Radial Velocity Variations of ADS 3085 A and B

Katoh Noriyuki, Itoh Yoichi, Sato Bun'ei

doi:10.32231/starsandgalaxies.1.0_39

Some observations have indicated that the binary frequency of pre-main-sequence stars is higher than that of main-sequence stars. Several hot jupiters which are gas planets with the orbital period of days are discovered in the main-sequence stars （e.g., Mayor & Queloz 1995）. Most of the main-sequence stars may be formed as the binary system. The difference of the binary rate between pre-main-sequence stars and main-sequence stars may be consistent with the frequency of the hot jupiter. We think that a binary formation correlates with a planet formation. Toyota et al. (2009) indicated that the standard deviations of the radial velocity of ADS 3085 A and ADS 3085 B are twice larger than the typical uncertainties of the velocities. The radial-velocity variation with the primary and secodary component may be caused by the orbital motion of the unknown companion object, respectively. We follow-up the radial velocities of ADS 3085 A and B from December 2007 to December 2009. We searched for the period of the radial velocity with the Lomb–Scargle algorithm (Scargle 1982). The radial velocities of ADS 3085 A and B may have the periodic variations with 7.7 d and 5.2 d, respectively. In both A and B, the cool spots on the surface of the star are moving with the stellar rotation because the chromospheric activity is active and the Hipparcos photometric data shows the magnitude variation. Since the radial velocity of ADS 3085 A strongly correlates with the chromospheric activity, the radial-velocity variation is caused by the stellar activity. In ADS 3085 B, although we do not show the correlation between radial-velocity variation and the chromospheric activity, the stellar activity may explains the radial-velocity variation.

Radial Velocity Variations of ADS 3085 A and B

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