Kinematics of OB Stars

Branham, Jr. Richard L.

doi:10.1086/339567

Cited by 17 publications

(23 citation statements)

References 15 publications

(17 reference statements)

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“…It is a high value but in agreement with recent studies of OYB5 star samples from the Hipparcos catalog by Miyamoto & Zhu (1998), Â ¼268:7AE11:9 km s À1 ; Uemura et al (2000), Â ¼ 255:52 AE 8:33 km s À1 ; or Branham (2002), Â ¼ 258:7 AE 34:29 km s À1 . A similar result (Â ¼ 270 km s À1 ) is also reached by Méndez et al (2000) using data from the Southern Proper Motion Catalog ( Platais et al 1998); thus, their result is obtained from measures of the proper motions independent of those from Hipparcos.…”

Section: Estimation Of the Oort Constantssupporting

confidence: 91%

OB Stars in the Solar Neighborhood. II. Kinematics

2006

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Using the spatial classification method and the structural parameters estimated for the Gould Belt (GB) and the local Galactic disk ( LGD) from a previous paper, we have evaluated spatial membership probabilities for a sample of O and B stars from the Hipparcos catalog ( Perryman and coworkers) with available proper motions and radial velocity data. Thus, being able to study the space velocity fields of both systems, we conclude that the GB and the LGD present different statistical distributions, both in velocity space and in phase space. In light of their possible existence as distinct systems, we analyze different kinematic aspects in the vicinity of the Sun, and we find the GB to be responsible for the highly negative vertex deviation found for the OB stars in the solar neighborhood. We also find that the GB noticeably alters the estimation of the Oort constants in the Galactic disk; thus, in order to establish comparisons with other kinematic studies based on older stellar populations, a careful pruning of the GB members must be performed. Further analysis of the GB velocity field and the moving groups that contribute to it suggest the possibility that the GB can be the result of a chance superposition of moving groups. We propose for future investigations the dynamical analysis of these moving groups in order to probe the origin of the GB.

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Section: Estimation Of the Oort Constantssupporting

confidence: 91%

OB Stars in the Solar Neighborhood. II. Kinematics

2006

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“…The difference ω = A − B gives the angular velocity of Galactic rotation in the solar neighborhood. Secondorder equations, for example, the generalized Oort model, which can be found in Ogorodnikov (1965), Edmondson (1937), and Branham (2002), are occasionally considered.…”

Section: Classical Kinematic Modelsmentioning

confidence: 99%

Kinematics of stars in the northern and southern galactic hemispheres

Vityazev

Tsvetkov

2012

Astron. Lett.

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“…At the end of the last century, the accuracy and whole-sky coverage of the Hipparcos mission led to a major improvement in the definition and characterization of nearby OB associations and clusters, which profoundly changed our knowledge and understanding of the solar vicinity (e.g. Figueras et al 1997;de Zeeuw et al 1999;Platais et al 1998;Subramaniam & Bhatt 2000;de Bruijne 2000;Branham 2002;Elias et al 2006a,b).…”

Section: Introductionmentioning

confidence: 99%

Cosmography of OB stars in the solar neighbourhood

Bouy

Alves

2015

A&A

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We construct a 3D map of the spatial density of OB stars within 500 pc from the Sun using the Hipparcos catalogue and find three large-scale stream-like structures that allow a new view on the solar neighbourhood. The spatial coherence of these blue streams and the monotonic age sequence over hundreds of parsecs suggest that they are made of young stars, similar to the young streams that are conspicuous in nearby spiral galaxies. The three streams are 1) the Scorpius to Canis Majoris stream, covering 350 pc and 65 Myr of star formation history; 2) the Vela stream, encompassing at least 150 pc and 25 Myr of star formation history; and 3) the Orion stream, including not only the well-known Orion OB1abcd associations, but also a large previously unreported foreground stellar group lying only 200 pc from the Sun. The map also reveals a remarkable and previously unknown nearby OB association, between the Orion stream and the Taurus molecular clouds, which might be responsible for the observed structure and star formation activity in this cloud complex. This new association also appears to be the birthplace of Betelgeuse, as indicated by the proximity and velocity of the red giant. If this is confirmed, it would solve the long-standing puzzle of the origin of Betelgeuse. The well-known nearby star-forming low-mass clouds, including the nearby T and R associations Lupus, Cha, Oph, CrA, Taurus, Vela R1, and various low-mass cometary clouds in Vela and Orion, appear in this new view of the local neighbourhood to be secondary star formation episodes that most likely were triggered by the feedback from the massive stars in the streams. We also recover well-known star clusters of various ages that are currently cruising through the solar neighbourhood. Finally, we find no evidence of an elliptical structure such as the Gould belt, a structure we suggest is a 2D projection effect, and not a physical ring.

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Kinematics of OB Stars

Cited by 17 publications

References 15 publications

OB Stars in the Solar Neighborhood. II. Kinematics

OB Stars in the Solar Neighborhood. II. Kinematics

Kinematics of stars in the northern and southern galactic hemispheres

Cosmography of OB stars in the solar neighbourhood

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