2018/12/27 by Valery V. Kravtsov, В. В. Кравцов, Kravtsov, Valery V.
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Astrophysics of Galaxies (astro-ph.GA) #FOS: Physical sciences #Stellar, planetary, and galactic studies #astro-ph.GA
paper · pdf · doi:10.48550/arxiv.1812.10656
3 pages, no figures; submitted to BAAA to be published in proceedings of Second Binational Meeting AAA-SOCHIAS, La Serena, Chile, Oct. 7-12, 2018; based on talk given at the meeting
arxiv created 2018/12/27 · openalex publication_date 2018/12/27 · arxiv updated 2018/12/31 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
The relaxation time at the half-mass radius of Galactic globular clusters (GGCs) is typically within a few Gyr. Hence, the majority of GGCs are expected to be well relaxed systems, given their age is around 12-13 Gyr. So any initial radial segregation between stars of the same initial mass on the main sequence (MS), in particular, the progenitors of the present day sub-giant and red-giant branch (SGB, RGB) stars should already have dissipated. However, a body of evidence contradicting to these expectations has been accumulated to date. The paradox could be solved by taking into account the effect of stellar collisions. They occur at particularly high rate in collapsing nuclei of GGCs and seem to be mainly responsible for unrelaxed central regions and the radial segregation observed. We draw attention that actually observed collisional blue stragglers should be less numerous than their lower-mass counterparts formed and accumulated at and below the present day MS turnoff. The effect of this is that MS/SGB/RGB stars of a given luminosity are not of the same mass but fall in a range of mass.