Explosion of very massive stars and the origin of intermediate mass black holes

AbstractWe calculate evolution, collapse, explosion, and nucleosynthesis of Population III very massive stars with 500 M⊙ and 1000 M⊙. It was found that both 500 M⊙ and 1000 M⊙ models enter the region of pair-instability but continue to undergo core collapse to black holes. For moderately aspherical explosions, the patterns of nucleosynthesis match the observational data of intergalactic and intercluster medium and hot gases in M82, better than models involving hypernovae and pair instability supernovae.Our results suggest that explosions of Population III core-collapse very massive stars contribute significantly to the chemical evolution of gases in clusters of galaxies. The final black hole masses are about 500 M⊙ for our most massive 1000 M⊙ models. This result may support the view that Population III very massive stars are responsible for the origin of intermediate mass black holes which were recently reported to be discovered.

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Nucleosynthesis of the Elements in Faint Supernovae and Hypernovae

Proceedings of the International Astronomical Union ◽

10.1017/s1743921310000128 ◽

2009 ◽

Vol 5 (S265) ◽

pp. 34-41

Author(s):

Ken'ichi Nomoto ◽

Takashi Moriya ◽

Nozomu Tominaga

Keyword(s):

Black Holes ◽

Neutron Stars ◽

Electron Capture ◽

Massive Stars ◽

Core Collapse ◽

Agb Stars ◽

Intermediate Mass ◽

Normal Core ◽

Intermediate Mass Black Holes

AbstractWe review the properties of supernovae (SNe) as a function of the progenitor's mass M. (1) Mup - 10 M⊙ stars are super-AGB stars and resultant electron capture SNe may be Faint supernovae like Type IIn SN 2008S. (2) 10 - 12 M⊙ stars undergo Fe-core collapse to form neutron stars (NSs) and Faint supernovae. (3) 12 M⊙ - MBN stars undergo Fe-core collapse to form NSs and normal core-collapse supernovae. (4) MBN - 90 M⊙ stars undergo Fe-core collapse to form Black Holes. Resultant supernovae are bifurcate into Hypernovae and Faint supernovae. The observed properties of SN 2008ha can be explained with this type of Faint supernovae. (5) 90 - 140 M⊙ stars produce Luminous SNe, like SNe 2007bi and 2006gy. (6) 140 - 300 M⊙ stars become pair-instability supernovae which could be Luminous supernovae (SNe 2007bi and 2006gy). (7) Very massive stars with M ≳ 300 M⊙ undergo core-collapse to form intermediate mass black holes. Some SNe could be more Luminous supernovae (like SN 2006gy).

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Intermediate-Mass Black Holes

Annual Review of Astronomy and Astrophysics ◽

10.1146/annurev-astro-032620-021835 ◽

2020 ◽

Vol 58 (1) ◽

pp. 257-312 ◽

Cited By ~ 7

Author(s):

Jenny E. Greene ◽

Jay Strader ◽

Luis C. Ho

Keyword(s):

Black Holes ◽

Black Hole ◽

Globular Clusters ◽

High Redshift ◽

Mass Function ◽

Intermediate Mass ◽

The Galaxy ◽

Robust Measurements ◽

Black Hole Masses ◽

Intermediate Mass Black Holes

We describe ongoing searches for intermediate-mass black holes with MBH ≈ 10–105 M⊙. We review a range of search mechanisms, both dynamical and those that rely on accretion signatures. We find the following conclusions: ▪ Dynamical and accretion signatures alike point to a high fraction of 109–1010 M⊙ galaxies hosting black holes with MBH∼ 105 M⊙. In contrast, there are no solid detections of black holes in globular clusters. ▪ There are few observational constraints on black holes in any environment with MBH ≈ 100–104 M⊙. ▪ Considering low-mass galaxies with dynamical black hole masses and constraining limits, we find that the MBH–σ* relation continues unbroken to MBH ∼105 M⊙, albeit with large scatter. We believe the scatter is at least partially driven by a broad range in black hole masses, because the occupation fraction appears to be relatively high in these galaxies. ▪ We fold the observed scaling relations with our empirical limits on occupation fraction and the galaxy mass function to put observational bounds on the black hole mass function in galaxy nuclei. ▪ We are pessimistic that local demographic observations of galaxy nuclei alone could constrain seeding mechanisms, although either high-redshift luminosity functions or robust measurements of off-nuclear black holes could begin to discriminate models.

