N. Galikyan, Sh. Khlghatyan, A. A. Kocharyan, V. G. Gurzadyan
{"title":"S2-star dynamics probing the Galaxy core cluster","authors":"N. Galikyan, Sh. Khlghatyan, A. A. Kocharyan, V. G. Gurzadyan","doi":"arxiv-2409.10567","DOIUrl":null,"url":null,"abstract":"The star cluster surrounding the supermassive black hole in the center of\nMilky Way is probed using the data on the S2 star. The value of precession\nfound at the physics-informed neural networks (PINN) analysis of the S2 data is\nused to consider the role of the scattering of S2 star on stars of the cluster,\ndescribed by a random force given by the Holtsmark distribution. The critical\nvalue for the star density of the core cluster for which the observed\nprecession value by PINN lies inside 70\\% confidence interval (between 15\\% and\n85\\% quantiles) around the median of precession due to scattering, is obtained\nas n_crit \\approx 8.3 10^6 pc^-3, that is at higher star densities the\nperturbation of the orbit of S2 would exceed the observed one.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"32 1","pages":""},"PeriodicalIF":0.0000,"publicationDate":"2024-09-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":null,"platform":"Semanticscholar","paperid":null,"PeriodicalName":"arXiv - PHYS - Astrophysics of Galaxies","FirstCategoryId":"1085","ListUrlMain":"https://doi.org/arxiv-2409.10567","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"","JCRName":"","Score":null,"Total":0}
引用次数: 0
Abstract
The star cluster surrounding the supermassive black hole in the center of
Milky Way is probed using the data on the S2 star. The value of precession
found at the physics-informed neural networks (PINN) analysis of the S2 data is
used to consider the role of the scattering of S2 star on stars of the cluster,
described by a random force given by the Holtsmark distribution. The critical
value for the star density of the core cluster for which the observed
precession value by PINN lies inside 70\% confidence interval (between 15\% and
85\% quantiles) around the median of precession due to scattering, is obtained
as n_crit \approx 8.3 10^6 pc^-3, that is at higher star densities the
perturbation of the orbit of S2 would exceed the observed one.
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