Exploring the origin of slow-rotating pulsars: Emission from STARS simulated white dwarfs
Abstract
An increasing number of slow-rotating pulsars and long-period transients have been observed in recent years. The periods of these sources can be significantly longer than typical pulsar sources, ranging from ~ 100 - 1000 s, or even longer. The observed periods and period derivatives predict high magnetic fields, higher than the Schwinger field, when we consider conventional pulsar models of dipole-driven emission from neutron stars. Interestingly, the periods of these sources are consistent with the current observations of white dwarfs (WDs). We explore the possibility of magnetic WDs, simulated using the stellar evolution code STARS, as the origin of some of these unusual pulsar observations. We simulate WDs with enhanced magnetic fields due to accretion after their formation. We also briefly touch on the more exotic possibility of super-Chandrasekhar WDs as the origin for these sources. We find that expanding the parameter space to include the possibility of a WD origin provides an alternate and viable explanation for these unusual observations.
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BibTeX
@misc{zuraiq2026exploring,
title = {{Exploring the origin of slow-rotating pulsars: Emission from STARS simulated white dwarfs}},
author = {Zenia Zuraiq and Banibrata Mukhopadhyay},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.28728},
eprint = {2610.28728},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.28728},
}
RIS
TY - UNPB
TI - Exploring the origin of slow-rotating pulsars: Emission from STARS simulated white dwarfs
AU - Zenia Zuraiq
AU - Banibrata Mukhopadhyay
PY - 2026
DA - 2026/10/20
PB - arXiv
DO - 10.48550/arxiv.2610.28728
UR - https://arxiv.org/abs/2610.28728
AB - An increasing number of slow-rotating pulsars and long-period transients have been observed in recent years. The periods of these sources can be significantly longer than typical pulsar sources, ranging from ~ 100 - 1000 s, or even longer. The observed periods and period derivatives predict high magnetic fields, higher than the Schwinger field, when we consider conventional pulsar models of dipole-driven emission from neutron stars. Interestingly, the periods of these sources are consistent with the current observations of white dwarfs (WDs). We explore the possibility of magnetic WDs, simulated using the stellar evolution code STARS, as the origin of some of these unusual pulsar observations. We simulate WDs with enhanced magnetic fields due to accretion after their formation. We also briefly touch on the more exotic possibility of super-Chandrasekhar WDs as the origin for these sources. We find that expanding the parameter space to include the possibility of a WD origin provides an alternate and viable explanation for these unusual observations.
ER -