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Planetary companions orbiting M giants HD 208527 and HD 220074

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arxiv 1211.2051 v1 pith:SP4AAH7V submitted 2012-11-09 astro-ph.SR

B.-C. Lee , I. Han , M.-G. Park This is my paper · ORCID
classification astro-ph.SR
keywords planetarygiantsaroundbohyunsancompanioncompanionsexoplanetsmasses
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Aims. The purpose of the present study is to research the origin of planetary companions by using a precise radial velocity (RV) survey. Methods. The high-resolution spectroscopy of the fiber-fed Bohyunsan Observatory Echelle Spectrograph (BOES) at Bohyunsan Optical Astronomy Observatory (BOAO) is used from September 2008 to June 2012. Results. We report the detection of two exoplanets in orbit around HD 208527 and HD 220074 exhibiting periodic variations in RV of 875.5 +/- 5.8 and 672.1 +/- 3.7 days. The RV variations are not apparently related to the surface inhomogeneities and a Keplerian motion of the planetary companion is the most likely explanation. Assuming possible stellar masses of 1.6 +/- 0.4 and 1.2 +/- 0.3 M_Sun, we obtain the minimum masses for the exoplanets of 9.9 +/- 1.7 and 11.1 +/- 1.8 M_Jup around HD 208527 and HD 220074 with an orbital semi-major axis of 2.1 +/- 0.2 and 1.6 +/- 0.1 AU and an eccentricity of 0.08 and 0.14, respectively. We also find that the previously known spectral classification of HD 208527 and HD 220074 was in error: Our new estimation of stellar parameters suggest that both HD 208527 and HD 220074 are M giants. Therefore, HD 208527 and HD 220074 are so far the first candidate M giants to harbor a planetary companion.

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  1. Origin of the Long-Period Radial Velocity Variation in the Red Supergiant HD 216946 (V424 Lac)

    astro-ph.SR 2026-07 conditional novelty 5.0 of 10

    The 1365-day radial-velocity period of HD 216946 is probably caused by chromospheric activity and extended-atmosphere dynamics, not by a Keplerian companion.

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