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Planet-Induced Emission Enhancements in HD 179949: Results from McDonald Observations

Published online by Cambridge University Press:  02 January 2013

L. Gurdemir ,
S. Redfield  and
M. Cuntz
L. Gurdemir
Affiliation:
Department of Physics, University of Texas at Arlington, Arlington, TX 76019, USA
S. Redfield
Affiliation:
Astronomy Department, Van Vleck Observatory, Wesleyan University, Middletown, CT 06459, USA
M. Cuntz*
Affiliation:
Department of Physics, University of Texas at Arlington, Arlington, TX 76019, USA
*
CCorresponding author. Email: [email protected]
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Abstract

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We monitored the Ca ii H and K lines of HD 179949, a notable star in the southern hemisphere, to observe and confirm previously identified planet induced emission (PIE) as an effect of star–planet interaction. We obtained high resolution spectra (R ∼ 53 000) with a signal-to-noise ratio S/N ≳ 50 in the Ca ii H and K cores during 10 nights of observation at the McDonald Observatory. Wide-band echelle spectra were taken using the 2.7-m telescope. Detailed statistical analysis of Ca ii K revealed fluctuations in the Ca II K core attributable to planet induced chromospheric emission. This result is consistent with previous studies by Shkolnik et al. (2003). Additionally, we were able to confirm the reality and temporal evolution of the phase shift of the maximum of star–planet interaction previously found. However, no identifiable fluctuations were detected in the Ca ii H core. The Al iλ3944 Å line was also monitored to gauge if the expected activity enhancements are confined to the chromospheric layer. Our observations revealed some variability, which is apparently unassociated with planet-induced activity.

Keywords

planet-star interactionsradiation mechanisms: nonthermalstars: activitystars: chromospheresstars: individual (HD 179949)stars: late-type
Type
Regular Papers
Information
Publications of the Astronomical Society of Australia , Volume 29 , Issue 2 , 2012 , pp. 141 - 149
Copyright
Copyright © Astronomical Society of Australia 2012

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