The hydrodynamics of shock waves has found numerous applications in the field
of fluid dynamics, astrophysics, high-energy physics, and cosmology. A shock
wave is a wave where the disturbance in the medium propagates faster than the
local speed of sound. On either side of the interference, the thermodynamic
variables vary discontinuously. It occurs when there is a rapid compression or
expansion of the system. The mass, momentum, and energy conservation laws
across the surface lead to the Rankine–Hugoniot (RH) and Taub equation
connecting the properties of the fluid on either side of the discontinuity.
In the talk I will discuss the implication of sock wave in phase transition in
neutron stars and magnetars. At the center of the neutron star, where density
is very high, the transition from nuclear matter to quark matter can happen.
First, the kinematic approach has been employed for studying phase transition
in neutron stars and magnetars. A new maximum mass limit for the hybrid star
(a star with a quark core surrounded by nuclear matter) formed after the shock-
induced phase transition in a neutron star has been found. We will also be
discussing the dynamic phase transition process as a two-step process: first, the
nuclear matter gets deconfined (strong interaction) into up and down quarks (2-
flavor matter), and then further decays into strange quarks (weak decay),
forming 3-favour matter (up, down, and strange). We found that gravitational
wave amplitude due to the phase transition is well within the present detector’s
capability; however, the frequency is on the higher side. We also have examined
other multiple signals from the phase transition, namely, the radio and neutrino
emissions.
We will also discuss the crucial findings of the work and their importance in the
present scenario in the future.