Evidence of a supernova origin for the black hole in the system GRO J1655 - 40

Israelian, G.; Rebolo, R.; Basri, Gibor; Casares, J.; Martín, E. L.

doi:10.1038/43625

Cited by 189 publications

(251 citation statements)

References 12 publications

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“…In the interim, the abundance excesses for X-ray absorption edges in GRS 1915]105 can be contrasted with the discovery of abundance anomalies in the optical spectra of companion stars in the microquasars GRO J1655[40 and V4641 Sgr (Israelian et al 1999 ;Brown et al 2000 ;Orosz et al 2001). In the latter cases, the overabundances of aprocess elements, but not the Fe group, have led to the hypothesis that the companion star captured supernova or hypernova ejecta is related to the formation of the black hole.…”

Section: Discussionmentioning

confidence: 99%

High‐ResolutionChandraHETGS andRossi X‐Ray Timing ExplorerObservations of GRS 1915+105: A Hot Disk Atmosphere and Cold Gas Enriched in Iron and Silicon

Lee

Reynolds

Remillard

et al. 2002

ApJ

220

284

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The time-averaged 30 ks Chandra AO1 High Energy Transmission Grating Spectrometer observation of the microquasar GRS 1915]105 in the low hard state reveals for the Ðrst time in this source neutral K absorption edges from iron, silicon, magnesium, and sulphur. Ionized resonance (r) absorption from H-and He-like species of Fe (XXV, XXVI) and possibly Ca XX are also seen as well as possible emission from neutral Fe Ka and ionized Fe XXV (forbidden or the resonance emission component of a P Cygni proÐle). We report the tentative detection of the Ðrst astrophysical signature of X-ray absorption Ðne structure in the photoelectric edge of Si (and possibly Fe and Mg) attributed to material in grains. The large column densities measured from the neutral edges reveal anomalous Si and Fe abundances and illustrate the importance of high-resolution X-ray measurements for assessing material that surrounds bright X-ray sources, especially if depletion onto grains plays a prominent role. Scenarios for which the anomalous abundances can be attributed to surrounding cold material associated with GRS 1915]105 and/or for which the enrichment may signify either a highly unusual supernova/hypernova or external supernova activity local to the binary are discussed. We attribute the ionized features to a hot disk, disk wind, or corona environment. Based on H-and He-like Fe (XXV, XXVI), we estimate constraints on the ionization parameter temperature (T [ 2.4 ] 106 K), and hydrogen equivalent number (log m Z 4.15), density cm~3) for this region. Variability studies with the simultaneous RXT E data show that (n Z 1012 the light-curve count rate tracks the changes in the disk blackbody as well as the power-law Ñux, with the most signiÐcant variations observed in the former. The Chandra data show spectral changes that also track the behavior of the light curve and may point to changes in both the ionizing Ñux and density of the absorber. A 3.69 Hz quasi-periodic oscillation and weak Ðrst harmonic are seen in the RXT E data.

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Section: Discussionmentioning

confidence: 99%

High‐ResolutionChandraHETGS andRossi X‐Ray Timing ExplorerObservations of GRS 1915+105: A Hot Disk Atmosphere and Cold Gas Enriched in Iron and Silicon

Lee

Reynolds

Remillard

et al. 2002

ApJ

220

284

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“…Its age can be estimated from a peculiar chemical abundance of the surface of the companion, with elements that can be traced back to a supernova explosion of type II. 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].…”

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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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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“…Cygnus X-1 (Mirabel & Rodrigues 2003b) and GRS 1915+105 (Israelian et al 1999), harbor high mass stellar BH´s (10 and 14 M ) and move in circular orbits, like massive disk stars. The kinematics of Cygnus X-1 implies that the progenitor of the BH was a > 25 M star, which collapsed via low energy supernova or prompt collapse.…”

Section: Resultsmentioning

confidence: 99%

The Galactic path of stellar black holes and neutron stars

Rodrigues

Mirabel

2004

Proc. IAU

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Abstract. The kinematics of black hole and neutron star X-ray binaries in the Galaxy should help to know their birth place and constrain their evolution. We have used multiple tools of modern astronomy to determine the trajectories in the Galaxy and track the origins of black hole and neutron star X-ray binaries that are of topical interest in astrophysics. We find three distinct classes of black hole and neutron star X-ray binaries: (1) low mass X-ray binaries that move at high velocities on galactocentric orbits similar to the most ancient stars born in the Galactic bulge and the halo, (2) those that move in the Galactic disk along paths that resemble the circular orbits of massive stars formed in the disk, and (3) high and intermediate mass X-ray binaries running away from their parent regions of star formation. Here we discuss some of the cases studied.

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Evidence of a supernova origin for the black hole in the system GRO J1655 - 40

Cited by 189 publications

References 12 publications

High‐ResolutionChandraHETGS andRossi X‐Ray Timing ExplorerObservations of GRS 1915+105: A Hot Disk Atmosphere and Cold Gas Enriched in Iron and Silicon

High‐ResolutionChandraHETGS andRossi X‐Ray Timing ExplorerObservations of GRS 1915+105: A Hot Disk Atmosphere and Cold Gas Enriched in Iron and Silicon

Black Hole Astrophysics in AdS Braneworlds

The Galactic path of stellar black holes and neutron stars

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