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RESEARCH ARTICLE
Contents Vol 29(2)

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

L. Gurdemir A , S. Redfield B and M. Cuntz A C
+ Author Affiliations
- Author Affiliations

A Department of Physics, University of Texas at Arlington, Arlington, TX 76019, USA

B Astronomy Department, Van Vleck Observatory, Wesleyan University, Middletown, CT 06459, USA

C Corresponding author. Email: cuntz@uta.edu

Australian Journal of Chemistry 29(2) 141-149 https://doi.org/10.1071/AS11074
Submitted: 17 December 2011  Accepted: 16 February 2012   Published: 2 April 2012

Abstract

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 i λ3944 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 interactions — radiation mechanisms: nonthermal — stars: activity — stars: chromospheres — stars: individual (HD 179949) — stars: late-type


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