Quantum Magnetic Collapse in Binary Systems

Quantum magnetic collapse is a possible phenomena that may occur in degenerate stars. If the pressure that is transverse to the magnetic field generated by the neutron star vanishes, it may lead to a collapse of the system. Such a collapse may result in a stellar remnant (such as a neutron star) that is elongated in the direction of the magnetic field or, for particular wavelengths, photons may be captured by strongly magnetized neutron stars.

In particular, we desire to build upon the work of Chaichian et, al (2000) by considering magnetic collapse in binary systems. The standard electroweak theory establishes that the upper limit of the magnetic field is M_w²/e = 10²⁴ G, which arises from the ground state of W± bosons. While the strength of the magnetic field may inhibit accretion efficiency, if the matter flux is sufficiently low, we can expect the accretion rate to not exceed Eddington efficiency. We then seek to determine how much the accreted matter contributes to the bosonic and leptonic chemical potential.