Formation of low-spinning 100 Msun black holes

Abstract

It is speculated that a merger of two massive stellar-origin BHs in a dense stellar environment may lead to the formation of a massive BH in the pair-instability mass gap (50-135 Msun). Such a merger-formed BH is expected to typically have a high spin (a=0.7). If such a massive BH acquires another BH it may lead to another merger detectable by LIGO/Virgo in gravitational waves. Acquiring a companion may be hindered by gravitational-wave kick/recoil, which accompanies the first merger and may quickly remove the massive BH from its parent globular or nuclear cluster. We test whether it is possible for a massive merger-formed BH in the pair-instability gap to be retained in its parent cluster and have low spin. Such a BH would be indistinguishable from a primordial BH. We employed results from numerical relativity calculations of black hole mergers to explore the range of gravitational-wave recoil velocities for various combinations of merging BH masses and spins. We compared merger-formed massive BH speeds with typical escape velocities from globular and nuclear clusters. We show that a globular cluster is highly unlikely to form and retain a 100 Msun BH if the spin of the BH is low (a<0.3) as such BHs acquire high recoil speeds (>200 km/s) that exceed typical escape speeds from globular clusters (50 km/s). However, a very low-spinning (a=0.1) and massive (100 Msun) BH could be formed and retained in a galactic nuclear star cluster. Even though such massive merger-formed BHs with such low spins acquire high speeds during formation (400 km/s), they may avoid ejection since massive nuclear clusters have high escape velocities (300-500 km/s). A future detection of a massive BH in the pair-instability mass gap with low spin would therefore not be proof of the existence of primordial BHs, which are sometimes claimed to have low spins and arbitrarily high masses.

published: A&A 640, L20 (2020)

References in corpus (10)

• Large Merger Recoils and Spin Flips From Generic Black-Hole Binaries
• Total recoil: the maximum kick from nonspinning black-hole binary inspiral
• Slowing the Spins of Stellar Cores
• Merging black holes in young star clusters
• On the final spin from the coalescence of two black holes
• The Masses and Spins of Neutron Stars and Stellar-Mass Black Holes
• Mergers of Stellar-Mass Black Holes in Nuclear Star Clusters
• Modeling kicks from the merger of non-precessing black-hole binaries
• The numerical relativity breakthrough for binary black holes
• A runaway collision in a young star cluster as the origin of the brightest supernova

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