Tidal effects on small bodies by massive black holes

TL;DR

This paper investigates how the strong gravitational field of the supermassive black hole at the Galactic Center affects small objects, potentially causing tidal disruption and flares observable as synchrotron radiation, with implications for understanding black hole environments.

Contribution

It introduces a model for tidal disruption of small objects near black holes and links flare light curves to geodesic orbital dynamics, offering new insights into black hole astrophysics.

Findings

Tidal effects can melt small objects like asteroids near black holes.

Flares may result from tidal squeezing and synchrotron radiation during disruption.

Light curves depend mainly on orbital dynamics, not physical properties of objects.

Abstract

The compact radio source Sagittarius A (Sgr A) at the centre of our Galaxy harbours a supermassive black hole, whose mass has been measured from stellar orbital motions. Sgr A is therefore the nearest laboratory where super-massive black hole astrophysics can be tested, and the environment of black holes can be investigated. Since it is not an active galactic nucleus, it also offers the possibility of observing the capture of small objects that may orbit the central black hole. We study the effects of the strong gravitational field of the black hole on small objects, such as a comet or an asteroid. We also explore the idea that the flares detected in Sgr A might be produced by the final accretion of single, dense objects with mass of the order of 10^20 g, and that their timing is not a characteristic of the sources, but rather of the space-time of the central galactic black hole in which they are moving. We find that tidal effects are strong enough to melt the solid object, and present calculations of the temporal evolution of the light curve of infalling objects as a function of various parameters. Our modelling of tidal disruption suggests that during tidal squeezing, the conditions for synchrotron radiation can be met. We show that the light curve of a flare can be deduced from dynamical properties of geodesic orbits around black holes and that it depends only weakly on the physical properties of the source.