GRRMHD Simulations of State Transitions in Non-Jetted Tidal Disruption Events
Brandon Curd, Safira Heridia, Aviyel Ahiyya, Richard Anantua

TL;DR
This study uses GRRMHD simulations to explore late-stage behavior of TDE debris disks, revealing thermal instability, X-ray spectral changes, and correlations with black hole spin, matching observations of AT2021ehb.
Contribution
First GRRMHD simulations of magnetized TDE debris disks during late stages, linking spectral evolution and disk collapse to black hole spin.
Findings
Disk becomes thermally unstable within 17-46 days.
X-ray luminosity declines by nearly two orders of magnitude after collapse.
Spectral properties match observed TDE AT2021ehb.
Abstract
Circularization of the stream material into a debris cloud during tidal disruption events (TDEs) was recently demonstrated in one of the most accurate long duration TDE simulations to-date. The cooling envelope model (CEM) provides a description of the circularized debris cloud and its emission over time well beyond circularization across different disruption parameters. In the CEM, sub-Eddington accretion rates occur early in TDEs and the debris has a shallow density profile of roughly , with Eddington accretion only being achieved after several months. To explore the late stages of the CEM, we perform general relativistic radiation magnetohydrodynamics (GRRMHD) simulations of magnetized tori adapted from the near Eddington phase of the CEM for a star disrupted around a black hole (BH). We find that the disk becomes thermally unstable…
Peer Reviews
No public reviews on file for this paper yet. If you reviewed it on a platform where reviews are public (OpenReview, ICLR, NeurIPS, ICML), you can paste yours below so the community can read it here.
Videos
No videos yet. Explain this paper in a talk, walkthrough, or lecture? Add one.
