Nuclear, Particle, Astroparticle and Cosmology (NUPAC) Seminars
Topics in the Physics of Supernovae and Neutron Stars
Presented by Sajad Abbar, UNM
A star with a mass larger than 8 ? 10 solar masses can end its life in a supernova explosion and possibly form a neutron star. In this talk, I will present the results of a research I did for my dissertation in which I studied two important aspects of the physics of supernovae and neutron stars, namely "neutrino flavor oscillations in supernovae" and "the thermal conductivity of the neutron star crust".
Neutrino flavor oscillations in the presence of ambient neutrinos is nonlinear in nature which leads to interesting phenomenology that has not been well understood. This phenomenon in the supernova context has been studied in the so-called neutrino bulb model which is a restricted, stationary and spherically symmetric supernova model. In my talk, I will show that both of the spatial and time symmetries can be broken spontaneously in a dense neutrino gas. Our results suggest that neutrino flavor oscillations in a dense neutrino gas can vary rapidly in space and time.
A star with a mass larger than 8 − 10 solar masses can end its lif=
e in a supernova explosion and possibly form a neutron star. In this talk, =
I will present the results of a research I did for my dissertation in which=
I studied two important aspects of the
physics of supernovae and neutron stars, namely "neutrino flavor osci=
llations in supernovae" and "the thermal conductivity of the neut=
ron star crust".
Neutrino flavor oscillations in the presence of ambient neutrinos is nonlin=
ear in nature which leads to interesting phenomenology that has not been we=
ll understood. This phenomenon in the supernova context has been studied in=
the so-called neutrino bulb model
which is a restricted, stationary and spherically symmetric supernova mode=
l. In my talk, I will show that both of the spatial and time symmetries can=
be broken spontaneously in a dense neutrino gas. Our results suggest that =
neutrino flavor oscillations in
a dense neutrino gas can vary rapidly in space and time.
Neutron star crust plays a very important role in its thermal evolution. In=
the second part of my talk, I will discuss briefly the quantum effects in =
the thermal conductivity of the neutron star crust. By comparing the result=
s obtained from the classical and
quantum Monte Carlo simulations and those obtained form a semi-analytical =
calculation based on the one-phonon approximation, I show that the quantum =
effects become important at temperature T < 0.3 ΩP, where ΩP i=
s the ion plasma frequency.
2:00 pm, Tuesday, April 5, 2016
PAIS-2540, PAIS
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