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81.
Doing space Astronomy on lunar surface has several advantages. We present here feasibility of an All Sky Monitoring Payload for Spectro-photometry
in X-rays (SPHINX) which can be placed on a lander on the moon or in a space craft orbiting around the moon. The Si–PIN photo-diodes
and CdTe crystals are used to detect solar flares, bright gamma bursts, soft gamma-ray repeaters from space and also X-ray
fluorescence (XRF) from lunar surface. We present the complete Geant4 simulation to study the feasibility of such an instrument
in presence of Cosmic Diffused X-Ray Background (CDXRB). We find that the signal to noise ratio is sufficient for moderate
to bright GRBs (above 5 keV), for the quiet sun (up to 100 keV), solar flares, soft gamma-ray repeaters, X-ray Fluorescence
(XRF) of lunar surface etc. This is a low-cost system which is capable of performing multiple tasks while stationed at the
natural satellite of our planet. 相似文献
82.
We self-consistently obtain shock locations in an accretion flow by using an analytical method. One can obtain the spectral
properties, quasi-periodic oscillation frequencies and the outflow rates when the inflow parameters are known. Since temperature
of the CENBOL decides the spectral states of the black hole, and also the outflow rate, the outflow rate is directly related
to the spectral states. 相似文献
83.
Indranil Chattopadhyay Sandip K. Chakrabarti 《Journal of Astrophysics and Astronomy》2002,23(1-2):149-153
Matter accreting onto black holes suffers a standing or oscillating shock wave in much of the parameter space. The post-shock
region is hot, puffed up and reprocesses soft photons from a Keplerian disc to produce the characteristic hard tail of the
spectrum of accretion discs. The post-shock torus is also the base of the bipolar jets. We study the interaction of these
jets with the hard photons emitted from the disc. We show that radiative force can accelerate outflows but the drag can limit
the terminal speed. We introduce an equilibrium speed υeq as a function of distance, above which the flow will experience radiative deceleration. 相似文献
84.
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87.
Santanu Mondal Sandip K. Chakrabarti Dipak Debnath 《Astrophysics and Space Science》2014,353(1):223-231
Accretion flows having positive specific energy are known to produce outflows and winds which escape to a large distance. According to Two Component Advective Flow (TCAF) model, centrifugal pressure dominated region of the flow just outside the black hole horizon, with or without shocks, acts as the base of this outflow. Electrons from this region are depleted due to the wind and consequently, energy transfer rate due to inverse Comptonization of low energy photons are affected. Specifically, it becomes easier to cool this region and emerging spectrum is softened. Our main goal is to show spectral softening due to mass outflow in presence of Compton cooling. To achieve this, we modify Rankine-Hugoniot relationships at the shock front when post-shock region suffers mass loss due to winds and energy loss due to inverse Comptonization. We solve two-temperature equations governing an accretion flow around a black hole which include Coulomb exchange between protons and electrons and other major radiative processes such as bremsstrahlung and thermal Comptonization. We then compute emitted spectrum from this post-shock flow. We also show how location of standing shock which forms outer boundary of centrifugal barrier changes with cooling. With an increase in disc accretion rate \((\dot{m}_{d})\) , cooling is enhanced and we find that the shock moves in towards the black hole. With cooling, thermal pressure is reduced, and as a result, outflow rate is decreased. We thus directly correlate outflow rate with spectral state of the disc. 相似文献
88.
89.
The central depths of the interstellar 4430 Å band and far UV extinction for a sample of reddened LMC members are presented here. 相似文献
90.