Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011ess.....2.2012o&link_type=abstract
American Astronomical Society, ESS meeting #2, #20.12
Astronomy and Astrophysics
Astronomy
Scientific paper
In the framework of a Korean-Japanese planet search program, we have been carrying out a precise Doppler survey of about 190 G or K type giants to search for planets around intermediate-mass giants. The main purpose of this program is to show the properties of planetary systems around intermediate-mass stars by the survey using the 1.8m telescope at Bohyunsan Optical Astronomy Observatory in Korea, and the 1.88m telescope at Okayama Astrophysical Observatory in Japan.
In our presentation, we report a new planetary companion with a minimum mass of 1.8 MJupiter orbiting the giant star with 2.4 M&sun; at a semi-major axis of 0.77 AU. The planet is the lowest-mass planetary companion among those discovered around clump giant stars with masses of >1.9 M&sun;. Plotting this system and other known systems on semi-major axis vs. stellar mass diagram, it seems like that the distribution of planetary systems around 1.9-2.5 M&sun; stars may differ from those around other intermediate-mass stars. Almost all the planets orbiting 1.5-1.9 M&sun; stars are normal giant planets (1-6 MJupiter), and are located on orbits with semi-major axes of >1 AU. However, planets orbiting 1.9-2.5 M&sun; stars seem to be classified in two groups: normal giant planets at inner orbits (0.6-1.3 AU) and superplanets (6-13 MJupiter) at outer orbits (1.9-3 AU). Moreover, all planet-mass companions orbiting 2.5-3 M&sun; stars reside at semi-major axes larger than 1.9 AU, while all brown dwarf-mass companions are orbiting at semi-major axes less than 1.9 AU. In order to verify these properties and examine roles of the Type-II migration and other typical mechanisms on planet formation and evolution around intermediate-mass giant starss, it would be required to evaluate the semi-major axes distribution by further Doppler surveys.
Han Inwoo
Izumiura Hideyuki
Lee Bowon
Omiya Masashi
Sato Bun'ei
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