The HD 192263 system: planetary orbital period and stellar variability disentangled
Article
Article Title | The HD 192263 system: planetary orbital period and stellar variability disentangled |
---|---|
ERA Journal ID | 1057 |
Article Category | Article |
Authors | Dragomir, Diana (Author), Kane, Stephen R. (Author), Henry, Gregory W. (Author), Ciardi, David R. (Author), Fischer, Debra A. (Author), Howard, Andrew W. (Author), Jensen, Eric L N (Author), Laughlin, Gregory (Author), Mahadevan, Suvrath (Author), Matthews, Jaymie M. (Author), Pilyavsky, Genady (Author), von Braun, Kaspar (Author), Wang, Sharon X. (Author) and Wright, Jason T. (Author) |
Journal Title | The Astrophysical Journal: an international review of astronomy and astronomical physics |
Journal Citation | 754 (1), pp. 37-45 |
Article Number | 37 |
Number of Pages | 9 |
Year | 2012 |
Publisher | IOP Publishing |
Place of Publication | United States |
ISSN | 0004-637X |
1538-4357 | |
Digital Object Identifier (DOI) | https://doi.org/10.1088/0004-637X/754/1/37 |
Web Address (URL) | http://iopscience.iop.org/article/10.1088/0004-637X/754/1/37 |
Abstract | As part of the Transit Ephemeris Refinement and Monitoring Survey, we present new radial velocities and photometry of the HD192263 system. Our analysis of the already available Keck-HIRES and CORALIE radial velocity measurements together with the five new Keck measurements we report in this paper results in improved orbital parameters for the system. We derive constraints on the size and phase location of the transit window for HD192263b, a Jupiter-mass planet with a period of 24.3587 ± 0.0022days. We use 10years of Automated Photoelectric Telescope photometry to analyze the stellar variability and search for planetary transits. We find continuing evidence of spot activity with periods near 23.4days. The shape of the corresponding photometric variations changes over time, giving rise to not one but several Fourier peaks near this value. However, none of these frequencies coincides with the planet's orbital period and thus we find no evidence of star-planet interactions in the system. We attribute the ∼23day variability to stellar rotation. There are also indications of spot variations on longer (8years) timescales. Finally, we use the photometric data to exclude transits for a planet with the predicted radius of 1.09 RJ , and as small as 0.79 RJ. |
Keywords | planetary systems; stars: activity; individual stars (HD 192263); starspots; photometric techniques: radial velocities; |
Contains Sensitive Content | Does not contain sensitive content |
ANZSRC Field of Research 2020 | 510109. Stellar astronomy and planetary systems |
Public Notes | For access to this article, please click on the URL link provided. |
Byline Affiliations | University of British Columbia, Canada |
California Institute of Technology (Caltech), United States | |
Tennessee State University, United States | |
National Aeronautics and Space Administration (NASA), United States | |
Massey University, New Zealand | |
University of California, United States | |
Swarthmore College, United States | |
Pennsylvania State University, United States | |
Institution of Origin | University of Southern Queensland |
https://research.usq.edu.au/item/q4322/the-hd-192263-system-planetary-orbital-period-and-stellar-variability-disentangled
1235
total views67
total downloads4
views this month0
downloads this month