Follow the Mass -- A Concordance Picture of Tidal Disruption Events

TL;DR

This study synthesizes three independent simulations of tidal disruption events (TDEs), revealing a consistent dynamical picture that aligns with observations and enables improved mass inference methods.

Contribution

It provides a unified simulation-based model of TDE dynamics that matches observed properties and introduces an updated method for estimating stellar and black hole masses.

Findings

Simulations produce similar TDE dynamics despite different methods.

The model accurately predicts observed flare energies, luminosities, and line widths.

The method estimates black hole masses around 10^6.3 solar masses.

Abstract

Three recent global simulations of tidal disruption events (TDEs) have produced, using different numerical techniques and parameters, very similar pictures of their dynamics. In typical TDEs, after the star is disrupted by a supermassive black hole, the bound portion of the stellar debris follows highly eccentric trajectories, reaching apocenters of several thousand gravitational radii. Only a very small fraction is captured upon returning to the vicinity of the supermassive black hole. Nearly all the debris returns to the apocenter, where shocks produce a thick irregular cloud on this radial scale and power the optical/UV flare. These simulation results imply that over a few years, the thick cloud settles into an accretion flow responsible for the long term emission. Despite not being designed to match observations, and without adjusting any parameters, the dynamical picture given by the three simulations aligns well with observations of typical events, correctly predicting the flares' typical total radiated energy, luminosity, temperature and emission line width. On the basis of these predictions, we provide an updated method (TDEmass) to infer the stellar and black hole masses from a flare's peak luminosity and temperature. This picture also correctly predicts that the luminosity observed years after the flare should be nearly constant. In addition, we show that in a magnitude-limited survey, if the intrinsic rate of TDEs is independent of black hole mass, the detected events will preferentially have black hole masses $\sim 10^{6.3 \pm 0.3} M_\odot$ and stellar masses $\sim 1 M_\odot$, with the width of the mass distribution for disrupted stars sensitive to the stellar mass function in the host galaxy's center.