# (Self-)Magnetized Bose-Einstein Condensate stars

**Authors:** G. Quintero Angulo, A. P\'erez Mart\'inez, H. P\'erez Rojas, D., Manreza Paret

arXiv: 1812.07657 · 2019-09-04

## TL;DR

This paper investigates how magnetic fields influence the structure and equations of state of Bose-Einstein Condensate stars, revealing that magnetization affects their size, mass, and internal magnetic profiles.

## Contribution

It introduces a model for self-magnetized BEC stars using gamma-structure equations, considering independent particle-magnetic and particle-particle interactions, and compares magnetic and non-magnetic configurations.

## Key findings

- Magnetized BEC stars are generally smaller and less massive than non-magnetic ones.
- Self-magnetized BEC stars can have their internal magnetic fields computed as a function of their radii.
- Magnetic effects are more significant at low densities, affecting star stability and structure.

## Abstract

We study magnetic field effects on the Equations of State (EoS) and the structure of Bose-Einstein Condensate (BEC) stars, i.e. a compact object composed by a gas of interacting spin one bosons formed up by the pairing of two neutrons. To include the magnetic field in the thermodynamic description, we suppose that particle-magnetic field and particle-particle interactions are independent. We consider two configurations for the magnetic field: one where it constant and externally fixed, and another where it is produced by the bosons by self-magnetization. Since the magnetic field produces the splitting of pressures in the directions along and perpendicular to the magnetic axis, stable configurations of self-magnetized and magnetized BEC stars are studied using the recently found $\gamma$-structure equations that describe axially symmetric objects. The magnetized BEC stars are, in general spheroidal, less massive and smaller than the non-magnetic ones, being these effects more relevant at low densities. For the self-magnetized BEC stars their inner profiles of magnetic field can be computed as a function of the equatorial radii. The values obtained for the core and surface magnetic fields are in agreement with those typical of compact objects.

## Full text

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## Figures

26 figures with captions in the complete paper: https://tomesphere.com/paper/1812.07657/full.md

## References

41 references — full list in the complete paper: https://tomesphere.com/paper/1812.07657/full.md

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Source: https://tomesphere.com/paper/1812.07657