Estimating magnetar radii with an empirical meta-model. (arXiv:1812.05879v1 [nucl-th])

Estimating magnetar radii with an empirical meta-model. (arXiv:1812.05879v1 [nucl-th])
<a href="http://arxiv.org/find/nucl-th/1/au:+Chatterjee_D/0/1/0/all/0/1">Debarati Chatterjee</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Gulminelli_F/0/1/0/all/0/1">Francesca Gulminelli</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Menezes_D/0/1/0/all/0/1">Debora P. Menezes</a>

The presence of strong magnetic fields in neutron stars, such as in
magnetars, may significantly affect their crust-core transition properties and
the crust size. This knowledge is crucial in the correct interpretation of
astrophysical phenomena involving magnetars, such as glitches in observed
rotation frequencies, cooling, bursts and possibly tidal polarizabilities. A
recently developed meta-modelling technique allows exploring the model
dependence of density functional theory equation of state calculations. In this
work, we extend this meta-model to investigate the effect of strong magnetic
fields on spinodal instabilities of neutron star matter and the associated
crust-core properties. Both Tolman-Oppenheimer-Volkov and a full
self-consistent numerical calculations are performed for the neutron star
structure, the results being quantitatively different for strong magnetic
fields.

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