scholarly journals Comparing the birth rate of stellar black holes in binary black hole mergers and long gamma-ray bursts

2018 ◽  
Vol 610 ◽  
pp. A58
Author(s):  
J.-L. Atteia ◽  
J.-P. Dezalay ◽  
O. Godet ◽  
A. Klotz ◽  
D. Turpin ◽  
...  
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Birth Rate ◽  
Gamma Ray ◽  
Reference Model ◽  
Stellar Mass ◽  
Gamma Ray Bursts ◽  
Birth Rates ◽  
Binary Black Hole ◽  
History Of

Context. Gravitational wave interferometers have proven the existence of a new class of binary black hole (BBH) weighing tens of solar masses, and have provided the first reliable measurement of the rate of coalescing black holes (BHs) in the local Universe. Furthermore, long gamma-ray bursts (GRBs) detected with gamma-ray satellites are believed to be associated with the birth of stellar-mass BHs, providing a measure of the rate of these events across the history of the Universe, thanks to the measure of their cosmological redshift. These two types of sources, which are subject to different detection biases and involve BHs born in different environments with potentially different characteristics, provide complementary information on the birth rate of stellar BHs. Aims. We compare the birth rates of BHs found in BBH mergers and in long GRBs. Methods. We construct a simple model that makes reasonable assumptions on the history of GRB formation, and takes into account some major uncertainties, like the beaming angle of GRBs or the delay between the formation of BBHs and their coalescence. We use this model to evaluate the ratio of the number of stellar mass BHs formed in BBH mergers to those formed in GRBs. Results. We find that in our reference model the birth rate of stellar BHs in BBH mergers represents a significant fraction of the rate of long GRBs and that comparable birth rates are favored by models with moderate beaming angles. These numbers, however, do not consider subluminous GRBs, which may represent another population of sources associated with the birth of stellar mass BHs. We briefly discuss this result in view of our understanding of the progenitors of GRBs and BBH mergers, and we emphasize that this ratio, which will be better constrained in the coming years, can be directly compared with the prediction of stellar evolution models if a single model is used to produce GRBs and BBH mergers with the same assumptions.

Reflective black holes

2021 ◽  
pp. 2150200
Author(s):  
Revaz Beradze ◽  
Merab Gogberashvili ◽  
Lasha Pantskhava
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Gravitational Waves ◽  
Gamma Ray ◽  
Gamma Ray Bursts ◽  
Radio Bursts ◽  
Hole Model

In this paper, a brief analysis of repeated and overlapped gamma-ray bursts, fast radio bursts and gravitational waves is done. These signals may not be emitted by isolated cataclysmic events and we suggest interpreting some of them within the impenetrable black hole model, as the radiation reflected and amplified by the black hole horizons.

scholarly journals The astrophysical odds of GW151216

2020 ◽  
Vol 498 (2) ◽  
pp. 1905-1910 ◽  
Author(s):  
Gregory Ashton ◽  
Eric Thrane
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Gravitational Wave ◽  
Bayesian Method ◽  
Massive Stars ◽  
Stellar Mass ◽  
Population Analyses ◽  
Wave Detection ◽  
Binary Black Hole ◽  
Bona Fide

ABSTRACT The gravitational-wave candidate GW151216 is a proposed binary black hole event from the first observing run of the Advanced LIGO detectors. Not identified as a bona fide signal by the LIGO–Virgo collaboration, there is disagreement as to its authenticity, which is quantified by pastro, the probability that the event is astrophysical in origin. Previous estimates of pastro from different groups range from 0.18 to 0.71, making it unclear whether this event should be included in population analyses, which typically require pastro > 0.5. Whether GW151216 is an astrophysical signal or not has implications for the population properties of stellar-mass black holes and hence the evolution of massive stars. Using the astrophysical odds, a Bayesian method that uses the signal coherence between detectors and a parametrized model of non-astrophysical detector noise, we find that pastro = 0.03, suggesting that GW151216 is unlikely to be a genuine signal. We also analyse GW150914 (the first gravitational-wave detection) and GW151012 (initially considered to be an ambiguous detection) and find pastro values of 1 and 0.997, respectively. We argue that the astrophysical odds presented here improve upon traditional methods for distinguishing signals from noise.

scholarly journals Observational evidence for stellar-mass black holes

2006 ◽  
Vol 2 (S238) ◽  
pp. 3-12 ◽  
Author(s):  
Jorge Casares
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Mass Spectrum ◽  
Radial Velocity ◽  
Stellar Mass ◽  
Observational Evidence ◽  
X Ray ◽  
History Of ◽  
X Ray Binaries ◽  
Dynamical Masses

AbstractRadial velocity studies of X-ray binaries provide the most solid evidence for the existence of stellar-mass black holes. We currently have 20 confirmed cases, with dynamical masses in excess of 3 M⊙. Accurate masses have been obtained for a subset of systems which gives us a hint at the mass spectrum of the black hole population. This review summarizes the history of black hole discoveries and presents the latest results in the field.

