Near-infrared jets in the Galactic microquasar GRS1915+105

Sams, B.; Eckart, A.; Sunyaev, R.

doi:10.1038/382047a0

Cited by 81 publications

(85 citation statements)

References 24 publications

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“…It is also possible that additional emission results from electrons that were re-accelerated in optically thin regions away from the reconnection zone (behind shock waves along the jet excited by the plasmon clouds, as emphasized above). This idea is supported for instance by IR observations of GRS 1915+105, which indicate a separation between the IR emission and the central source ∼0.2 arcsec or ∼2500 AU at 12.5 kpc (Sams et al 1996), i.e., further away from the predicted launching region by the present model (Fig. 2).…”

Section: X-ray Emissionsupporting

confidence: 68%

The role of magnetic reconnection on jet/accretion disk systems

Pino¹,

Piovezan

Kadowaki³

2010

A&A

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Context. It was proposed earlier that the relativistic ejections observed in microquasars could be produced by violent magnetic reconnection episodes at the inner disk coronal region (de Gouveia Dal Pino & Lazarian 2005). Aims. Here we revisit this model, which employs a standard accretion disk description and fast magnetic reconnection theory, and discuss the role of magnetic reconnection and associated heating and particle acceleration in different jet/disk accretion systems, namely young stellar objects (YSOs), microquasars, and active galactic nuclei (AGNs). Methods. In microquasars and AGNs, violent reconnection episodes between the magnetic field lines of the inner disk region and those that are anchored in the black hole are able to heat the coronal/disk gas and accelerate the plasma to relativistic velocities through a diffusive first-order Fermi-like process within the reconnection site that will produce intermittent relativistic ejections or plasmons.Results. The resulting power-law electron distribution is compatible with the synchrotron radio spectrum observed during the outbursts of these sources. A diagram of the magnetic energy rate released by violent reconnection as a function of the black hole (BH) mass spanning 10 9 orders of magnitude shows that the magnetic reconnection power is more than sufficient to explain the observed radio luminosities of the outbursts from microquasars to low luminous AGNs. In addition, the magnetic reconnection events cause the heating of the coronal gas, which can be conducted back to the disk to enhance its thermal soft X-ray emission as observed during outbursts in microquasars. The decay of the hard X-ray emission right after a radio flare could also be explained in this model due to the escape of relativistic electrons with the evolving jet outburst. In the case of YSOs a similar magnetic configuration can be reached that could possibly produce observed X-ray flares in some sources and provide the heating at the jet launching base, but only if violent magnetic reconnection events occur with episodic, very short-duration accretion rates which are ∼100−1000 times larger than the typical average accretion rates expected for more evolved (T Tauri) YSOs.

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Section: X-ray Emissionsupporting

confidence: 68%

The role of magnetic reconnection on jet/accretion disk systems

Pino¹,

Piovezan

Kadowaki³

2010

A&A

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“…Infrared jets were discovered [23], and infrared flares were seen to occur after radio flares [8,14]. These investigations provide solid evidence that the infrared flares represent synchrotron emission from rapidly evolving jets.…”

Section: Clues For the Origin Of Jets In Grs1915+105mentioning

confidence: 63%

Monitoring the Galactic microquasars with RXTE

Remillard¹,

Morgan

1999

Nuclear Physics B - Proceedings Supplements

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The Galactic microquasars GRS1915+105 and GRO J1655-40 were targets for dedicated monitoring programs with RXT E throughout 1996 and 1997. We review recent results with particular attention to the X-ray QPOs seen in these sources. We confirm the reappearance of 67 Hz oscillations in GRS1915+105 in several different spectral states. Six intervals, each of 1 to 6 months duration, yield QPO detections with a central frequency of 66.7 ± 1.4 Hz and a FWHM of 3.4 ± 1.0 Hz. Comparing these observing intervals, the average X-ray luminosity varies by a factor of 4 with no significant change in the central QPO frequency. GRS1915+105 has been active in X-rays since 1992, and it shows no signs of evolving toward quiescence. In contrast, GRO J1655-40, which began its most recent X-ray outburst on 1996 April 25, is seen to fade below 20 mCrab on 1997 Aug 17. There are no reappearances of the 300 Hz QPO during the entire second half of the X-ray outburst; during this time the X-ray spectrum is dominated by the soft, thermal component. There are still several models seeking to explain the high frequency QPOs in microquasars. While it is likely that the cause invokes some effect of General Relativity, the correct model and the details of the emission mechanism remain uncertain.

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“…For a black hole of mass M the density and mean temperature in the accretion flow scale with M −1 and M −1/4 , respectively. The maximum magnetic field at a given radius in a radiation dominated accretion disk scales with M −1/2 , which implies that in the vicinity of stellar-mass black holes the magnetic fields may be 10 4 times stronger than that found near supermassive black holes [131].…”

Section: Microquasars and Jetsmentioning

confidence: 99%

Atomic X-ray spectroscopy of accreting black holes

Liedahl¹,

Torres²

2005

Can. J. Phys.

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Current astrophysical research suggests that the most persistently luminous objects in the Universe are powered by the flow of matter through accretion disks onto black holes. Accretion disk systems are observed to emit copious radiation across the electromagnetic spectrum, each energy band providing access to rather distinct regimes of physical conditions and geometric scale. X-ray emission probes the innermost regions of the accretion disk, where relativistic effects prevail. While this has been known for decades, it also has been acknowledged that inferring physical conditions in the relativistic regime from the behavior of the X-ray continuum is problematic and not satisfactorily constraining. With the discovery in the 1990s of iron X-ray lines bearing signatures of relativistic distortion came the hope that such emission would more firmly constrain models of disk accretion near black holes, as well as provide observational criteria by which to test general relativity in the strong field limit. Here we provide an introduction to this phenomenon. While the presentation is intended to be primarily tutorial in nature, we aim also to acquaint the reader with trends in current research. To achieve these ends, we present the basic applications of general relativity that pertain to X-ray spectroscopic observations of black hole accretion disk systems, focusing on the Schwarzschild and Kerr solutions to the Einstein field equations. To this we add treatments of the fundamental concepts associated with the theoretical and modeling aspects of accretion disks, as well as relevant topics from observational and theoretical X-ray spectroscopy. PACS Nos.: 32.30. Rj, 32.80.Hd, 95.30.Dr, 95.30.Sf, 95.85.Nv, 97.10.Gz. 97.80.Jp, 98.35.Mp, 98.62.Mw

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Near-infrared jets in the Galactic microquasar GRS1915+105

Cited by 81 publications

References 24 publications

The role of magnetic reconnection on jet/accretion disk systems

The role of magnetic reconnection on jet/accretion disk systems

Monitoring the Galactic microquasars with RXTE

Atomic X-ray spectroscopy of accreting black holes

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