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Intermediate-mass black holes in globular clusters: observations and simulations - Update

Proceedings of the International Astronomical Union ◽

10.1017/s1743921315010601 ◽

2015 ◽

Vol 12 (S316) ◽

pp. 240-245

Author(s):

Nora Lützgendorf ◽

Markus Kissler-Patig ◽

Karl Gebhardt ◽

Holger Baumgardt ◽

Diederik Kruijssen ◽

...

Keyword(s):

Black Holes ◽

Black Hole ◽

Globular Clusters ◽

Galactic Center ◽

Early Stage ◽

Life Time ◽

Intermediate Mass ◽

Software Environment ◽

Integral Field ◽

Intermediate Mass Black Holes

AbstractThe study of intermediate-mass black holes (IMBHs) is a young and promising field of research. If IMBH exist, they could explain the rapid growth of supermassive black holes by acting as seeds in the early stage of galaxy formation. Formed by runaway collisions of massive stars in young and dense stellar clusters, intermediate-mass black holes could still be present in the centers of globular clusters, today. We measured the inner kinematic profiles with integral-field spectroscopy for 10 Galactic globular cluster and determined masses or upper limits of central black holes. In combination with literature data we further studied the positions of our results on known black-hole scaling relations (such as M• − σ) and found a similar but flatter correlation for IMBHs. Applying cluster evolution codes, the change in the slope could be explained with the stellar mass loss occurring in clusters in a tidal field over its life time. Furthermore, we present results from several numerical simulations on the topic of IMBHs and integral field units (IFUs). N-body simulations were used to simulate IFU data cubes. For the specific case of NGC 6388 we simulated two different IFU techniques and found that velocity dispersion measurements from individual velocities are strongly biased towards lower values due to blends of neighbouring stars and background light. In addition, we use the Astrophysical Multipurpose Software Environment (AMUSE) to combine gravitational physics, stellar evolution and hydrodynamics to simulate the accretion of stellar winds onto a black hole. We find that the S-stars need to provide very strong winds in order to explain the accretion rate in the galactic center.

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Intermediate-mass black holes in globular clusters: constraints on the spin of a black hole

Astrophysics ◽

10.1007/s10511-011-9204-7 ◽

2011 ◽

Vol 54 (4) ◽

pp. 548-552 ◽

Cited By ~ 15

Author(s):

S. D. Buliga ◽

V. I. Globina ◽

Yu. N. Gnedin ◽

T. M. Natsvlishvili ◽

M. Yu. Piotrovich ◽

...

Keyword(s):

Black Holes ◽

Black Hole ◽

Globular Clusters ◽

Intermediate Mass ◽

Intermediate Mass Black Holes

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Monte Carlo modeling of globular star clusters: many primordial binaries and IMBH formation

Proceedings of the International Astronomical Union ◽

10.1017/s1743921315007838 ◽

2014 ◽

Vol 10 (S312) ◽

pp. 213-222

Author(s):

Mirek Giersz ◽

Nathan Leigh ◽

Michael Marks ◽

Arkadiusz Hypki ◽

Abbas Askar

Keyword(s):

Black Holes ◽

Monte Carlo ◽

Black Hole ◽

Star Clusters ◽

Orbital Parameter ◽

Intermediate Mass ◽

Cluster Evolution ◽

Global Cluster ◽

Cluster Properties ◽

Intermediate Mass Black Holes

AbstractWe will discuss the evolution of star clusters with a large initial binary fraction, up to 95%. The initial binary population is chosen to follow the invariant orbital-parameter distributions suggested by Kroupa (1995). The Monte Carlo MOCCA simulations of star cluster evolution are compared to the observations of Milone et al. (2012) for photometric binaries. It is demonstrated that the observed dependence on cluster mass of both the binary fraction and the ratio of the binary fractions inside and outside of the half mass radius are well recovered by the MOCCA simulations. This is due to a rapid decrease in the initial binary fraction due to the strong density-dependent destruction of wide binaries described by Marks, Kroupa & Oh (2011). We also discuss a new scenario for the formation of intermediate mass black holes in dense star clusters. In this scenario, intermediate mass black holes are formed as a result of dynamical interactions of hard binaries containing a stellar mass black hole, with other stars and binaries. We will discuss the necessary conditions to initiate the process of intermediate mass black hole formation and the dependence of its mass accretion rate on the global cluster properties.

