高能暂现源 · 每日文献综述

Primordial black holes (PBHs) provide a unique probe of the early Universe. Their cosmological evolution is governed by the competition between mass accretion and Hawking evaporation. In this paper we look into the details impact of accretion. Most of the earlier analysis relied on non-relativistic accretion models. In this work, we reinvestigate this in a fully relativistic framework for Kerr PBHs in the radiation-dominated era. We derive relativistic accretion rate and compute spin-dependent efficiency λ<SUB>Kerr</SUB>(a <SUB>*</SUB>). Using this result, we construct coupled evolution equations for the PBH mass and spin that include both relativistic accretion and spin-dependent evaporation. Our analysis shows that relativistic accretion significantly increases PBH masses and consequently suppresses their spins, causing all PBHs to become effectively Schwarzschild well before evaporation. These effects strengthen the Big Bang Nucleosynthesis (BBN) bound on the initial PBH mass by a factor of ∼4─5, reduce the mass required for survival to the present epoch to ∼2.7 × 10<SUP>14</SUP> g, and shift the viable particle like DM parameter space. Notably the early accretion induced spin-down effect further washes out the well known high-frequency, spin-induced feature in the high frequency stochastic gravitational-wave background, modifying predictions for future detectors.

The remnant of a black hole binary merger settles into a stationary configuration by "ringing down" through the emission of gravitational waves that consist of a superposition of damped exponentials with discrete complex frequencies—the remnant black hole's quasinormal modes. While the frequencies themselves depend solely on the mass and spin of the remnant, the mode amplitudes depend on the merger dynamics. We investigate quasinormal mode excitation by a point particle plunging from the innermost stable circular orbit of a Kerr black hole. Our formalism is general, but we focus on computing the quasinormal mode excitation coefficients in the frequency domain for equatorial orbits, and we analyze their dependence on the remnant black hole spin. We find that higher overtones and subdominant multipoles of the radiation become increasingly significant for rapidly rotating black holes. This suggests that the prospects for detecting overtones and higher-order modes are considerably enhanced for highly spinning merger remnants.

We study rotating hybrid stars, with particular emphasis on the effect of spin on the deconfinement phase transition and star properties. Our analysis is based on a hybrid equation of state with a phase transition from hadronic matter containing hyperons to color-superconducting quark matter, where the quark phase is modeled within a relativistic density functional approach. By varying the strength of the vector repulsion and diquark pairing couplings in the microscopic quark Lagrangian, we construct a set of hybrid star sequences with different quark-matter onset densities. This framework ensures consistency with astrophysical and gravitational wave constraints on mass, radius, and tidal deformability. We show how increasing the rotational frequency affects the maximum gravitational mass, oblateness, central energy density of compact stars, as well as the onset of quasiradial oscillations and nonaxisymmetric instabilities. Our results indicate that, for the most favorable parameter sets with strong vector coupling, hybrid stars containing a color-superconducting quark-matter core can account for the fastest-spinning and most massive known neutron star, PSR J0952-0607. In contrast, this pulsar cannot be explained by the purely hadronic equation of state considered in this study. These findings are highly relevant for future observations with the Square Kilometre Array (SKA), which will significantly expand the known pulsar population and enable precise measurements of masses and spin frequencies.

The inflationary <inline-formula><mml:math><mml:mi>B</mml:mi></mml:math></inline-formula>-mode signals encode invaluable information about the origin of our Universe, and searching for potential signatures of primordial gravitational waves (PGWs) is one of the major science goals for future precision observations of cosmic microwave background (CMB) polarization. However, dominant <inline-formula><mml:math><mml:mi>B</mml:mi></mml:math></inline-formula>-mode signals of both Galactic foreground contamination and gravitational lensing effects prevent direct measurements of the PGW <inline-formula><mml:math><mml:mi>B</mml:mi></mml:math></inline-formula>-mode signals. There are existing proposals which can effectively eliminate these two contaminants but issues remain for future high-sensitivity and multifrequency CMB polarization observations, such as spatially varying spectral energy distribution (SED) of polarized foreground and cosmological <inline-formula><mml:math><mml:mi>B</mml:mi></mml:math></inline-formula>-mode signals due to primordial magnetic fields. In this work, we investigate inference of PGW <inline-formula><mml:math><mml:mi>B</mml:mi></mml:math></inline-formula>-mode signals in the presence of both complexities. We employ a constrained moment internal linear combination method to remove polarization signals arising from spatially varying SEDs. Also, we employ a power-spectrum-based approach to extracting both the Galactic and cosmological <inline-formula><mml:math><mml:mi>B</mml:mi></mml:math></inline-formula>-mode components. Two methods have been validated by mock data and different consistency tests have been performed. We apply these two methods to end-to-end simulations for future high-sensitivity and multifrequency polarization observations and investigate the detectability of different <inline-formula><mml:math><mml:mi>B</mml:mi></mml:math></inline-formula>-mode signals in the presence of complex polarized foregrounds under different scenarios. This study will be important for new physics studies with <inline-formula><mml:math><mml:mi>B</mml:mi></mml:math></inline-formula>-mode signatures.