Spectroscopy of blue straggler stars in Galactic open cluster NGC 2682 (M67)
In this presentation, we report spectroscopic analysis of eight blue straggler stars (BSSs) and three turn-off stars (TOs) in the old open cluster (OC) NGC 2682. From the high resolution (R~60,000) spectra obtained by the Subaru / HDS, we derived radial velocity, rotation velocity, and calculated chemical abundances of lithium, carbon and oxygen. Radial velocity of the target stars is consistent with the mean radial velocity of member stars of the cluster. Thus, we confirm the targets are indeed the real members of the cluster. Rotation velocity of BSSs distributes in a wide range of few km/s to hundred km/s, while those of TOs is restricted to a small value (vsini ≦7 km/s) . Both mass transfer scenario and collision scenario are expected to spin up BSSs. Target stars with measured Li abundances show a good agreement to the trend between A(Li) and Teff found in previous works . Moreover, BSSs have C and O abundances not significantly different from those of the TOs. Exceptions are BSS S997 and S1273. S997 shows a slight enhancement in O abundance, while S1273 shows a significant depletion in C abundance and a slight depletion in O abundance compared to other BSSs and TOs in the same cluster. These anomalies in C and O abundances may be interpreted by mass transfer scenario.
Cheul Hong Min
VERA observations of SiO masers in Symbiotic star R Aquarii
R Aquarii (R Aqr) is one of the closest symbiotic systems and one of the SiO maser sources associated with the Mira variable in Symbiotic star. These systems are very interesting target, and R Aqr is very exciting laboratory because of the existence of jet-like feature.
Though observations of the system have not yielded consistent values of the orbital parameters, the binary parameters of the orbit give an evidence whether or not Roche lobe outflow in the long period variable and interacting stellar winds of the formation of accretion disk and jet in secondary star. VERA has performed the observations toward R
Aqr since 2004. VERA its unique observation system is a powerful tool for astrometry, and we can hopefully obtain information about its orbital motions. In this presentation, I will present the result of VERA observations for R Aqr.