| SYS | | 0265937 |
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| LBL | | 01227^^^^^2200241^^^450 |
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| 005 | | 20240513085528.5 |
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| 014 | | $a 000427543900010 $2 WOS CC. SCIE |
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| 014 | | $a 2-s2.0-85054824735 $2 SCOPUS |
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| 014 | | $a 2-s2.0-85054835220 $2 SCOPUS |
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| 017 | 70 | $a 10.1016/j.nuclphysa.2018.10.014 $2 DOI |
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| 035 | | $a biblio/93811 $2 CREPC2 |
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| 100 | | $a 20181212d2018 m y slo 03 ba |
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| 101 | 0- | $a eng |
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| 102 | | $a CH |
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| 200 | 1- | $a On cooling of neutron stars with a stiff equation of state including hyperons $f Hovik Grigorian, Evgeni E. Kolomeitsev ... [et al.] |
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| 330 | 0- | $a Exploiting a stiff equation of state of the relativistic mean-field model MKVORHf with sigma-scaled hadron effective masses and couplings, including hyperons, we demonstrate that the existing neutron-star cooling data can be appropriately described within “the nuclear medium cooling scenario” under the assumption that different sources have different masses |
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| 463 | -1 | $1 001 umb_un_cat*0289894 $1 011 $a 2218-1997 $1 200 1 $a Universe $v Vol. 4, no. 2 (2018), pp. 1-6 $1 210 $a Basel $c Multidisciplinary Digital Publishing Institute $d 2018 |
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| 606 | 0- | $3 umb_un_auth*0247154 $a equation of state |
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| 606 | 0- | $3 umb_un_auth*0221939 $a neutron stars |
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| 606 | 0- | $3 umb_un_auth*0298406 $a neutrína $X neutrinos |
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| 615 | | $n 53 $a Fyzika |
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| 675 | | $a 53 |
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| 700 | -1 | $3 umb_un_auth*0272897 $a Grigorian $b Hovik $4 070 $9 25 |
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| 701 | -1 | $3 umb_un_auth*0131258 $a Kolomeitsev $b Evgeni E. $p UMBFP06 $4 070 $9 25 $f 1970- $T Katedra fyziky |
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| 701 | -1 | $3 umb_un_auth*0258764 $a Maslov $b Konstantin A. $9 25 $4 070 |
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| 701 | -1 | $3 umb_un_auth*0160605 $a Voskresensky $b Dmitri $4 070 $9 25 |
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| 801 | | $a SK $b BB301 $g AACR2 $9 unimarc sk |
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| 856 | | $u https://www.mdpi.com/2218-1997/4/2/29 $a Link na zdrojový dokument |
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| T85 | | $x existuji fulltexy |
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