate a FIP bias for this star in the range ≈-0.3 to -0.1, larger than the ${\lesssim}-$0.5 expected for stars of this type, but similar to stars hosting close-in hot Jupiters. We detect significant intensity variability over time scales ranging from 100 s - 10 ks, and also evidence for spectral variability over time scales of 1-10 ks. We combine the Chandra flux measurements with Swift and XMM-Newton measurements to detect periodicities and determine that the dominant signal is tied to the stellar polar rotational period, consistent with expectations that the corona is rotational-pole dominated. We also find evidence for periodicity at both the planetary orbital frequency and at its beat frequency with the stellar polar rotational period, suggesting the presence of a magnetic connection between the planet and the stellar pole. If these periodicities represent an SPI signal, it is likely driven by a quasi-continuous form of heating (e.g., magnetic field stretching) rather than sporadic, hot, impulsive flare-like reconnections.
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