Formation, Possible Detection and Consequences of Highly Magnetized Compact Stars by Banibrata Mukhopadhyay et al. on Wednesday 23 November

Over the past several years, there has been enormous interest in massive

neutron stars and white dwarfs due to either their direct or indirect evidence.

The recent detection of gravitational wave event GW190814 has confirmed the

existence of compact stars with masses as high as $\sim2.5-2.67M_{\odot}$

within the so-called mass gap, indicating the existence of highly massive

neutron stars. One of the primary goals to invoke massive compact objects was

to explain the recent detections of over a dozen Type Ia supernovae, whose

peculiarity lies with their unusual light curve, in particular the high

luminosity and low ejecta velocity. In a series of recent papers, our group has

proposed that highly magnetised white dwarfs with super-Chandrasekhar masses

can be promising candidates for the progenitors of these peculiar supernovae.

The mass-radius relations of these magnetised stars are significantly different

from those of their non-magnetised counterparts, which leads to a revised

super-Chandrasekhar mass-limit. These compact stars have wider ranging

implications, including those for soft gamma-ray repeaters, anomalous X-ray

pulsars, white dwarf pulsars and gravitational radiation. Here we review the

development of the subject over the last decade or so, describing the overall

state of the art of the subject as it stands now. We mainly touch upon the

possible formation channels of these intriguing stars as well as the

effectiveness of direct detection methods. These magnetised stars can have many

interesting consequences, including reconsideration of them as possible

standard candles.

arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.11998v1