Gamma-ray bursts from stellar mass accretion disks around black holes

1993 ◽  
Vol 405 ◽  
pp. 273 ◽  
Author(s):  
S. E. Woosley
Keyword(s):  
Black Holes ◽  
Accretion Disks ◽  
Gamma Ray ◽  
Stellar Mass ◽  
Gamma Ray Bursts

scholarly journals Recent searches for continuous gravitational waves

2017 ◽  
Vol 32 (39) ◽  
pp. 1730035 ◽  
Author(s):  
Keith Riles
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Neutron Star ◽  
Gravitational Waves ◽  
Gamma Ray ◽  
Continuous Wave ◽  
New Era ◽  
Binary Neutron Star ◽  
Binary Black Hole ◽  
Bose Einstein

Gravitational wave astronomy opened dramatically in September 2015 with the LIGO discovery of a distant and massive binary black hole coalescence. The more recent discovery of a binary neutron star merger, followed by a gamma ray burst (GRB) and a kilonova, reinforces the excitement of this new era, in which we may soon see other sources of gravitational waves, including continuous, nearly monochromatic signals. Potential continuous wave (CW) sources include rapidly spinning galactic neutron stars and more exotic possibilities, such as emission from axion Bose Einstein “clouds” surrounding black holes. Recent searches in Advanced LIGO data are presented, and prospects for more sensitive future searches are discussed.

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

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.

scholarly journals EVOLUTIONS OF STELLAR-MASS BLACK HOLE HYPERACCRETION SYSTEMS IN THE CENTER OF GAMMA-RAY BURSTS

2015 ◽  
Vol 815 (1) ◽  
pp. 54 ◽  
Author(s):  
Cui-Ying Song ◽  
Tong Liu ◽  
Wei-Min Gu ◽  
Shu-Jin Hou ◽  
Jian-Xiang Tian ◽  
...  
Keyword(s):  
Black Hole ◽  
Gamma Ray ◽  
Stellar Mass ◽  
Gamma Ray Bursts

scholarly journals Similar phenomena at different scales: black holes, the Sun, γ-ray bursts, supernovae, galaxies and galaxy clusters

2006 ◽  
Vol 2 (14) ◽  
pp. 41-62 ◽  
Author(s):  
Shuang Nan Zhang
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Gamma Ray ◽  
Gamma Ray Bursts ◽  
The Sun ◽  
Physical Processes ◽  
X Ray ◽  
Physical Mechanisms ◽  
X Ray Binaries ◽  
Fundamental Physical

AbstractMany similar phenomena occur in astrophysical systems with spatial and mass scales different by many orders of magnitudes. For examples, collimated outflows are produced from the Sun, proto-stellar systems, gamma-ray bursts, neutron star and black hole X-ray binaries, and supermassive black holes; various kinds of flares occur from the Sun, stellar coronae, X-ray binaries and active galactic nuclei; shocks and particle acceleration exist in supernova remnants, gamma-ray bursts, clusters of galaxies, etc. In this report I summarize briefly these phenomena and possible physical mechanisms responsible for them. I emphasize the importance of using the Sun as an astrophysical laboratory in studying these physical processes, especially the roles magnetic fields play in them; it is quite likely that magnetic activities dominate the fundamental physical processes in all of these systems.As a case study, I show that X-ray lightcurves from solar flares, black hole binaries and gamma-ray bursts exhibit a common scaling law of non-linear dynamical properties, over a dynamical range of several orders of magnitudes in intensities, implying that many basic X-ray emission nodes or elements are inter-connected over multi-scales. A future high timing and imaging resolution solar X-ray instrument, aimed at isolating and resolving the fundamental elements of solar X-ray lightcurves, may shed new lights onto the fundamental physical mechanisms, which are common in astrophysical systems with vastly different mass and spatial scales. Using the Sun as an astrophysical laboratory, “Applied Solar Astrophysics” will deepen our understanding of many important astrophysical problems.

BLACK HOLE ENERGETICS AND THE PRODUCTION OF GAMMA RAY BURSTS

1999 ◽  
Vol 08 (01) ◽  
pp. 23-42
Author(s):  
MARINA GIBILISCO
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Energy Loss ◽  
Gamma Ray ◽  
Gamma Ray Bursts ◽  
Discharge Process ◽  
Inhomogeneous Distribution ◽  
Charged Black Holes ◽  
Rotating Black Holes ◽  
Kinetic Energy Loss

In this paper I study the energetics of massive, charged black holes, pointing out the importance of the discharge process in increasing the energy loss of these objects. The decrement of the energy of a black hole is due to three contributions, namely the Hawking evaporation, the kinetic energy loss (for rotating black holes) and the pair production following the discharge process (for charged black holes). Here I evaluate the energy balance for Kerr, Kerr–Newman and Reissner–Nordström black holes, showing that, even if the discharge process is very fast, it can increase in a significant way the energy loss: that enables the emission of gamma ray bursts whose characteristics are similar to those of the experimentally observed bursts. Following this idea, one can explain in a quite satisfactory way both the peculiar bimodality observed in the gamma ray burst duration and their isotropic but inhomogeneous distribution.

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