Quenched Superconductivity in Magnetars: Implications and Insights
Explore the world of magnetars and delve into the fascinating realm of quenched superconductivity, uncovering insights into their properties, field dynamics, and potential implications on various physical phenomena such as neutrino emissivity and heat capacity.
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Presentation Transcript
Quenched Superconductivity in Magnetars Monika Sinha Indian Institute of Technology Jodhpur Armen Sedrakian ITP, J. W. Goethe University, Frankfurt, Germany
Magnetara new class of neutron stars Bs = 1014 -1015 G Interior field even greater Superconductivity inside magnetar Quenched?
Motivation Type-II superconductivity London s penetration depth ? ? 1 ? = > 2 Coherence length Type-II superconductivity exists if 0 ??2 = Quantum of flux ??1< ? < ??2 2 ?2 0 = ? 2? From virial theorem ????> ??2 ????= 1018 G
Inputs ? ? = 16.14 MeV ?? = 32.20 MeV ?0 = 250.90 MeV ?0 = 0.152 fm-3
Results 0 0 ??2 = ??2 = 2 ?2 1 + ? 2 ?2 ?? ?= ???? ? ?2 ????? 27 2 8 ??2 ?2 ?2 ? = ??? max??2 6.25 1016 G
Implications Field decay Rotational dynamics Neutrino emissivity glitch cooling Reheating Heat capacity Electrical conductivity
Emissivity ??? Neutrino emissivity ??? ? ? + ? + ? ??? 2 (???+ ???)2 ??? ? =??? Direct Urca process ???2/3 2 Pair-breaking process
dUrca emissivity ( ?+ ?) ? ? ? > 0 ? < 0
Pair-breaking emissivity ?/?= =??/??/?(?)4??2 15 2?7?
Summary and outlook Neutrino emissivity is affected due to unpairing effect. Detailed cooling simulations are needed to confront the theory of magnetar with quenched superconductivity with the observations. Heat capacity, reheating due to field decay are to be addressed under this condition. Electrical conductivity, field decay, rotational dynamic, coupling of normal matter to superfluid matter should be revisited with this result. It is useful to address the problem of relating these observed surface fields to those in magnetar interiors as predicted by theoretical models. ?? ???? ??= ??3 ??? ?~??1; ??? ? ??????? ?? ????? relevant to our work ?~??2 We find roughly two orders of magnitude drop in the field value between the crust-core boundary and the surface of the star with ? 0.5?0 However, further work is needed to establish the relation in the strong field regime ?~??2.
