Element abundances of unevolved stars in the open cluster M 67
نویسندگان
چکیده
منابع مشابه
Chemical composition of evolved stars in the open cluster M 67 ⋆
High-resolution spectra of six core heliumburning ‘clump’ stars and three giants in the open cluster M 67 have been obtained with the SOFIN spectrograph on the Nordic Optical Telescope to investigate abundances of up to 25 chemical elements. Abundances of carbon were studied using the C2 Swan (0,1) band head at 5635.5 Å. The wavelength interval 7980–8130 Å with strong CN features was analysed i...
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We use differential CCD photometry to search for variability in BV I among 990 stars projected in and around the old open cluster M67. In a previous paper we reported results for 22 cluster members that are optical counterparts to X-ray sources; this study focuses on the other stars in our observations. A variety of sampling rates were employed, allowing variability on time scales ranging from ...
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We present the results of a 47-ks Chandra-ACIS observation of the old open cluster M67. We detected 25 proper-motion cluster members (including ten new sources) and 12 sources (all new) that we suspect to be members from their locations close to the main sequence (1<B–V <1.7). Of the detected members, 23 are binaries. Among the new sources that are members and probable members are four spectros...
متن کاملNeutron-Capture Element Abundances in Halo Stars
Abundance comparisons of neutron-capture elements – those formed in slow (sprocess) and rapid (r-process) neutron-capture nucleosynthesis – are providing important new information about the nature of the earliest Galactic nucleosynthesis and the first stellar generations (see recent reviews by Truran et al. 2002, Sneden & Cowan 2003 and Cowan & Thielemann 2004). Most previous studies have been ...
متن کاملPhotometric variability in the open cluster M 67 I . Cluster members detected in X - rays
We study photometric variability among the optical counterparts of X-ray sources in the old open cluster M67. The two puzzling binaries below the giant branch are both variables: for S 1113 the photometric period is compatible with the orbital period, S 1063 either varies on a period longer than the orbital period, or does not vary periodically. For the spectroscopic binaries S 999, S 1070 and ...
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ژورنال
عنوان ژورنال: Astronomy & Astrophysics
سال: 2006
ISSN: 0004-6361,1432-0746
DOI: 10.1051/0004-6361:20054291