2012/07/11 by Nader Haghighipour, R. Paul Butler, Eugenio J. Rivera +2 · 1 citation
Physics and Astronomy · #Astronomy and Astrophysical Research #Scientific Research and Discoveries #Stellar, planetary, and galactic studies #astro-ph.EP
paper · pdf · doi:10.1088/0004-637x/756/1/91
published as ApJ, 756, article id.91 (2012) · 23 pages, 4 figures, 5 tables, accepted for publication in ApJ
arxiv created 2012/07/11 · openalex publication_date 2012/08/20 · arxiv updated 2015/06/05 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/31
Keck/HIRES precision radial velocities of HD 207832 indicate the presence of two Jovian-type planetary companions in Keplerian orbits around this G star. The planets have minimum masses of M sin i = 0.56 M Jup and 0.73 M Jup , with orbital periods of ∼162 and ∼1156 days, and eccentricities of 0.13 and 0.27, respectively. Strömgren b and y photometry reveals a clear stellar rotation signature of the host star with a period of 17.8 days, well separated from the period of the radial velocity variations, reinforcing their Keplerian origin. The values of the semimajor axes of the planets suggest that these objects have migrated from the region of giant planet formation to closer orbits. In order to examine the possibility of the existence of additional (small) planets in the system, we studied the orbital stability of hypothetical terrestrial-sized objects in the region between the two planets and interior to the orbit of the inner body. Results indicated that stable orbits exist only in a small region interior to planet b. However, the current observational data offer no evidence for the existence of additional objects in this system.