Magnetic Fields of Spherical Compact Stars in Braneworld

TL;DR

This paper investigates how brane tension in a braneworld scenario affects the magnetic fields of spherical compact stars, providing solutions that suggest observable modifications in pulsar and magnetar emissions.

Contribution

It presents new solutions for magnetic fields in braneworld models, highlighting the impact of brane tension on magnetic field strength and electromagnetic energy loss in compact stars.

Findings

Brane tension enhances magnetic field strength inside and outside the star.

Modifications could lead to observable differences in pulsar and magnetar emissions.

Electromagnetic energy loss can be amplified by up to several orders depending on brane tension.

Abstract

We study the dipolar magnetic field configuration in dependence on brane tension and present solutions of Maxwell equations in the internal and external background spacetime of a magnetized spherical star in a Randall-Sundrum II type braneworld. The star is modelled as sphere consisting of perfect highly magnetized fluid with infinite conductivity and frozen-in dipolar magnetic field. With respect to solutions for magnetic fields found in the Schwarzschild spacetime brane tension introduces enhancing corrections both to the interior and the exterior magnetic field. These corrections could be relevant for the magnetic fields of magnetized compact objects as pulsars and magnetars and may provide the observational evidence for the brane tension through the modification of formula for magneto-dipolar emission which gives amplification of electromagnetic energy loss up to few orders depending on the value of the brane tension.