Non-radial oscillations in newly born compact star considering effects of phase transition

Abstract

The massive stars end their lives by supernova explosions leaving central compact objects that may evolve into neutron stars. Initially, after birth, the star remains hot and gradually cools down. We explore the matter and star properties during this initial stage of the compact stars considering the possibility of the appearance of deconfined quark matter in the core of the star. At the initial stage after the supernova explosion, the occurrence of non-radial oscillation in the newly born compact object is highly possible. Non-radial oscillations are an important source of GWs. There is a high chance for GWs from these oscillations, especially the nodeless fundamental (f-) mode to be detected by next-generation GW detectors. We study the evolution in frequencies of non-radial oscillation after birth considering phase transition and predicting the possible signature for different possibilities of theoretical compact star models.

Accepted for publication in MNRAS

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• Effects of dark boson mediated feeble interaction between dark matter (DM) and quark matter on $f$-mode oscillation of DM admixed quark stars
• Non-radial oscillations of hadronic neutron stars, quark stars, and hybrid stars : Calculation of $f$, $p$, and $g$ mode frequencies
• Quasi-normal f-modes of anisotropic quark stars in full general relativity
• Suppression of composition $g$-modes in chemically-equilibrating warm neutron stars
• $f$-mode oscillations in hot Neutron Stars: Effect of hyperons and neutrino trapping
• $f$ and $p$ mode oscillation of proto-neutron stars with systematic variation of the nucleon effective mass
• Axial $w$-modes of anisotropic neutron stars