Abstract Details

Name: Kiren O V
Affiliation: Lecturer
Conference ID: ASI2020_296
Title : Evolution of Primordial Dark Matter Planets in Early Universe
Authors and Co-Authors : Kiren O V Arun Kenath C Sivaram
Abstract Type : Poster
Abstract Category : General Relativity and Cosmology
Abstract : Dark matter is theorized as one of the basic constituents of the universe, five times more abundant than ordinary matter. Several astronomical measurements have confirmed the existence of dark matter, leading to experiments worldwide (like XENON1T experiment) to directly observe dark matter particle. Till now the interaction of these matters with ordinary matter have proven so feeble that they have escaped direct detection. In our recent paper we had discussed possibility of DM at high redshifts forming primordial planets composed entirely of DM to be one of the reasons for not detecting DM. Such DM objects could have formed in the earlier epochs of the universe (when local DM density was much higher) and be in existence now. We had tabulated wide range of masses and Radius of such DM planets with an upper limit of Neptune mass down to Asteroid mass. Here we discuss the evolution of these DM planets. The DM particles are heavier (60 – 100 GeV) compared to the abundant Hydrogen and Helium. They also collapse much earlier than Hydrogen and Helium (not being coupled to radiation). After the accretion of DM particles, Helium starts to gravitate and gets accreted, followed by Hydrogen. Helium will sink lower as it is heavy compared to Hydrogen, as a result these DM planets will have a layer of DM particles, followed by a layer of Helium and then Hydrogen. The total mass accreted on these DM planets is calculated integrating over the complete epoch. As more mass is accreted the temperatures of Hydrogen and Helium increases, which could trigger nuclear reactions.