Year: 2026
Type: article
Abstract: During a tidal disruption event (TDE), a star loses mass due to the tidal gravitational forces of the black hole. In a partial TDE, a stellar remnant is left behind. Several dozen TDEs have been detected so far, including repeating partial events. We use the P hantom smoothed particle hydrodynamics code to model the disruption of a 1 M ⊙ star around a 10 6 M ⊙ black hole for impact parameters resulting in ≤50% mass loss. We only consider zero-energy orbits. Our simulations show that the mass fallback rate can exceed the Eddington limit for β ≥ 0.8, allowing debris to obscure the accretion disc by forming a reprocessing layer, similar to full TDEs. The mass fallback rate is shallower than t −5/3 , tracking closer to t −9/4 . Assuming thermal emission from the debris, that shock heating is trapped, that electron scattering dominates the opacity, and a color correction ( f col ) of 1.7, we find temperatures of ∼ 10 4 K, optical bolometric luminosities of ∼ 10 42−44 erg s −1 , and blackbody radii ranging from 10 to 100 au for our simulations. We compare our values with observations and find support for the previous argument that some TDEs classified as full disruptions might actually be partial. Moreover, our results explain the detected optical/UV TDEs. We also find that our zero-energy partial TDEs have properties similar to the repeating partial TDEs such as ASSASN-19dj , ASSASN-14ko , ASSASN-18ul , ASSASN-22ci , and AT2020vdq . In the β = 0.8 isentropic simulation where radiation is assumed to escape, we find X-ray luminosities of ∼10 44−45 erg s −1 and radii lower than the inner most-stable circular orbit.
Source: The Astrophysical Journal
Language: English
Subfield: Astronomy and Astrophysics
Field: Physics and Astronomy
Domain: Physical Sciences
Open Access status: gold
Estimated APC paid: $4,499
OpenAlex ID: W7165614437
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