期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 517, 期 3, 页码 3613-3639出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stac2563
关键词
gravitation; methods: numerical; Galaxy: kinematics and dynamics; Galaxy: stellar content; open clusters and associations: individual: Hyades, Praesepe, Coma Berenices, COIN-Gala 13, NGC 752, NGC 2419, Pal 5, Pal 14, GD-1; solar neighbourhood
资金
- Grant Agency of the Czech Republic [20-21855S]
- DAAD-East-European-Exchange programme at the University of Bonn
- Agence Nationale de la Recherche (ANR) [ANR-18- CE31-0006, ANR-19-CE31-0017]
- European Research Council (ERC) under the European Union [834148]
- Agencia Estatal de Investigacion (AEI) of the Ministerio de Ciencia e Innovacion (MCINN) [FJC2018-037323-I]
After their birth, many stars go through the tidal threshold of their cluster and enter the classical tidal tails. The asymmetry between the leading and trailing tails is a test of gravitational theory. Observations of open clusters show that there are more stars in the leading tail than in the trailing tail. Future research is needed to study the tidal tails around open clusters of different ages and develop appropriate methods for analysis.
After their birth a significant fraction of all stars pass through the tidal threshold (prgh) of their cluster of origin into the classical tidal tails. The asymmetry between the number of stars in the leading and trailing tails tests gravitational theory. All five open clusters with tail data (Hyades, Praesepe, Coma Berenices, COIN-Gaia 13, NGC 752) have visibly more stars within d(cl) approximate to 50 pc of their centre in their leading than their trailing tail. Using the Jerabkova-compact-convergent-point (CCP) method, the extended tails have been mapped out for four nearby 600-2000 Myr old open clusters to d(cl) > 50 pc. These are on near-circular Galactocentric orbits, a formula for estimating the orbital eccentricity of an open cluster being derived. Applying the Phantom of Ramses code to this problem in Newtonian gravitation the tails are near-symmetrical. In Milgromian dynamics (MOND), the asymmetry reaches the observed values for 50 < d(cl)/pc < 200 being maximal near peri-galacticon, and can slightly invert near apo-galacticon, and the Kupper epicyclic overdensities are asymmetrically spaced. Clusters on circular orbits develop orbital eccentricity due to the asymmetrical spill-out, therewith spinning up opposite to their orbital angular momentum. This positive dynamical feedback suggests Milgromian open clusters to demise rapidly as their orbital eccentricity keeps increasing. Future work is necessary to better delineate the tidal tails around open clusters of different ages and to develop a Milgromian direct n-body code.
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