Radial velocity study of the CP star Epsilon Ursae Majoris

Details Radial velocity study of the CP star Epsilon Ursae Majoris Radial velocity study of the CP star Epsilon Ursae Majoris

2009-04-23

arxiv.org/abs/0904.3562v1

Mon.Not.Roy.Astron.Soc.385:L1,2008

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

5 pages, 3 figures, accepted by MNRAS

Scientific paper

10.1111/j.1745-3933.2008.00419.x

In this Letter, the radial velocity variability of the chemically peculiar star Epsilon Ursae Majoris ($\epsilon$ UMa) from the sharp cores of the hydrogen lines is investigated. This study is based on the ELODIE archival data obtained at different phases of the rotational cycle. The star exhibits low-amplitude radial velocity variations with a period of P=5.0887 d. The best Keplerian solution yields an eccentricity e=0.503 and a minimum mass ~14.7$M_{\rm Jup}$ on the hypothesis that the rotational axis of $\epsilon$ UMa is perpendicular to the orbital plane. This result indicate that the companion is the brown-dwarf with the projected semi-amplitude variation of the radial velocity $K_{\rm 2}$=135.9 km/sec and the sine of inclination times semi-major axis $a_{2}$sin(i)=0.055 au.

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