Numerical simulation of the electron capture process in a magnetar interior

Abstract

In a superhigh magnetic field, direct Urca reactions can proceed for an arbitrary proton concentration. Since only the electrons with high energy E (E > Q, Q is the threshold energy of inverse β-decay) at large Landau levels can be captured, we introduce the Landau level effect coefficient q and the effective electron capture rate eff . By using eff , the values of L X and L ν are calculated, where L X and L ν are the average neutrino luminosity of AXPs and the average X-ray luminosity of AXPs L X , respectively. The complete process of electron capture inside a magnetar is simulated numerically.

General relativistic calculations for white dwarfs

“…It has been speculated that the presence of a magnetic field drastically modifies the situation in a compact star due to the Landau quantization of the electronic energy levels. Gao et al (2011) simulated the electron β-capture in a magnetar by considering electrons belonging to the higher Landau levels in a super high magnetic field that admit the energy threshold values for inverse β-decay to occur. For a 4 2 He white dwarf star, Das & Mukhopadhyay (2012) considered the modified equation of state due to the Landau levels of the electrons in a magnetic field.…”

The Landau level-superfluid modified factor and the overal soft X/γ-ray efficiency coefficient of a magnetar

“…Though magnetic fields of such magnitude inside magnetars are unauthentic, and are not consistent with our model (B ∼ 10 14−15 G), their calculations are useful in supporting our following presumptions: when B ∼ 10 14−15 G, the value of Y p may be enhanced, and could be higher than the mean value of Y p inside a common NS (∼0.05); direct Urca processes are expected to occur in a magnetar interior. Based on these presumptions, we also obtain a concise expression for E F (e), E F (e) 43.44( B B cr ) 1 4 ( ρ ρ 0 Y p 0.12 ) 1 4 MeV by solving (1) of this paper (cited from Gao et al 2011c).…”

Supernova antineutrino energy losses of 59Co, 56Co, 56Ni, and 56Fe by β−‐decay in strongly screened plasma

“…In the process of beta decay, either a positron and a neutrino are released, or an electron and an antineutrino are released. As we know, neutrinos carry away more than 99% of the energy released by the weak reaction in the core of the presupernova (e.g., Gao et al , , ). We have also discussed the weak interaction and related issues (e.g., Liu ;Liu ;Liu ;2014d;Liu ;Liu et al , ;Liu et al , ;Liu & Liu ).…”