TY  - JOUR
A1  - Dexheimer, Verônica Antocheviz
A1  - Franzon, Bruno
A1  - Gomes, Renata de Oliveira
A1  - Farias, Ricardo L. S.
A1  - Avancini, Sidney dos Santos
A1  - Schramm, Stefan
T1  - What is the magnetic field distribution for the equation of state of magnetized neutron stars?
T2  - Physics Letters B
N2  - In this Letter, we report a realistic calculation of the magnetic field profile for the equation of state inside strongly magnetized neutron stars. Unlike previous estimates, which are widely used in the literature, we find that magnetic fields increase relatively slowly with increasing baryon chemical potential (or baryon density) of magnetized matter. More precisely, the increase is polynomial instead of exponential, as previously assumed. Through the analysis of several different realistic models for the microscopic description of stellar matter (including hadronic, hybrid and quark models) combined with general relativistic solutions endowed with a poloidal magnetic field obtained by solving Einstein–Maxwell's field equations in a self-consistent way, we generate a phenomenological fit for the magnetic field distribution in the stellar polar direction to be used as input in microscopic calculations.
KW  - Neutron star
KW  - Equation of state
KW  - Quark deconfinement
KW  - Magnetic field
Y1  - 2017
UR  - http://publikationen.ub.uni-frankfurt.de/frontdoor/index/index/docId/54627
UR  - https://nbn-resolving.org/urn:nbn:de:hebis:30:3-546270
SN  - 1873-2445
SN  - 0370-2693
VL  - 773.2017
SP  - 487
EP  - 491
PB  - Elsevier
CY  - Amsterdam
ER  -