Galactic magnetic field ( GMF ) and secondary cosmic rays ( CRs ) ( e.g . ^ { 10 } beryllium , 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 ^ { 10 } Be/ ^ { 9 } Be 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 \gamma -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 ( z _ { t } ) varies in the range of 2 to 6 kpc for the density profiles considered in our work .