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Kinematics of OB-associations in the 3-kpc solar neighborhood

Published online by Cambridge University Press:  13 January 2020

Anna M. Melnik ,
Andrei K. Dambis ,
Elena V. Glushkova  and
Pertti Rautiainen
Anna M. Melnik
Affiliation:
Sternberg Astronomical Institute, Lomonosov Moscow State University, Universitetskii pr. 13, Moscow, 119991, Russia email: anna@sai.msu.ru
Andrei K. Dambis
Affiliation:
Sternberg Astronomical Institute, Lomonosov Moscow State University, Universitetskii pr. 13, Moscow, 119991, Russia email: anna@sai.msu.ru Faculty of Physics, Lomonosov Moscow State University, Leninskie Gory 1-2, Moscow, 119991, Russia
Elena V. Glushkova
Affiliation:
Sternberg Astronomical Institute, Lomonosov Moscow State University, Universitetskii pr. 13, Moscow, 119991, Russia email: anna@sai.msu.ru Faculty of Physics, Lomonosov Moscow State University, Leninskie Gory 1-2, Moscow, 119991, Russia
Pertti Rautiainen
Affiliation:
Astronomy Research Unit, University of Oulu, P.O. Box 3000, FI-90014 Oulun yliopisto, Finland
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Abstract

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We use Gaia (DR1, DR2) stellar proper motions to study the kinematics of OB-associations. The average one-dimensional velocity dispersion inside 18 OB-associations with more than 10 Gaia DR1 stars is σv = 3.9 km s−1. The median virial and stellar masses of OB-associations are equal to 7×105 and 9 × 103 solar masses, respectively. The median star-formation efficiency is ε = 2.1%. We have found the expansion in several OB-associations. Models of the Galaxy with a two-component outer ring R1R2 can reproduce the average residual velocities of OB-associations in the Perseus, Sagittarius and Local System complexes.

Keywords

Galaxy: kinematics and dynamicsopen clusters and associations: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S345: Origins: From the Protosun to the First Steps of Life , August 2018 , pp. 39 - 42
Copyright
© International Astronomical Union 2020 

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