The maximum and minimum mass of protoneutron stars in the Brueckner theory

Abstract

We study the structure of protoneutron stars within the finite-temperature Brueckner-Bethe-Goldstone theoretical approach, paying particular attention to how it is joined to a low-density nuclear equation of state. We find a slight sensitivity of the minimum value of the protoneutron star mass to the low-density equation of state, whereas the maximum mass is hardly affected.

Hyperon-hyperon interactions with the Nijmegen ESC08 model

“…Like in [1], also this paper uses the non-relativistic BBG expansion, and studies the possible appearance of hyperons in NS matter within the BHF theoretical many-body approach, continuing several earlier publications [17][18][19][20][21][22][23][24][25]. The fundamental input of these parameterfree calculations are realistic potentials in the nucleonnucleon (NN), NY, and YY sectors, supplemented by three-body forces (TBF), which at least in the NN case are required in order to ensure a correct saturation point of nuclear matter.…”

Evolution of a proto-neutron star with a nuclear many-body equation of state: Neutrino luminosity and gravitational wave frequencies

“…Following [26], we assume that finite-temperature effects do not modify the functional dependency of f I B on the proton fraction, i.e.,…”

“…(10). In the literature, there is no generally accepted fitting formula for these functions [19,[26][27][28][29]. In order to perform our evolutionary numerical simulations, we need a fitting formula which is accurate in a wide density range, extending from n B ≲ 0.5 fm −3 to n B ≳ 0.001 fm −3 relevant for the core and the crust of the star, respectively.…”

“…In order to perform our evolutionary numerical simulations, we need a fitting formula which is accurate in a wide density range, extending from n B ≲ 0.5 fm −3 to n B ≳ 0.001 fm −3 relevant for the core and the crust of the star, respectively. Therefore, we cannot use the fitting formula of [26], which is only accurate for large densities. Moreover, we need a free energy with continuous secondorder derivatives.…”

Structure of the hadron-quark mixed phase in protoneutron stars

“…In the low-density range, where nucleonic clustering sets in, we cannot use the BHF approach, and therefore we join (Burgio & Schulze 2010) the BHF EOS to the finite-temperature or -entropy EOS of Shen et al (1998a,b), which is more appropriate at densities below n B < ∼ 0.07 fm −3 , since it does include the treatment of finite nuclei.…”