Discovery and observations by watch of the X-ray transient GRS 1915+105

Castro‐Tirado, Alberto J.; Brandt, S.; Lund, N.; Lapshov, I.; Sunyaev, R.; Shlyapnikov, A. A.; Guziy, S.; Павленко, Е. П.

doi:10.1086/191998

Cited by 130 publications

(80 citation statements)

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“…GRS 1915+105 is a Galactic X-ray binary in the Aquila constellation (l = 45.37 • , b = −0.22 • ), discovered on 15 August 1992 by the WATCH all-sky X-ray monitor on board the GRANAT satellite (Castro-Tirado et al 1994).…”

Section: Grs 1915+105 and Its Optical Extinctionmentioning

confidence: 99%

On the optical extinction and distance of GRS 1915+105

Chapuis

Corbel

2004

A&A

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Abstract. Based on new millimeter and radio observations, we reevaluate the total hydrogen column density along the line of sight to the microquasar GRS 1915+105 to N H = (3.5±0.3)×10 22 cm −2 . Our value is consistent with the one derived from X-ray measurements, namely (3.8 ± 0.3) × 10 22 cm −2 (Ebisawa et al. 1998). Using the empirical law between the visual extinction and the total column density of hydrogen, A v is found to 19.6 ± 1.7 mag. This result is ∼7 mag lower than previously thought, and therefore, a reevaluation of infrared fluxes after derredening is needed. The revisited kinematic study allows to give a lower limit to the distance of GRS 1915+105 , namely 6.0 kpc. Taking into account the most accurate upper limit of distance inferred from radio data (11.2 ± 0.8 kpc, Fender et al. 1999) as well as this lower limit, this implies a distance of 9.0 ± 3.0 kpc.

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Section: Grs 1915+105 and Its Optical Extinctionmentioning

confidence: 99%

On the optical extinction and distance of GRS 1915+105

Chapuis

Corbel

2004

A&A

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“…The microquasar GRS 1915+105 remains one of the most exotic and variable objects in the X-ray, IR and radio spectrum bands since its discovery (Castro-Tirado et al 1994). A major accomplishment has been the implied connection between the jet and the accretion disk as interpreted through modelling of its X-ray variability (Belloni et al 1997;Klein-Wolt et al 2002).…”

Section: Introductionmentioning

confidence: 99%

The rotational broadening and the mass of the donor star of GRS 1915+105

Harlaftis

Greiner

2004

A&A

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Abstract. The binary parameters of the microquasar GRS 1915+105 have been determined by the detection of Doppler-shifted 12 CO and 13 CO lines in its K-band spectrum (Greiner et al. 2001b). Here, we present further analysis of the same K-band VLT spectra and we derive a rotational broadening of the donor star of υ sin i = 26±3 km s −1 from the 12 CO/ 13 CO lines. Assuming that the K-type star is tidally locked to the black hole and is filling its Roche-lobe surface, then the implied mass ratio is q = M d Mx = 0.058 ± 0.033. This result, combined with (P, K, i) = (33.5 d, 140 km s −1 , 66 • ) gives a more refined mass estimate for the black hole, M x = 14.0 ± 4.4 M , than previously estimated, using an inclination of i = 66 • ± 2 • (Fender et al. 1999) as derived from the orientation of the radio jets and a more accurate distance. The mass for the early K-type giant star is M d = 0.81 ± 0.53 M , consistent with a more evolved stripped-giant donor star in GRS 1915+105 than, for example, the donor star of the prototype black-hole X-ray transient, V404 Cyg which has the longest binary period after GRS 1915+105.

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“…GRS 1915+105 (Castro-Tirado et al 1994) is the prototypical microquasar, a galactic X-ray binary ejecting plasma clouds at v ≈ 0.92 c (Mirabel & Rodriguez 1994). It exhibits unique X-ray variability patterns (Greiner et al 1996) which have been interpreted as accretion disk instabilities leading to an infall of parts of the inner accretion disk (Belloni et al 1997).…”

Section: Introductionmentioning

confidence: 99%

Identification of the donor in the X-ray binary GRS 1915+105

Greiner

Cuby²,

McCaughrean

et al. 2001

A&A

110

103

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Abstract. We report on the results of medium-resolution spectroscopy of GRS 1915+105 in the near-infrared H and K band using the 8 m VLT at ESO. We clearly identify absorption bandheads from 12 CO and 13 CO. Together with other features this results in a classification of the mass-donating star in this binary as a K-M III star, clearly indicating that GRS 1915+105 belongs to the class of low-mass X-ray binaries (LMXB).

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Discovery and observations by watch of the X-ray transient GRS 1915+105

Cited by 130 publications

References 1 publication

On the optical extinction and distance of GRS 1915+105

On the optical extinction and distance of GRS 1915+105

The rotational broadening and the mass of the donor star of GRS 1915+105

Identification of the donor in the X-ray binary GRS 1915+105

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