Production of the large scale superluminal ejections of the microquasar GRS 1915+105 by violent magnetic reconnection

Details Production of the large scale superluminal ejections of the microquasar GRS 1915+105 by violent magnetic reconnection Production of the large scale superluminal ejections of the microquasar GRS 1915+105 by violent magnetic reconnection

Oct 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005a%26a...441..845d&link_type=abstract

Astronomy and Astrophysics, Volume 441, Issue 3, October III 2005, pp.845-853

Physics

44

Acceleration Of Particles, Accretion, Accretion Disks, Black Hole Physics, Magnetic Fields

Scientific paper

We propose here that the large-scale superluminal ejections observed in the galactic microquasar GRS 1915+105 during radio flare events are produced by violent magnetic reconnection episodes in the corona just above the inner edge of the magnetized accretion disk that surrounds the central 10 M&sun; black hole. The process occurs when a large-scale magnetic field is established by a turbulent dynamo in the inner disk region with a ratio between the gas+radiation and the magnetic pressures β ≃ 1, implying a magnetic field intensity of 7 × 108 G. During this process, substantial angular momentum is removed from the disk by the wind generated by the vertical magnetic flux therefore increasing the disk mass accretion to a value near (but below) the critical one (dot M ˜ 1019 g s-1). Part of the magnetic energy released by reconnection heats the coronal gas (Tc ≲ 5 × 108 K) that produces a steep X-ray spectrum with luminosity LX ≃ 1039 erg s- 1, consistent with observations. The remaining magnetic energy released goes to accelerate the particles to relativistic velocities (v ˜ vA ˜ c, where vA is the Alfvén speed) in the reconnection site through first-order Fermi processes. In this context, two possible mechanisms have been examined that produce power-law electron distributions N(E) ∝ E-α_E, with αE = 5/2, 2, and corresponding synchrotron radio power-law spectra with spectral indices which are compatible with that observed during the flares ( Sν ∝ ν-0.75, - 0.5).

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