  In this article, we present the effect of a strong magnetic field in the
burning of a neutron star (NS). We have used relativistic magneto-hydrostatic
(MHS) conservation equations for studying the PT from nuclear matter (NM) to
quark matter (QM). We found that the shock-induced phase transition (PT) is
likely if the density of the star core is more than three times nuclear
saturation ($\rho_s$) density. The conversion process from NS to quark star
(QS) is found to be an exothermic process beyond such densities. The burning
process at the star center most likely starts as a deflagration process.
However, there can be a small window at lower densities where the process can
be a detonation one. At small enough infalling matter velocities the resultant
magnetic field of the QS is lower than that of the NS. However, for a higher
value of infalling matter velocities, the magnetic field of QM becomes larger.
Therefore, depending on the initial density fluctuation and on whether the PT
is a violent one or not the QS could be more magnetic or less magnetic. The PT
also have a considerable effect on the tilt of the magnetic axis of the star.
For smaller velocities and densities the magnetic angle are not affected much
but for higher infalling velocities tilt of the magnetic axis changes suddenly.
The magnetic field strength and the change in the tilt axis can have a
significant effect on the observational aspect of the magnetars.
