Tidal deformability of boson stars and dark matter clumps

普适关系遇见因果性：约束中子星动力学潮汐Love数

Universal Relations Meet Causality: Bounding the Dynamical Love Number of Neutron Stars

研究利用因果性等约束将中子星潮汐响应转化为全纯自映射，通过Schwarz-Pick定理给出动力学潮汐修正上限，并与最新计算对比，发现界限在百分之几内饱和，证实f模主导性，可提供不依赖状态方程的动力学潮汐上限。

Flaring of tidally compressed dark-matter clumps

We explore the physics and observational consequences of tidal compression events (TCEs) of dark-matter clumps (DMCs) by supermassive black holes (SMBHs). Our analytic calculations show that a DMC approaching a SMBH much closer than the tidal radius undergoes significant compression along the axis perpendicular to the orbital plane, shortly after pericenter passage. For DMCs composed of self-annihilating dark-matter particles, we find that the boosted DMC density and velocity dispersion lead to a flaring of the annihilation rate, most pronounced for a velocity- dependent annihilation cross sec…

Confronting nuclear equation of state in the presence of dark matter using GW170817 observation in relativistic mean field theory approach

We confront admixture of dark matter inside neutron star using gravitational wave constraints coming from binary neutron star merger. We consider a relativistic mean field model including $σ-ω-ρ$ meson interaction with NL3 parameterization. We study fermionic dark matter interacting with nucleonic matter via Higgs portal mechanism. We show that admixture of dark matter inside the neutron star soften the equation state and lower the value of tidal deformability. Gravitational wave GW170817 observation puts an upper bound on tidal deformability of a binary neutron star with low spin prior at 90\…

我们能识别原初黑洞吗？对亚太阳质量引力波观测的潮汐检验

Can we identify primordial black holes? Tidal tests for subsolar-mass gravitational-wave observations

本文研究如何通过潮汐效应区分亚太阳质量原初黑洞双星与中子星或白矮星等恒星双星，并预测LVK及下一代探测器可高显著性测量或约束潮汐形变，从而验证或排除原初黑洞起源。

Jeans Instability of Palomar 5's Tidal Tail

Tidal tails composed of stars should be unstable to the Jeans instability and this can cause them to look like beads on a string. The Jeans wavelength and tail diameter determine the wavelength and growth rate of the fastest growing unstable mode. Consequently the distance along the tail to the first clump and spacing between clumps can be used to estimate the mass density in the tail and its longitudinal velocity dispersion. Clumps in the tidal tails of the globular cluster Palomar 5 could be due to Jeans instability. We find that their spacing is consistent with the fastest growing mode if t…

Generation of gravitational waves and tidal disruptions in clumpy galaxies

Obtaining a better understanding of intermediate-mass black holes (IMBHs) is crucial, as their properties could shed light on the origin and growth of their supermassive counterparts. Massive star-forming clumps, which are present in a large fraction of massive galaxies at $z \sim$ 1-3, are amongst the venues wherein IMBHs could reside. We perform a series of Fokker-Planck simulations to explore the occurrence of tidal disruption (TD) and gravitational wave (GW) events about an IMBH in a massive star-forming clump, modelling the latter so that its mass ($10^8 \,{\rm M}_{\odot}$) and effective …