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Collisions in primordial star clusters

Astronomy and Astrophysics ◽

10.1051/0004-6361/201732224 ◽

2018 ◽

Vol 614 ◽

pp. A14 ◽

Cited By ~ 22

Author(s):

B. Reinoso ◽

D. R. G. Schleicher ◽

M. Fellhauer ◽

R. S. Klessen ◽

T. C. N. Boekholt

Keyword(s):

Black Holes ◽

Massive Stars ◽

Star Clusters ◽

Parameter Study ◽

Effective Parameters ◽

Intermediate Mass ◽

Stellar Collisions ◽

Accretion Rates ◽

Relevant Role ◽

Intermediate Mass Black Holes

Collisions were suggested to potentially play a role in the formation of massive stars in present day clusters, and have likely been relevant during the formation of massive stars and intermediate mass black holes within the first star clusters. In the early Universe, the first stellar clusters were particularly dense, as fragmentation typically only occurred at densities above 109 cm−3, and the radii of the protostars were enhanced as a result of larger accretion rates, suggesting a potentially more relevant role of stellar collisions. We present here a detailed parameter study to assess how the number of collisions and the mass growth of the most massive object depend on the properties of the cluster. We also characterize the time evolution with three effective parameters: the time when most collisions occur, the duration of the collisions period, and the normalization required to obtain the total number of collisions. We apply our results to typical Population III (Pop. III) clusters of about 1000 M⊙, finding that a moderate enhancement of the mass of the most massive star by a factor of a few can be expected. For more massive Pop. III clusters as expected in the first atomic cooling halos, we expect a more significant enhancement by a factor of 15–32. We therefore conclude that collisions in massive Pop. III clusters were likely relevant to form the first intermediate mass black holes.

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Very massive stars, pair-instability supernovae and intermediate-mass black holes with the sevn code

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stx1576 ◽

2017 ◽

Vol 470 (4) ◽

pp. 4739-4749 ◽

Cited By ~ 97

Author(s):

Mario Spera ◽

Michela Mapelli

Keyword(s):

Black Holes ◽

Massive Stars ◽

Intermediate Mass ◽

Intermediate Mass Black Holes

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mocca-survey Database I: Binary black hole mergers from globular clusters with intermediate mass black holes

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa2677 ◽

2020 ◽

Vol 498 (3) ◽

pp. 4287-4294

Author(s):

Jongsuk Hong ◽

Abbas Askar ◽

Mirek Giersz ◽

Arkadiusz Hypki ◽

Suk-Jin Yoon

Keyword(s):

Black Holes ◽

Black Hole ◽

Gravitational Waves ◽

Globular Clusters ◽

Stellar Mass ◽

Intermediate Mass ◽

Binary Black Holes ◽

Black Hole Binaries ◽

Binary Black Hole ◽

Intermediate Mass Black Holes

ABSTRACT The dynamical formation of black hole binaries in globular clusters that merge due to gravitational waves occurs more frequently in higher stellar density. Meanwhile, the probability to form intermediate mass black holes (IMBHs) also increases with the density. To explore the impact of the formation and growth of IMBHs on the population of stellar mass black hole binaries from globular clusters, we analyse the existing large survey of Monte Carlo globular cluster simulation data (mocca-survey Database I). We show that the number of binary black hole mergers agrees with the prediction based on clusters’ initial properties when the IMBH mass is not massive enough or the IMBH seed forms at a later time. However, binary black hole formation and subsequent merger events are significantly reduced compared to the prediction when the present-day IMBH mass is more massive than ${\sim}10^4\, \rm M_{\odot }$ or the present-day IMBH mass exceeds about 1 per cent of cluster’s initial total mass. By examining the maximum black hole mass in the system at the moment of black hole binary escaping, we find that ∼90 per cent of the merging binary black holes escape before the formation and growth of the IMBH. Furthermore, large fraction of stellar mass black holes are merged into the IMBH or escape as single black holes from globular clusters in cases of massive IMBHs, which can lead to the significant underpopulation of binary black holes merging with gravitational waves by a factor of 2 depending on the clusters’ initial distributions.

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