Stellar Cartography

Partial Tidal Disruption Events: The Elixir Of Life

By Keith Cowing
Status Report
March 8, 2024
Filed under , , ,
Partial Tidal Disruption Events: The Elixir Of Life
Remnants of 1 MβŠ™, 3 MβŠ™, and 10 MβŠ™ MAMS models at 4.8 days, 7.3 days, and 9 days post-pericentre, respectively (top to bottom). Except, the 10 MβŠ™, 𝛽 = 2.15 is analysed at 59 days post-pericentre. We show column density perpendicular to the orbital plane, showing only material identified as belonging to the remnant (i.e. bound and not belonging to the streams). Each panel is 200 RβŠ™ Γ— 200 RβŠ™. Each row shows the models at different penetration factors, with the first column showing the models before the disruption. The radius of the remnants increases as the star approaches closer to the SMBH. The remnants bear a striking similarity to G-objects in the galactic centre (Ciurlo et al. 2020). astro-ph.HE

In our Galactic Center, about 10,000 to 100,000 stars are estimated to have survived tidal disruption events, resulting in partially disrupted remnants.

These events occur when a supermassive black hole (SMBH) tidally interacts with a star, but not enough to completely disrupt the star. We use the 1D stellar evolution code Kepler and the 3D smoothed particle hydrodynamics code Phantom to model the tidal disruption of 1, 3, and 10 solar mass stars at zero-age (ZAMS), middle-age (MAMS), and terminal-age main-sequence (TAMS).

We map the disruption remnants into Kepler in order to understand their post-distribution evolution. We find distinct characteristics in the remnants, including increased radius, rapid core rotation, and differential rotation in the envelope. The remnants undergo composition mixing that affects their stellar evolution. Whereas the remnants formed by disruption of ZAMS models evolve similarly to unperturbed models of the same mass, for MAMS and TAMS stars, the remnants have higher luminosity and effective temperature.

Potential observational signatures include peculiarities in nitrogen and carbon abundances, higher luminosity, rapid rotation, faster evolution, and unique tracks in the Hertzsprung-Russell diagram

Megha Sharma (Monash University), Daniel J. Price (Monash University), Alexander Heger (Monash University)

Comments: 22 pages, 27 figures, submitted to MNRAS, comments welcome
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)
Cite as: arXiv:2403.04211 [astro-ph.HE] (or arXiv:2403.04211v1 [astro-ph.HE] for this version)
Submission history
From: Megha Sharma
[v1] Thu, 7 Mar 2024 04:28:13 UTC (10,253 KB)

Explorers Club Fellow, ex-NASA Space Station Payload manager/space biologist, Away Teams, Journalist, Lapsed climber, Synaesthete, Na’Vi-Jedi-Freman-Buddhist-mix, ASL, Devon Island and Everest Base Camp veteran, (he/him) πŸ––πŸ»