Radial velocities of blue stragglers. 1: A catalog of candidates in six open clusters

1994 ◽  
Vol 108 ◽  
pp. 1828 ◽  
Author(s):  
A. A. E. Milone ◽  
D. W. Latham
Keyword(s):  
Open Clusters ◽  
Radial Velocities ◽  
Blue Stragglers

scholarly journals Spectroscopic Binaries in the Open Cluster M67

1992 ◽  
Vol 135 ◽  
pp. 155-157 ◽  
Author(s):  
David W. Latham ◽  
Robert D. Mathieu ◽  
Alejandra A.E. Milone ◽  
Robert J. Davis
Keyword(s):  
Circular Orbit ◽  
Main Sequence ◽  
Open Cluster ◽  
Radial Velocities ◽  
Spectroscopic Binaries ◽  
Eccentric Orbit ◽  
Circular Orbits ◽  
Blue Stragglers ◽  
Short Period ◽  
Blue Straggler

AbstractFor almost 400 members of M67 we have accumulated about 5,000 precise radial velocities. Already we have orbital solutions for more than 32 spectroscopic binaries in M67. Many of these orbits were derived by combining the Palomar and CfA observations, thus extending the time coverage to more than 20 years. The distribution of eccentricity versus period shows evidence for tidal circularization on the main sequence. The transition from circular orbits is fairly clean. Excluding the blue stragglers, the first eccentric orbit has a period of 11.0 days, while the last circular orbit has a period of 12.4 days. For longer periods the distribution of eccentricity is the same as for field stars. The blue straggler S1284 has an eccentric orbit despite its short period of 4.2 days.

Stellar and molecular radial velocities for six young open clusters

1988 ◽  
Vol 95 ◽  
pp. 1122 ◽  
Author(s):  
Tianxing Liu ◽  
Kenneth A. Janes ◽  
T. M. Bania ◽  
Randy L. Phelps
Keyword(s):  
Open Clusters ◽  
Radial Velocities

scholarly journals A Determination of Secular Parallaxes of Reference Stars from Relative Proper Motions of Open Clusters

1970 ◽  
Vol 7 ◽  
pp. 74-76
Author(s):  
A. N. Deutsch
Keyword(s):  
Systematic Errors ◽  
Open Clusters ◽  
Radial Velocities ◽  
Proper Motions ◽  
The Mean

The determination of secular parallaxes of stars is usually based on meridian observations of proper motions of bright stars, this introducing known systematic errors. The mean parallaxes of stars can be obtained by means of radial velocities which are known for the bright stars. The more perspective method, the reference of stars to galaxies, is not applicable at low galactic latitudes.

scholarly journals Stellar Spins in the Pleiades, Praesepe, and M35 Open Clusters

2021 ◽  
Vol 923 (1) ◽  
pp. 23
Author(s):  
Brian F. Healy ◽  
P. R. McCullough ◽  
Kevin C. Schlaufman
Keyword(s):  
Systematic Error ◽  
Open Clusters ◽  
Photometric Data ◽  
Radial Velocities ◽  
Proper Motions ◽  
Kinematics Analysis ◽  
Mean Velocity ◽  
Clockwise Direction ◽  
Single Cluster

Abstract We analyze spectroscopic and photometric data to determine the projected inclinations of stars in three open clusters: the Pleiades, Praesepe, and M35. We determine the sin i values of 42, 35, and 67 stars in each cluster, respectively, and from their distributions we find that isotropic spins and moderate alignment are both consistent with the Pleiades and Praesepe data. While it is difficult to distinguish between these scenarios for a single cluster, an ensemble of such distributions may facilitate a distinction. The M35 inclination distribution is most consistent with a superposition of isotropic and anisotropic spins, the source of which could be systematic error or a physical grouping of aligned stars. We also study internal cluster kinematics using radial velocities and proper motions. Our kinematics analysis reveals significant plane-of-sky rotation in Praesepe, with a mean velocity of 0.132 ± 0.022 km s−1 in a clockwise direction.

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