Abstract
Galactic magnetic field (GMF) and secondary cosmic rays (CRs) (e.g. 10beryllium, boron, antiproton) are important components to understand the propagation of CRs in the Milky Way Galaxy. Realistic modeling of GMF is based on the Faraday rotation measurements of various Galactic and extragalactic radio sources and synchrotron emission from CR leptons in the radio frequency range, thereby providing information of halo height. On the other hand, diffusion coefficient and halo height are also estimated from the 10Be/9Be and B/C ratios. Moreover, density distribution of gaseous components of interstellar medium (ISM) also plays an important role as secondary CRs are produced due to interaction of primary CRs with the gaseous components of ISM . We consider mainly molecular, atomic, and ionized components of hydrogen gas for our study. Recent observations and hydrodynamical simulations provide new forms of density profiles of hydrogen gas in Milky Way Galaxy. In the DRAGON code, we have implemented our chosen density profiles, based on realistic observations in radio, X-ray and γ-ray wavebands, and hydrodynamical simulations of interstellar hydrogen gas to study the variation in the height of the halo required to fit the observed CR spectra. Our results show the halo height (zt) varies in the range of 2 to 6 kpc for the density profiles considered in our work.
Highlights
The study of the origin of Galactic cosmic rays (CRs) is one of the most enigmatic areas of research at present
Our prime motive is to study the effects of variations in the density profiles of molecular, atomic and ionized hydrogen gas in the Milky Way Galaxy on its height of the halo
For this purpose we considered the model of Galactic magnetic field (GMF) consistent with the Faraday rotation measurements and synchrotron emissions
Summary
The study of the origin of Galactic cosmic rays (CRs) is one of the most enigmatic areas of research at present. Ginzburg and Syrovatskii [1] was the first who had introduced various terms, used to study propagation of CRs, to include possible gain and losses in the flux of CRs. Previously, leaky box model and its variants were widely used to study the observed GeV flux ratio of secondary to primary [2, 3]. Along with energy dependence, the spatial dependence of diffusion coefficient and more realistic structures of the Galactic magnetic field (GMF) have been taken into account to solve the transport equation of CRs [8–13]. Despite such advancements, several important questions on CR propagation remain open
Sign-in/Register to view highlights & summary Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
