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A Magnetic Model for Low/Hard States Associated with Jets in Black Hole X-Ray Binaries
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作者 Ding-Xiong Wang Jiu-Zhou Wang +1 位作者 zhao-ming gan Chang-Yin Huang 《International Journal of Astronomy and Astrophysics》 2012年第3期156-166,共11页
A model for the low/hard (LH) state associated with a steady jet in black hole X-ray binaries (BHXBs) is proposed based on disc-corona model with open magnetic fields trapped in magnetic patches, which arises from ‘f... A model for the low/hard (LH) state associated with a steady jet in black hole X-ray binaries (BHXBs) is proposed based on disc-corona model with open magnetic fields trapped in magnetic patches, which arises from ‘flux expulsion’ effect of convective turbulence. We fit the spectral profiles of the LH state for the BHXBs, 4U 1543-475, GX 339-4, XTE J1550-564 and GRO J1655-40, and fit the relation between jet power and X-ray luminosity dynamically in the LH state by adjusting accretion rate and the outer boundary of the corona over the disc. 展开更多
关键词 ACCRETION ACCRETION DISKS Black Hole Physics X-Rays BINARIES MAGNETIC FIELDS
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Triggering star formation by both radiative and mechanical AGN feedback
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作者 Chao Liu zhao-ming gan Fu-Guo Xie 《Research in Astronomy and Astrophysics》 SCIE CAS CSCD 2013年第8期899-911,共13页
We perform two dimensional hydrodynamic numerical simulations to study the positive active galactic nucleus (AGN) feedback which triggers, rather than suppresses, star formation. Recently, it was shown by Nayakshin ... We perform two dimensional hydrodynamic numerical simulations to study the positive active galactic nucleus (AGN) feedback which triggers, rather than suppresses, star formation. Recently, it was shown by Nayakshin et al. and Ishibashi et al. that star formation occurs when the cold interstellar medium (ISM) is squeezed by the impact of mass outflow or radiation pressure, respectively. Mass outflow is ubiquitous in this astrophysical context, and radiation pressure is also important if the AGN is luminous. For the first time in this subject, we incorporate both mass outflow feedback and radiative feedback into our model. Consequently, the ISM is shocked into shells by the AGN feedback, and these shells soon fragment into clumps and filaments because of Rayleigh-Taylor and thermal instabilities. We have two major findings: (1) the star formation rate can indeed be very large in the clumps and filaments. However, the resultant star formation rate density is too large compared with previous works, which is mainly because we ignore the fact that most of the stars that are formed would be disrupted when they move away from the galactic center. (2) Although radiation pressure feedback has a limited effect, when mass outflow feedback is also included, they reinforce each other. Specifically, in the gas-poor case, mass outflow is always the dominant contributor to feedback. 展开更多
关键词 methods: numerical - accretion - shock waves - galaxies: active - galaxies: starburst
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