Volume 594, October 2016
|Number of page(s)||10|
|Published online||18 October 2016|
The effect of pair-instability mass loss on black-hole mergers
1 Astronomical Observatory, Warsaw University, Ujazdowskie 4, 00-478 Warsaw, Poland
2 Monash Centre for Astrophysics, School of Physics and Astronomy, Monash University, Victoria 3800, Australia
3 School of Physics & Astronomy, University of Minnesota, Minneapolis, MN 55455, USA
4 Center for Nuclear Astrophysics, Department of Physics and Astronomy, Shanghai Jiao-Tong University, Shanghai 200240, PR China
5 Joint Institute for Nuclear Astrophysics, 1 Cyclotron Laboratory, National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, MI 48824-1321, USA
6 Research School of Astronomy and Astrophysics, The Australian National University, Canberra, ACT 2611, Australia
7 ARC Centre of Excellence for All-sky Astrophysics (CAASTRO), 2006 New south Wales, Australia
8 Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA
9 Enrico Fermi Institute, Department of Physics, Department of Astronomy and Astrophysics, and Kavli Institute for Cosmological Physics, University of Chicago, Chicago, IL 60637, USA
10 Center for Computational Relativity and Gravitation, Rochester Institute of Technology, Rochester, New York 14623, USA
11 CCS-2, MSD409, Los Alamos National Laboratory, Los Alamos, NM 87545, USA
12 Department of Physics and Astronomy, The University of Mississippi, University, MS 38677, USA
13 CENTRA, Departamento de Física, Instituto Superior Técnico, Universidade de Lisboa, Avenida Rovisco Pais 1, 1049 Lisboa, Portugal
Received: 22 May 2016
Accepted: 17 July 2016
Context. Mergers of two stellar-origin black holes are a prime source of gravitational waves and are under intensive investigation. One crucial ingredient in their modeling has been neglected: pair-instability pulsation supernovae with associated severe mass loss may suppress the formation of massive black holes, decreasing black-hole-merger rates for the highest black-hole masses.
Aims. We demonstrate the effects of pair-instability pulsation supernovae on merger rate and mass using populations of double black-hole binaries formed through the isolated binary classical evolution channel.
Methods. The mass loss from pair-instability pulsation supernova is estimated based on existing hydrodynamical calculations. This mass loss is incorporated into the StarTrack population synthesis code. StarTrack is used to generate double black-hole populations with and without pair-instability pulsation supernova mass loss.
Results. The mass loss associated with pair-instability pulsation supernovae limits the Population I/II stellar-origin black-hole mass to 50 M⊙, in tension with earlier predictions that the maximum black-hole mass could be as high as 100 M⊙. In our model, neutron stars form with mass 1−2 M⊙. We then encounter the first mass gap at 2−5 M⊙ with the compact object absence due to rapid supernova explosions, followed by the formation of black holes with mass 5−50 M⊙, with a second mass gap at 50−135 M⊙ created by pair-instability pulsation supernovae and by pair-instability supernovae. Finally, black holes with masses above 135 M⊙ may potentially form to arbitrarily high mass limited only by the extent of the initial mass function and the strength of stellar winds. Suppression of double black-hole-merger rates by pair-instability pulsation supernovae is negligible for our evolutionary channel. Our standard evolutionary model, with the inclusion of pair-instability pulsation supernovae and pair-instability supernovae, is fully consistent with the Laser Interferometric Gravitational-wave Observatory (LIGO) observations of black-hole mergers: GW150914, GW151226, and LVT151012. The LIGO results are inconsistent with high (≳ 400 km s-1) black hole (BH) natal kicks. We predict the detection of several, and up to as many as ~60, BH-BH mergers with a total mass of 10−150 M⊙ (most likely range: 20−80 M⊙) in the forthcoming ~60 effective days of the LIGO O2 observations, assuming the detectors reach the optimistic target O2 sensitivity.
Key words: stars: massive / black hole physics / gravitational waves
© ESO, 2016
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