English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

This paper introduces a series of papers presenting a quantitative theory forthe tidal disruption of main sequence stars by supermassive black holes. Usingfully general relativistic hydrodynamics simulations and MESA-model initialconditions, we explore the pericenter-dependence of tidal disruption propertiesfor eight stellar masses ($0.15 \leq M_*/M_\odot \leq 10$) and six black holemasses ($10^5 \leq M_{BH}/M_\odot \leq 5 \times 10^7$). We present here theresults most relevant to observations. The effects of internal stellarstructure and relativity decouple for both the disruption cross section and thecharacteristic energy width of the debris. Moreover, the full disruption crosssection is almost independent of $M_*$ for $M_*/M_\odot \lesssim 3$.Independent of $M_*$, relativistic effects increase the critical pericenterdistance for full disruptions by up to a factor $\sim 3$ relative to theNewtonian prediction. The probability of a direct capture is also independentof $M_*$; at $M_{BH}/M_\odot \simeq 5 \times 10^6$ this probability is equal tothat of a complete disruption. The width of the debris energy distribution$\Delta E$ can differ from the standard estimate by factors from 0.35 to 2,depending on $M_*$ and $M_{BH}$, implying a corresponding change in thecharacteristic mass-return timescale. The "frozen-in approximation" isinconsistent with $\Delta E$, and mass-loss continues over a long span of time.We provide analytic forms, suitable for use in both event rate estimates andparameter inference, to describe all these trends. For partial disruptions, wefind a nearly-universal relation between the star's angular momentum and thefraction of $M_*$ remaining. Within the "empty loss-cone" regime, partialdisruptions must precede full disruptions. These partial disruptions candrastically affect the rate and appearance of subsequent total disruptions.

Tidal Disruptions of Main Sequence Stars -- I. Observable Quantities and their Dependence on Stellar and Black Hole Mass