X-ray nova in Musca (GRS 1124 - 68) - Hard X-ray source with narrow annihilation line

Sunyaev, R.; Churazov, E.; Gilfanov, M.; Dyachkov, A.; Khavenson, N.; Гребенев, С. А.; Kremnev, R. S.; Sukhanov, K. G.; Goldwurm, A.; Ballet, J.; Cordier, B.; Paul, Jacques; Denis, M.; Védrenne, G.; Niel, M.; Jourdain, E.

doi:10.1086/186352

Cited by 76 publications

(27 citation statements)

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“…Evidently, to produce pair‐dominated jets pair production has to dominate the pair annihilation process, as has been theoretically investigated by Mishra & Melia (1993) and Yamasaki et al (1999). Observationally, electron–positron jets were suggested in the galactic black hole candidate Nova Muscae 1991/GS 1124–684 (Sunyaev et al 1992), GRS 1915+105 (Mirabel & Rodriguez 1998), and in quasar 3C 279 (Wardle et al 1998). Though there is little doubt about the existence of pair‐dominated jets, radiative acceleration/collimation of such jets, on the other hand, is a different issue altogether.…”

Section: Discussion and Concluding Remarksmentioning

confidence: 91%

Radiatively driven rotating pair-plasma jets from two-component accretion flows

Chattopadhyay

2005

Monthly Notices of the Royal Astronomical Society

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Centrifugal pressure of matter spiralling on to black holes has long been known to produce standing or oscillating shocks. The post‐shock disc puffs up in the form of a torus, which intercepts soft photons from the outer Keplerian disc and inverse‐Comptonizes them to produce hard photons. The post‐shock region also produces jets. We study the interaction of both hard photons and soft photons, with rotating electron–positron jets. We show that hard photons from the post‐shock torus are instrumental in acceleration of jets, while soft photons from the Keplerian disc is a better collimating agent. We also show that if the jets are launched closer to the black hole, relativistic and collimated jets are produced; if they are launched at larger distances both collimation and acceleration are less. We also show that if the shock location is at relatively larger distances from the black hole, collimation is better.

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Section: Discussion and Concluding Remarksmentioning

confidence: 91%

Radiatively driven rotating pair-plasma jets from two-component accretion flows

Chattopadhyay

2005

Monthly Notices of the Royal Astronomical Society

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“…The annihilation feature observed persists for at least 10 h (Sunyaev et al 1992). The production of an outflow must have lasted at least for that length of time.…”

Section: Implications Of a Bipolar Flowmentioning

confidence: 87%

“…The rate of annihilation implied by the line flux is _ N þ , 2 £ 10 43 pairs s 21 for a distance of 5.5 kpc (Orosz et al 1996). This enormous rate is sustained for at least 10 h (Sunyaev et al 1992). It is therefore very unlikely that this feature at 474 keV arises from a large number of pairs formed practically instantaneously and then slowly annihilating away.…”

Section: Constraints From the Annihilation Linementioning

confidence: 98%

“…Nova Muscae (GRS 1124 2 684Þ was discovered on 1991 January 8 with Granat (Lund & Brandt 1991;Sunyaev 1991) and Ginga (Makino 1991). An extensive monitoring campaign with Granat covering most of 1991 January and February followed this initial discovery (Gil'fanov et al 1991, hereafter GSC91;Sunyaev et al 1992;Gil'fanov et al 1993). During observations on January 20 -21, a strong, narrow line near 500 keV was detected.…”

Section: T H E C a S E O F N Ova M U S C A Ementioning

confidence: 99%

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Pair annihilation and radio emission from galactic jet sources: the case of Nova Muscae

Kaiser¹,

Hannikainen²

2002

Monthly Notices of the Royal Astronomical Society

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In the hard X‐ray spectra of some X‐ray binaries line features at around 500 keV are detected. We interpret these as arising from pair annihilation in relativistic outflows leading to a significant Doppler shift of the frequencies of the lines. We show how this can be used to accurately determine the bulk velocity and orientation to the line of sight of the outflows. Constraints on the energy requirements of such outflows are also derived. Furthermore, we show that a small fraction of pairs escaping the annihilation region may give rise to the radio synchrotron emission observed in some of these objects. We apply these ideas to the hard X‐ray and radio observations of Nova Muscae 1991. In this object, the energy requirements seem to rule out a large proton fraction in the outflows.

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“…Paschen lines were also observed in SS 433 (Filippenko et al 1988). Possible pair-annihilation lines were also detected in IE 1740.7-2942 Sunyaev et al 1991) and in the X-ray Nova Musucae 1991 (Sunyaev et al 1992;Goldwurm et al 1992).…”

Section: Introductionmentioning

confidence: 82%

Line Spectrum from Advection-Dominated Accretion Disks

Fukue¹,

Ohna²

1997

Publications of the Astronomical Society of Japan

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The emission-line profiles from advection-dominated accretion disks were calculated for a wide variety of parameters. As a model of advection-dominated disks, we adopted a self-similar solution by Narayan and Yi (1994, AAA 61.064.083) and a beta disk driven by radiation drag by Fukue and Umemura (1995, AAA 64.064.034). The emissivity assumed was a power of the radius. The parameters are then the size of the emitting regions, the power index of the emissivity, and the inclination angle, except for a few parameters inherent in each model. The line profiles in advection-dominated cases, like those from a Keplerian disk, are generally double peaked, partly due to the rotational motion and partly due to the radial infall motion. In a Keplerian disk and a self-similar disk the separation of peaks depends on the size of the emitting regions, whereas does not depend on the size so much in the beta disk. One of the strategies to distinguish these models is to observe the separation for the different species, which originate in different regions on the disk. In addition, the separation for advection-dominated accretion disks is systematically small, since the rotational velocity is generally smaller than the Keplerian velocity. In profile variations during an eclipse a blue peak disappears at first and a red peak follows in the Keplarian disks, while both peaks change simultaneously in avection-dominated accretion disks. This can be another strategy to discriminate models.

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X-ray nova in Musca (GRS 1124 - 68) - Hard X-ray source with narrow annihilation line

Cited by 76 publications

References 0 publications

Radiatively driven rotating pair-plasma jets from two-component accretion flows

Radiatively driven rotating pair-plasma jets from two-component accretion flows

Pair annihilation and radio emission from galactic jet sources: the case of Nova Muscae

Line Spectrum from Advection-Dominated Accretion Disks

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