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SUMMARY:Modelling black hole accretion through an 𝛼-disc with a resolve
 d interstellar medium in dwarf galaxies - Eun-jin Shin (IoA)
DTSTART:20250328T113000Z
DTEND:20250328T123000Z
UID:TALK228601@talks.cam.ac.uk
CONTACT:Sandro Tacchella
DESCRIPTION:We perform high-resolution simulations of an isolated dwarf ga
 laxy with a virial mass of 1e10 Msun harbouring a 1e4 Msun intermediate ma
 ss black hole (IMBH) embedded in a nuclear star cluster (NSC) at its centr
 e. To model a realistic interstellar medium (ISM)\, we incorporate IMF-sam
 pled star formation\, photo-ionisation feedback\, H_II region modelling\, 
 photoelectric heating from a spatially varying far-ultraviolet field\, and
  supernova feedback. Our approach employs a sub-grid Shakura-Sunyaev accre
 tion disc model to accurately simulate the evolution of BH mass and spin. 
 Using super-Lagrangian refinement techniques\, we resolve spatial scales u
 p to 0.01 pc\, capturing the self-gravitating radius of the accretion disc
 \, allowing accurate measurement of mass and angular momentum transfer to 
 the IMBH. The gravitational potential of the NSC captures the ISM\, formin
 g a circumnuclear disc (CND)\, while its torques drive angular momentum lo
 ss from parsec to sub-parsec scales\, circularising gas onto the 𝛼-accr
 etion disc and fuelling IMBH accretion. We further investigate star format
 ion in the vicinity of the IMBH. In the innermost regions\, within 0.2 pc\
 , star formation is highly suppressed. However\, at distances of approxima
 tely 1 to 7 pc from the centre\, the gas remains locally susceptible to fr
 agmentation\, leading to the formation of massive\, young stars. The feedb
 ack from these stars can potentially disrupt the CND entirely and cut off 
 the gas supply to the IMBH. Our study demonstrates the complexity of IMBH 
 accretion once the resolved ISM is taken into account and paves the way fo
 r next-generation studies incorporating IMBH-driven feedback processes.
LOCATION:Ryle Seminar Room\, KICC + online
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