Abstract
Interpretation of Quiescent Behavior of Iron K-Alpha (Fe Kand945) Emission Line from Sigma Gem
Highlights
Iron K-alpha (Fe K ) emission lines result when an electron transits to the innermost “K” shell from a 2p orbital of the second or “L” shell of atom releasing 6.4 keV of energy as florescence emission line photon [1]
Some high energy astrophysics software was used in analyzing data in this research, these are XSELECT, XSPEC
For the bremsstrahlung fit parameter in the flare period it shows that the continuum temperature (KT) is 54±0.28,the power law photon index was not found while the photon count (F count) is 0.8±0.01
Summary
Iron K-alpha (Fe K ) emission lines result when an electron transits to the innermost “K” shell (principal quantum number 1) from a 2p orbital of the second or “L” shell (with principal quantum number 2) of atom releasing 6.4 keV of energy as florescence emission line photon [1]. The thermal origin of the X-ray emission from galaxy clusters was resolved with the detection of the 6.7 keV iron line in their X-ray Spectra [2]. An example of K-alpha lines is those seen for iron as iron atoms radiating X-rays spirall into a black hole at the center of a galaxy. For such purpose the energy, E of the line is adequately calculated to 2-digit accuracy by the use of Moseley’s law:. From the analysis of the K emission spectra, basic physical properties within the emitting region can be deduced, such as temperatures, densities, excitation conditions, ionization balance, elemental abundances and electric - and magnetic field distributions [7,8]
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