Number of the records: 1
Charged rho-meson condensation in neutron stars
SYS 0265934 LBL 02521^^^^^2200277^^^450 005 20240513091020.2 014 $a 000427447200017 $2 CCC 014 $a 000427447200017 $2 WOS CC. SCIE 014 $a 2-s2.0-85038227308 $2 SCOPUS 017 70
$a 10.1016/j.nuclphysa.2017.12.002 $2 DOI 035 $a biblio/93630 $2 CREPC2 100 $a 20181212d2018 m y slo 03 ba 101 0-
$a eng 102 $a NL 200 1-
$a Charged rho-meson condensation in neutron stars $f Evgeni E. Kolomeitsev, K. A. Maslov ... [et al.] 330 0-
$a We extend relativistic mean-field models with hadron masses and meson–baryon coupling constants dependent on the scalar field σ, including hyperons and (1232)baryons, to incorporate a possibility of the charged ρmeson condensation in neutron star matter. The influence of the ρ−condensation on the equation of state proves to be strongly model dependent. In our models of one type (KVORcut-based ones) the ρ−condensation arises by a second-order phase transition above a critical density and the maximum value of the neutron star mass diminishes only slightly. The matter composition changes more significantly. In our models of other type (MKVOR*-based ones), if the system is considered at fixed density, the ρ−condensation arises by a second-order phase transition at the baryon density n =n(II)c,ρand at a slightly higher density n =n(I)c,ρthere occurs a first-order phase transition. In a neutron star matter starting with a density n <n(II)c,ρthere appears a region of a mixed phase, or the system is described by Maxwell construction, that results in a substantial decrease of the value of the maximum neutron star mass. Nevertheless in the models under consideration the observational constraint on the maximum neutron star mass is fulfilled. Besides, in MKVOR*-based models the appearance of the ρ−condensate is accompanied by a strong rearrangement of the matter composition. Dependence of the results on a choice of the ρmeson scaling functions for the effective ρmeson mass and coupling constants is also investigated 463 -1
$1 001 umb_un_cat*0289345 $1 200 1 $a Nuclear Physics A $v Vol. 970, (2018), pp. 291-315 $1 210 $a Amsterdam $c Elsevier B.V. $d 2018 $1 011 $a 0375-9474 $1 011 $a 1873-1554 606 0-
$3 umb_un_auth*0221939 $a neutron stars 606 0-
$3 umb_un_auth*0247154 $a equation of state 606 0-
$3 umb_un_auth*0170471 $a condensation 615 $n 53 $a Fyzika 675 $a 53 700 -1
$3 umb_un_auth*0131258 $a Kolomeitsev $b Evgeni E. $p UMBFP06 $4 070 $9 34 $f 1970- $T Katedra fyziky 701 -1
$3 umb_un_auth*0244210 $a Maslov $b K. A. $9 33 $4 070 701 -1
$3 umb_un_auth*0160605 $a Voskresensky $b Dmitri $4 070 $9 33 801 $a SK $b BB301 $g AACR2 $9 unimarc sk 856 $u https://www.sciencedirect.com/science/article/pii/S0375947418300447 $a Link na plný text T85 $x existuji fulltexy
Number of the records: 1