期刊
JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
卷 -, 期 2, 页码 -出版社
IOP Publishing Ltd
DOI: 10.1088/1475-7516/2022/02/027
关键词
neutron stars; magnetic fields; pulsar magnetosphere
资金
- NSF [PHY-1827573, PHY-1912769, PHY-2011383]
- CONACyT [140630, 376127]
- NSERC
- NSERC through CIFAR
- UNAM-PAPIIT grant [IA100721]
- Perimeter Institute for Theoretical Physics
- Government of Canada through the Department of Innovation, Science and Economic Development Canada
- Province of Ontario through the Ministry of Research, Innovation and Science
- Canada Foundation for Innovation
- Government of Ontario
- Ontario Research Fund Research Excellence
- University of Toronto
The study focused on analyzing sky maps and light curves of gamma-ray emission from neutron stars in compact binaries and in isolation, exploring various magnetic field structures' impact on gamma-ray emission, and proposing a simple approximation for rapid exploration of binary magnetic field structures.
We study sky maps and light curves of gamma-ray emission from neutron stars in compact binaries, and in isolation. We briefly review some gamma-ray emission models, and reproduce sky maps from a standard isolated pulsar in the Separatrix Layer model. We consider isolated pulsars with several variations of a dipole magnetic field, including superpositions, and predict their gamma-ray emission. Our results provide new heuristics on what can and cannot be inferred about the magnetic field configuration of pulsars from high-energy observations. We find that typical double-peak light curves can be produced by pulsars with significant multipole structure beyond a single dipole. For binary systems, we also present a simple approximation that is useful for rapid explorations of binary magnetic field structure. Finally, we predict the gamma-ray emission pattern from a compact black hole-neutron star binary moments before merger by applying the Separatrix Layer model to data simulated in full general relativity; we find that face-on observers receive little emission, equatorial observers see one broad peak, and more generic observers typically see two peaks.
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