Spenser’s Inhumanity

Campana, Joseph

doi:10.7756/spst.030.017.277-99

Cited by 8 publications

(4 citation statements)

References 2 publications

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“…McDowell (1985) suggested that molecular clouds offer high density for spherically accreting BHs to produce detectable fluxes. Campana & Pardi (1993) estimated the number of BHs in the molecular clouds. Heckler & Kolb (1996) proposed a search strategy for isolated stellar mass BHs in the solar neighborhood using optical surveys.…”

Section: Appendix A: Comparison With Previous Workmentioning

confidence: 99%

GW 150914-like black holes as Galactic high-energy sources

Ioka

Matsumoto

Teraki

et al. 2017

Monthly Notices of the Royal Astronomical Society

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The first direct detections of gravitational waves (GWs) from black hole (BH) mergers, GW150914, GW151226 and LVT151012, give a robust lower limit ∼ 70000 on the number of merged, highly-spinning BHs in our Galaxy. The total spin energy is comparable to all the kinetic energy of supernovae that ever happened in our Galaxy. The BHs release the spin energy to relativistic jets by accreting matter and magnetic fields from the interstellar medium (ISM). By considering the distributions of the ISM density, BH mass and velocity, we calculate the luminosity function of the BH jets, and find that they can potentially accelerate TeV-PeV cosmic-ray particles in our Galaxy with total power ∼ 10 37±3 erg s −1 as PeVatrons, positron factories and/or unidentified TeV gamma-ray sources. Additional ∼ 300 BH jet nebulae could be detectable by CTA (Cherenkov Telescope Array). We also argue that the accretion from the ISM can evaporate and blow away cold material around the BH, which has profound implications for some scenarios to predict electromagnetic counterparts to BH mergers.

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Section: Appendix A: Comparison With Previous Workmentioning

confidence: 99%

GW 150914-like black holes as Galactic high-energy sources

Ioka

Matsumoto

Teraki

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…There have been many studies on the detectability of such accreting INSs (Ostriker et al 1970;Treves & Colpi 1991;Blaes & Madau 1993;Treves et al 2000;Perna et al 2003;Ikhsanov & Biermann 2007) and IBHs (Shvartsman 1971;Grindlay 1978;Carr 1979;McDowell 1985;Campana & Pardi 1993;Popov & Prokhorov 1998;Fujita et al 1998 Barkov et al 2012;Fender et al 2013;Ioka et al 2017;Matsumoto et al 2018). A number of observational searches have also been performed in the past for such accreting INSs and IBHs (Stocke et al 1995;Walter et al 1996;Wang 1997;Schwope et al 1999;Chisholm et al 2003;Muno et al 2006).…”

Section: Introductionmentioning

confidence: 99%

X-ray detectability of accreting isolated black holes in our Galaxy

Tsuna

Kawanaka

Totani

2018

Monthly Notices of the Royal Astronomical Society

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Detectability of isolated black holes (IBHs) without a companion star but emitting X-rays by accretion from dense interstellar medium (ISM) or molecular cloud gas is investigated. We calculate orbits of IBHs in the Galaxy to derive a realistic spatial distribution of IBHs, for various mean values of kick velocity at their birth υ avg . X-ray luminosities of these IBHs are then calculated considering various phases of ISM and molecular clouds, for a wide range of the accretion efficiency λ (a ratio of the actual accretion rate to the Bondi rate) that is rather uncertain. It is found that detectable IBHs mostly reside near the Galactic Centre (GC), and hence taking the Galactic structure into account is essential. In the hard X-ray band, where identification of IBHs from other contaminating X-ray sources may be easier, the expected number of IBHs detectable by the past survey by NuSTAR towards GC is at most order unity. However, 30-100 IBHs may be detected by the future survey by FORCE with an optimistic parameter set of υ avg = 50 km s −1 and λ = 0.1, implying that it may be possible to detect IBHs or constrain the model parameters.

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“…IBHs have thus mainly focused on accreting sources (Shvartsman 1971;McDowell 1985;Campana & Pardi 1993;Popov & Prokhorov 1998;Fujita et al 1998;Armitage & Natarajan 1999;Agol & Kamionkowski 2002;Maccarone 2005;Mii & Totani 2005;Barkov et al 2012;Fender et al 2013;Ioka et al 2017;Matsumoto et al 2018;Tsuna et al 2018). Although past searches using X-ray data have found candidates of accreting IBHs (Chisholm et al 2003;Muno et al 2006), no strong candidates are known at present.…”

Section: Introductionmentioning

confidence: 99%

Radio emission from accreting isolated black holes in our galaxy

Tsuna

Kawanaka

2019

Monthly Notices of the Royal Astronomical Society

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Apart from the few tens of stellar-mass black holes discovered in binary systems, an order of 10 8 isolated black holes (IBHs) are believed to be lurking in our Galaxy. Although some IBHs are able to accrete matter from the interstellar medium, the accretion flow is usually weak and thus radiatively inefficient, which results in significant material outflow. We study electron acceleration generated by the shock formed between this outflow and the surrounding material, and the subsequent radio synchrotron emission from accelerated electrons. By numerically calculating orbits of IBHs to obtain their spatial and velocity distributions, we estimate the number of IBHs detectable by surveys using SKA1-mid (SKA2) as ∼ 30 (∼ 700) for the most optimistic case. The SKA's parallax measurements may accurately give their distances, possibly shedding light on the properties of the black holes in our Galaxy.

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Spenser’s Inhumanity

Cited by 8 publications

References 2 publications

GW 150914-like black holes as Galactic high-energy sources

GW 150914-like black holes as Galactic high-energy sources

X-ray detectability of accreting isolated black holes in our Galaxy

Radio emission from accreting isolated black holes in our galaxy

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