Kinematic studies of early-type stars. II. The velocity field within 2 KPC of the Sun.

Rubin, C. V.; Burley, J.

doi:10.1086/109235

Cited by 10 publications

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“…(6) Since observational kinematical data, i.e., proper motions and radial velocities, of stars or clusters in the Galaxy are relatively limited, there have only been a few authors who investigated the large-scale radial motion of the Galaxy that included a determination of the parameters C and D, which are small quantities in comparison with the Oort constants A and B reflecting the differential rotation of the Galaxy. In an early work, Rubin & Burley (1964) derived (C, D) = (1 ± 1, −2 ± 1) km s −1 kpc −1 by using some 800 early-type stars. Later, Zhao (1984b) used 1412 O, B type stars and found (C, D) = (0.5 ± 0.5, −2.0 ± 0.4) km s −1 kpc −1 .…”

Section: Resultsmentioning

confidence: 99%

Kinematics of the Open Cluster System in the Galaxy

Zhao

Chen

2006

Chin. J. Astron. Astrophys.

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Absolute proper motions and radial velocities of 202 open clusters in the solar neighborhood, which can be used as tracers of the Galactic disk, are used to investigate the kinematics of the Galaxy in the solar vicinity, including the mean heliocentric velocity components (u 1 , u 2 , u 3) of the open cluster system, the characteristic velocity dispersions (σ 1 , σ 2 , σ 3), Oort constants (A, B) and the large-scale radial motion parameters (C, D) of the Galaxy. The results derived from the observational data of proper motions and radial velocities of a subgroup of 117 thin disk young open clusters by means of a maximum likelihood algorithm are: (u 1 , u 2 , u 3) = (−16.1 ± 1.0, −7.9 ± 1.4, −10.4 ± 1.5) km s −1 , (σ 1 , σ 2 , σ 3) = (17.0 ± 0.7, 12.2 ± 0.9, 8.0 ± 1.3) km s −1 , (A, B) = (14.8 ± 1.0, −13.0 ± 2.7) km s −1 kpc −1 , and (C, D) = (1.5 ± 0.7, −1.2 ± 1.5) km s −1 kpc −1. A discussion on the results and comparisons with what was obtained by other authors is given.

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Section: Resultsmentioning

confidence: 99%

Kinematics of the Open Cluster System in the Galaxy

Zhao

Chen

2006

Chin. J. Astron. Astrophys.

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“…In their works Rubin and Burley (1964), Feast and Shuttleworth (1965), Petrie (1963), Petrie and Petrie (1968), Bonneau (1967a) and others are already using new observational data for obtaining the velocity field up to 3-4 kpc distance.…”

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The velocity dispersions of O- and B-stars within a few kpc

Shatsova¹

1970

Symp. - Int. Astron. Union

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Abstract. The results of a study of the dispersion of velocities of 0-B5 stars up to a distance of 3 kpc are described.The modern catalogues of motions of OB stars enable us to pass, in the study of stellar kinematics, from the solar vicinity to more distant regions. In their works Burley (1964), Feast andShuttleworth (1965), Petrie (1963), Petrie (1968), Bonneau (1967a) and others are already using new observational data for obtaining the velocity field up to 3-4 kpc distance.To each volume element of the Galaxy one may attribute as kinematic characte ristics the velocity of the centroid and the distribution function of peculiar velocities or, what amounts to the same, the velocity dispersion, the asymmetry, etc. In the present paper an attempt is made to derive within the accessible volume of the Galaxy the distribution of velocity dispersions.As observational basis we used the radial velocities and distances taken from the catalogues of Rubin et al (1962) and Bonneau (1967b). The volume of space covered by these catalogues was divided into heliocentric rings, or semirings, and sectors. The average number of stars in a single section for r<3 kpc amounts to 56 and 53 in Rubin's and Bonneau's catalogues respectively.The observed velocities of stars were corrected for standard solar motion, the Oort's term of galactic rotation and the average residual radial velocity corresponding to the volume element to which the star belongs. A special examination has shown that the average velocity consists of the errors in Oort's terms (mainly due to syste matic errors in the distances), the higher order terms of galactic rotation, the radial motion (if any) in the Galaxy, as well as any local motion.The errors in the mean distances in the Oort's term and in the velocity dispersion were determined by an analytic method which was worked out by us following the ideas of Feast and Shuttleworth (1965) These values figure among other solutions in the paper of Petrie and Petrie (1968). The local motions in the majority of space elements do not exceed the errors of average residual velocities. The maximum velocities appeared in the sections /" = 120°-150° and r>2kpc (K r = 7-ll km s" 1 ) and r=\-2 kpc, R

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