PIRSA:20110049

Video URL

https://pirsa.org/20110049

Disappearing stars without a trace: what is their maximum angular momentum?

Murguia Berthier, A. (2020). Disappearing stars without a trace: what is their maximum angular momentum? . Perimeter Institute for Theoretical Physics. https://pirsa.org/20110049

Murguia Berthier, Ariadna. Disappearing stars without a trace: what is their maximum angular momentum? . Perimeter Institute for Theoretical Physics, Nov. 12, 2020, https://pirsa.org/20110049 

          @misc{ scivideos_PIRSA:20110049,
            doi = {10.48660/20110049},
            url = {https://pirsa.org/20110049},
            author = {Murguia Berthier, Ariadna},
            keywords = {Strong Gravity},
            language = {en},
            title = {Disappearing stars without a trace: what is their maximum angular momentum? },
            publisher = {Perimeter Institute for Theoretical Physics},
            year = {2020},
            month = {nov},
            note = {PIRSA:20110049 see, \url{https://scivideos.org/pirsa/20110049}}
          }

Ariadna Murguia Berthier University of California, Santa Cruz

Talk numberPIRSA:20110049
DOI10.48660/20110049
Source RepositoryPIRSA
Collection
Talk Type Scientific Series
Subject

Abstract

We have tentative evidence of massive stars that disappear without a bright transient. It is commonly argued that this massive stars have low angular momentum and can collapse into a black hole without significant feedback. In this talk I will make use of general-relativistic hydrodynamical simulations to understand the flow around a newly-formed black hole. I will discuss the angular momentum needed in order for the infalling material to be accreted into the black hole without forming a centrifugally supported structure, thus generating no effective feedback. If the feedback from the black hole is significant, the collapse can be halted and, as a result, it is likely followed by a bright transient. With the results from the simulation, I will constrain the maximum rotation rate for the disappearing massive progenitors know, and set a limit on the rate of expected disappearing stars.