The runaway black hole GRO J1655-40

Mirabel, I. F.; Mignani, Roberto; Rodrigues, I.; Combi, J. A.; Rodriguez, L.F.; Guglielmetti, Fabrizia

doi:10.1051/0004-6361:20021440

Cited by 82 publications

(116 citation statements)

References 30 publications

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“…Very recently, multiple wavelength observations of GRO J1655-40 were used to determine its velocity and possible origin in the sky [39]. From these observations, providing the first direct evidence for stellar black hole formation in supernovae explosions, one can estimate the age of the black hole to be 0.7 Myr [39]. Altogether this gives only a mild bound on L < ∼ 0.2 mm, comparable to table-top experiments.…”

Section: The Evaporation Time Of Large Black Holesmentioning

confidence: 86%

“…Since the rate at which the companion loses matter towards the accretion disk is known, one can place the limit of < ∼ 10 6 yr on the age of the black hole [37,38]. Very recently, multiple wavelength observations of GRO J1655-40 were used to determine its velocity and possible origin in the sky [39]. From these observations, providing the first direct evidence for stellar black hole formation in supernovae explosions, one can estimate the age of the black hole to be 0.7 Myr [39].…”

Section: The Evaporation Time Of Large Black Holesmentioning

confidence: 99%

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Black Hole Astrophysics in AdS Braneworlds

Emparan¹,

García-Bellido²,

Kaloper³

2003

J. High Energy Phys.

101

102

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We consider astrophysics of large black holes localized on the brane in the infinite RandallSundrum model. Using their description in terms of a conformal field theory (CFT) coupled to gravity, deduced in Ref.[1], we show that they undergo a period of rapid decay via Hawking radiation of CFT modes. For example, a black hole of mass few × M ⊙ would shed most of its mass in ∼ 10 4 − 10 5 years if the AdS radius is L ∼ 10 −1 mm, currently the upper bound from table-top experiments. Since this is within the mass range of X-ray binary systems containing a black hole, the evaporation enhanced by the hidden sector CFT modes could cause the disappearance of X-ray sources on the sky. This would be a striking signature of RS2 with a large AdS radius. Alternatively, for shorter AdS radii, the evaporation would be slower. In such cases, the persistence of X-ray binaries with black holes already implies an upper bound on the AdS radius of L < ∼ 10 −2 mm, an order of magnitude better than the bounds from table-top experiments. The observation of primordial black holes with a mass in the MACHO range M ∼ 0.1 − 0.5 M ⊙ and an age comparable to the age of the universe would further strengthen the bound on the AdS radius to L < ∼ few × 10 −6 mm. 1 roberto.emparan@cern.ch 2

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Section: The Evaporation Time Of Large Black Holesmentioning

confidence: 86%

Section: The Evaporation Time Of Large Black Holesmentioning

confidence: 99%

Black Hole Astrophysics in AdS Braneworlds

Emparan¹,

García-Bellido²,

Kaloper³

2003

J. High Energy Phys.

101

102

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“…However, the discovery of BH X-ray binaries with high spatial velocities (e.g. Mirabel et al 2001Mirabel et al , 2002, points to a similar birth velocity distribution for NSs and BHs. Hence, in this work we assume that BHs have the same velocity distribution of NSs.…”

Section: Isolated Compact Remnantsmentioning

confidence: 99%

Probing isolated compact remnants with microlensing

Sartore

Treves

2010

A&A

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Aims. We consider isolated compact remnants (ICoRs), i.e. neutrons stars and black holes that do not reside in binary systems and therefore cannot be detected as X-ray binaries. ICoRs may represent ∼5 percent of the stellar mass budget of the Galaxy, but they are very hard to detect. Here we explore the possibility of using microlensing to identify ICoRs. Methods. In a previous paper we described a simulation of neutron star evolution in phase space in the Galaxy, taking into account the distribution of the progenitors and the kick at formation. Here we first reconsider the evolution and distribution of neutron stars and black holes with an added a bulge component. From the new distributions we calculate the microlensing optical depth, event rate and distribution of event time scales, comparing and contrasting the case of ICoRs and "normal stars". Results. We find that the contribution of remnants to optical depth is slightly lower than without kinematics, owing to the evaporation from the Galaxy. On the other hand, the relative contribution to the rate of events is a factor ∼5 higher. In all, ∼6−7 percent of the events are likely related to ICoRs. In particular, ∼30−40 percent of the events with duration >100 days are possibly related to black holes. Conclusions. It seems therefore that microlensing observations are a suitable tool to probe the population of Galactic ICoRs.

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“…Ribó et al 2002;Dhawan et al 2007;Miller-Jones et al 2009a). Of particular interest are the runaway systems, which have acquired very high peculiar velocities (Mirabel et al 2001(Mirabel et al , 2002. With enough information, a complete evolutionary history of the binary system can be obtained with constraints on the progenitor and the formation of the compact object, (see e.g.…”

Section: Introductionmentioning

confidence: 99%

On the origin of LS 5039 and PSR J1825−1446

Moldón

Ribó

Paredes

et al. 2012

A&A

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Context. The gamma-ray binary LS 5039 and the isolated pulsar PSR J1825−1446 were proposed to have been formed in the supernova remnant (SNR) G016.8−01.1. Aims. We aim to obtain the Galactic trajectory of LS 5039 and PSR J1825−1446 to find their origin in the Galaxy, and in particular to check their association with SNR G016.8−01.1 to restrict their age. Methods. By means of radio and optical observations we obtained the proper motion and the space velocity of the sources. Results. The proper motion of PSR J1825−1446 corresponds to a transverse space velocity of 690 km s −1 at a distance of 5 kpc. Its Galactic velocity at different distances is not compatible with the expected Galactic rotation. The velocity and characteristic age of PSR J1825−1446 make it incompatible with SNR G016.8−01.1. There are no clear OB associations or SNRs crossing the past trajectory of PSR J1825−1446. We estimate the age of the pulsar to be 80-245 kyr, which is compatible with its characteristic age. The proper motion of LS 5039 is μ α cos δ = 7.09 and μ δ = −8.82 mas yr −1 . The association of LS 5039 with SNR G016.8−01.1 is unlikely, although we cannot discard it. The system would have had to be formed in the association Ser OB2 (at 2.0 kpc) if the age of the system is 1.0-1.2 Myr, or in the association Sct OB3 (distance 1.5-2 kpc) for an age of 0.1-0.2 Myr. If the system were not formed close to Ser OB2, the pseudo-synchronization of the orbit would be unlikely. Conclusions. PSR J1825−1446 is a high-velocity isolated pulsar ejected from the Galaxy. The distance to LS 5039, which needs to be constrained by future astrometric missions such as Gaia, is a key parameter for restricting its origin and age.

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The runaway black hole GRO J1655-40

Cited by 82 publications

References 30 publications

Black Hole Astrophysics in AdS Braneworlds

Black Hole Astrophysics in AdS Braneworlds

Probing isolated compact remnants with microlensing

On the origin of LS 5039 and PSR J1825−1446

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