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The Utilization of Bayesian Framework in Determining Projected Spatial Distributions of Star Clusters
Hidayat Y.A.a, Arifyanto M.I.a, Apriliaa
a Department of Astronomy, Faculty of Mathematics and Natural Sciences, Institut Teknologi Bandung, Indonesia
[vc_row][vc_column][vc_row_inner][vc_column_inner][vc_separator css=”.vc_custom_1624529070653{padding-top: 30px !important;padding-bottom: 30px !important;}”][/vc_column_inner][/vc_row_inner][vc_row_inner layout=”boxed”][vc_column_inner width=”3/4″ css=”.vc_custom_1624695412187{border-right-width: 1px !important;border-right-color: #dddddd !important;border-right-style: solid !important;border-radius: 1px !important;}”][vc_empty_space][megatron_heading title=”Abstract” size=”size-sm” text_align=”text-left”][vc_column_text]© 2020 Published under licence by IOP Publishing Ltd.Star clusters are groups of stars that are bonded to each other by their gravitational forces. In general, star clusters are divided into the globular cluster and open cluster. There will always be some dynamic interactions in their lifetime, i.e. the process of relaxation and equipartition of interstellar encounter energy. The modeling is done by using King, Generalised King (GKing), Optimised Generalised King (OGKing), Elson Fall Freeman (EFF), Generalised Density Profile (GDP), and Restricted Generalised Density Profile (RGDP) profiles. Based on the Bayes factor, the results of a review of the density structure for star cluster Blanco 1 are dominated by King group profiles (King, GKing, and OGKing). Ellipticity values at the core radius (ϵrc and tidal radius (ϵrtobtained are 0.07-0.01+0.56 and 0.10-0.01+0.66, respectively. The estimation of the occurrence of mass segregation can be viewed from the value of κ. The κ valued obtained for Blanco 1 is 0.06-0.24+0.10 means that it undergo some mass segregation. The total mass obtained using the tidal force relationship of gravitational interactions with the potential Galaxy is 1623-364+273M⊙.[/vc_column_text][vc_empty_space][vc_separator css=”.vc_custom_1624528584150{padding-top: 25px !important;padding-bottom: 25px !important;}”][vc_empty_space][megatron_heading title=”Author keywords” size=”size-sm” text_align=”text-left”][vc_column_text]Bayesian frameworks,Density profile,Density structures,Dynamic interaction,Globular clusters,Gravitational forces,Gravitational interaction,Mass segregation[/vc_column_text][vc_empty_space][vc_separator css=”.vc_custom_1624528584150{padding-top: 25px !important;padding-bottom: 25px !important;}”][vc_empty_space][megatron_heading title=”Indexed keywords” size=”size-sm” text_align=”text-left”][vc_column_text][/vc_column_text][vc_empty_space][vc_separator css=”.vc_custom_1624528584150{padding-top: 25px !important;padding-bottom: 25px !important;}”][vc_empty_space][megatron_heading title=”Funding details” size=”size-sm” text_align=”text-left”][vc_column_text][/vc_column_text][vc_empty_space][vc_separator css=”.vc_custom_1624528584150{padding-top: 25px !important;padding-bottom: 25px !important;}”][vc_empty_space][megatron_heading title=”DOI” size=”size-sm” text_align=”text-left”][vc_column_text]https://doi.org/10.1088/1742-6596/1523/1/012008[/vc_column_text][/vc_column_inner][vc_column_inner width=”1/4″][vc_column_text]Widget Plumx[/vc_column_text][/vc_column_inner][/vc_row_inner][/vc_column][/vc_row][vc_row][vc_column][vc_separator css=”.vc_custom_1624528584150{padding-top: 25px !important;padding-bottom: 25px !important;}”][/vc_column][/vc_row]