Two new long-period giant planets from the McDonald Observatory planet search and two stars with long-period radial velocity signals related to stellar activity cycles
- McDonald Observatory and Department of Astronomy, University of Texas at Austin, Austin, TX 78712 (United States)
- School of Physics and Australian Centre for Astrobiology, UNSW Australia, Sydney, NSW 2052 (Australia)
- Computational Engineering and Science Research Centre, University of Southern Queensland, Toowoomba, Queensland 4350 (Australia)
- NASA Exoplanet Science Institute and Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125 (United States)
- Department of Physics, Southern Connecticut State University, 501 Crescent St., New Haven, CT 06515 (United States)
- Physikalisches Institut, Center for Space and Habitability, University of Bern, CH-3012 Bern (Switzerland)
- NASA Ames Research Center, Moffett Field, CA 94035 (United States)
- National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719 (United States)
- Astrophysics Research Institute, Liverpool John Moores University, 146 Brownlow Hill, Liverpool, L3 5RF (United Kingdom)
We report the detection of two new long-period giant planets orbiting the stars HD 95872 and HD 162004 (ψ{sup 1} Dra B) by the McDonald Observatory planet search. The planet HD 95872b has a minimum mass of 4.6 M{sub Jup} and an orbital semimajor axis of 5.2 AU. The giant planet ψ{sup 1} Dra Bb has a minimum mass of 1.5 M{sub Jup} and an orbital semimajor axis of 4.4 AU. Both of these planets qualify as Jupiter analogs. These results are based on over one and a half decades of precise radial velocity (RV) measurements collected by our program using the McDonald Observatory Tull Coude spectrograph at the 2.7 m Harlan J. Smith Telescope. In the case of ψ{sup 1} Dra B we also detect a long-term nonlinear trend in our data that indicates the presence of an additional giant planet, similar to the Jupiter–Saturn pair. The primary of the binary star system, ψ{sup 1} Dra A, exhibits a very large amplitude RV variation due to another stellar companion. We detect this additional member using speckle imaging. We also report two cases—HD 10086 and HD 102870 (β Virginis)—of significant RV variation consistent with the presence of a planet, but that are probably caused by stellar activity, rather than reflexive Keplerian motion. These two cases stress the importance of monitoring the magnetic activity level of a target star, as long-term activity cycles can mimic the presence of a Jupiter-analog planet.
- OSTI ID:
- 22887063
- Journal Information:
- Astrophysical Journal, Vol. 818, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); Since 2009, the country of publication for this journal is the UK.; ISSN 0004-637X
- Country of Publication:
- United Kingdom
- Language:
- English
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