Kicks of magnetized strange quark stars induced by anisotropic emission of neutrinos

Abstract

We study the anisotropic neutrino emission from the core of neutron stars induced by the star's magnetic field. We model the core as made out of a magnetized ideal gas of strange quark matter and implement the conditions for stellar equilibrium in this environment. The calculation is performed without resorting to analytical simplifications and for temperature, density and magnetic field values corresponding to typical conditions for a neutron star's evolution. The anisotropic neutrino emission produces a rocket effect that contributes to the star's kick velocity. We find that the computed values for the kick velocity lie within the range of the observed values, reaching velocities of the order of ∼ 1000 km s −1 for magnetic fields between 10 15 − 10 18 G and radii of 20 to 5 km, respectively.

Neutron star kick velocity induced by neutrino chirality flip and a lower bound for the neutrino magnetic moment

“…We show that this requirement places a lower bound for the magnitude of the neutrino magnetic moment which is larger than the corresponding value as predicted by the Standard Model (SM). We show that this result, combined with the most stringent upper bound for the neutrino magnetic moment (Ayala et al 1999;Ayala et al 2000) opens a window of plausible values for the process.…”

“…The main contribution to the kick velocities comes from the neutrino emission at higher temperatures (between 50 and 30 MeV) and larger chemical potentials (∼300 MeV), at the beginning of the NS evolution (around 15 s after the core collapse and ends approximately 35 s later; Lattimer & Prakash 2004). We thus study the chirality flip process within the core of the NS assuming these conditions which are consistent with those assumed to place the upper bound on the neutrino magnetic moment from the chirality flip in supernovae (Ayala et al 1999;Ayala et al 2000).…”

Thermal corrections to the gluon magnetic Debye mass

“…After straightforward algebra, we realize that Eqs. (C. 19) and (C.20) are equal to Eqs. (C.9) and (C.10), respectively.…”

“…Possible signatures of the presence of such fields in the interaction region can be the chiral magnetic effect [14] or the enhanced production of prompt photons [15][16][17][18]. Moreover, magnetic fields can have an impact on the properties of compact astrophysical objects, such as neutron stars [19].…”

Pion mass modification in a weak magnetic field

“…Strong magnetic fields are present in a wide variety of physical system, from heavy‐ion collisions (Kharzeev et al ; McLerran & Skokov ), the interior of compact astrophysical objects (Ayala et al ; Duncan & Thompson ; Esposito et al ), and the early universe (Navarro et al ; Sanchez et al ). In Earth‐based experiments, particularly in peripheral heavy‐ion collisions, at relativistic heavy ion collider and at the large hadron collider, we can find huge magnetic fields, which have been estimated to be of the order of a few times the pion mass squared G (Skokov et al ).…”