On the Maximum Stellar Rotation to form a Black Hole without an Accompanying Luminous Transient
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On the Maximum Stellar Rotation to form a Black Hole without an Accompanying Luminous Transient. / Murguia-Berthier, Ariadna; Batta, Aldo; Janiuk, Agnieszka; Ramirez-Ruiz, Enrico; Mandel, Ilya; Noble, Scott C.; Everson, Rosa Wallace.
In: Astrophysical Journal Letters, Vol. 901, No. 2, 24, 01.10.2020.Research output: Contribution to journal › Letter › Research › peer-review
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T1 - On the Maximum Stellar Rotation to form a Black Hole without an Accompanying Luminous Transient
AU - Murguia-Berthier, Ariadna
AU - Batta, Aldo
AU - Janiuk, Agnieszka
AU - Ramirez-Ruiz, Enrico
AU - Mandel, Ilya
AU - Noble, Scott C.
AU - Everson, Rosa Wallace
PY - 2020/10/1
Y1 - 2020/10/1
N2 - The collapse of a massive star with low angular momentum content is commonly thought to result in the formation of a black hole without an accompanying bright transient. Our goal in this Letter is to understand the flow in and around a newly formed black hole, involving accretion and rotation, via general relativistic hydrodynamics simulations aimed at studying the conditions under which infalling material can accrete without forming a centrifugally supported structure and, as a result, generate no effective feedback. On the other hand, if the feedback from the black hole is significant, the collapse would be halted and we suggest that the event is likely to be followed by a bright transient. We find that feedback is only efficient if the specific angular momentum of the infalling material at the innermost stable circular orbit exceeds that of geodesic circular flow at that radius by at least 20%. We use the results of our simulations to constrain the maximal stellar rotation rates of the disappearing massive progenitors PHL293B-LBV and N6946-BH1, and to provide an estimate of the overall rate of disappearing massive stars. We find that about a few percent of single O-type stars with measured rotational velocities are expected to spin below the critical value before collapse and are thus predicted to vanish without a trace.
AB - The collapse of a massive star with low angular momentum content is commonly thought to result in the formation of a black hole without an accompanying bright transient. Our goal in this Letter is to understand the flow in and around a newly formed black hole, involving accretion and rotation, via general relativistic hydrodynamics simulations aimed at studying the conditions under which infalling material can accrete without forming a centrifugally supported structure and, as a result, generate no effective feedback. On the other hand, if the feedback from the black hole is significant, the collapse would be halted and we suggest that the event is likely to be followed by a bright transient. We find that feedback is only efficient if the specific angular momentum of the infalling material at the innermost stable circular orbit exceeds that of geodesic circular flow at that radius by at least 20%. We use the results of our simulations to constrain the maximal stellar rotation rates of the disappearing massive progenitors PHL293B-LBV and N6946-BH1, and to provide an estimate of the overall rate of disappearing massive stars. We find that about a few percent of single O-type stars with measured rotational velocities are expected to spin below the critical value before collapse and are thus predicted to vanish without a trace.
KW - Relativistic disks
KW - Accretion
KW - Massive stars
KW - Hydrodynamical simulations
KW - General relativity
KW - FAILED SUPERNOVAE
KW - ACCRETION DISCS
KW - CORE-COLLAPSE
KW - FLOWS
KW - VARIABILITY
KW - SIMULATIONS
KW - EVOLUTION
KW - SEARCH
KW - SHOCKS
KW - DISKS
U2 - 10.3847/2041-8213/abb818
DO - 10.3847/2041-8213/abb818
M3 - Letter
VL - 901
JO - The Astrophysical Journal Letters
JF - The Astrophysical Journal Letters
SN - 2041-8205
IS - 2
M1 - 24
ER -
ID: 252155533