Tidal disruption effects near black holes and Lambda-gravity

Abstract

The tidal disruption of stars in the vicinity of massive black holes is discussed in the context of $\Lambda$-gravity. The latter provides an explanation to the Hubble tension as a possible consequence of two Hubble flows, the local and global ones. The bunch of notions which play role for the considered tidal effect are obtained, along with the rate of the disrupted stars. The role of pulsars is emphasized due to their ability to penetrate up to the horizon of the massive black hole as for them the tidal radius can reach the horizon. Tidal disruption mechanism also can lead to segregation of stars by their mean density vs the distance from the black hole, the denser stars surviving at shorter distances. The interplay of the central gravity field and the repulsive $\Lambda$-term increasing with radius and its certain observational consequences are discussed.

arXiv comment6 pages, 3 figures; Eur.Phys.J.Plus (in press)

References in corpus (18)

• A Massive Pulsar in a Compact Relativistic Binary
• Tensions between the Early and the Late Universe
• The Expansion of the Universe is Faster than Expected
• Rates of tidal disruption of stars by massive central black holes
• On the Hubble constant tension in the SNe Ia Pantheon sample
• Prospects for Probing the Spacetime of Sgr A* with Pulsars
• A Quantitative Test of the No-Hair Theorem with Sgr A* using stars, pulsars, and the Event Horizon Telescope
• Loss Cone Dynamics
• First-order Cosmological Perturbations Engendered by Point-like Masses
• Clustering of Galaxies with f(R) gravity
• Black hole shadow to probe modified gravity
• The cosmological constant derived via galaxy groups and clusters
• Two fundamental constants of gravity unifying the dark matter and the dark energy
• On the common nature of dark matter and dark energy: galaxy groups
• Hubble tension vs two flows
• On the Lambda-evolution of galaxy clusters
• Lense-Thirring precession and modified gravity constraints
• Lense-Thirring precession and gravito-gyromagnetic ratio