The Galactic population and properties of young, highly-energetic pulsars
| dc.contributor.author | JOHNSTON, Simon | |
| hal.structure.identifier | Centre d'Etudes Nucléaires de Bordeaux Gradignan [CENBG] | |
| dc.contributor.author | SMITH, D.A. | |
| dc.contributor.author | KARASTERGIOU, A. | |
| dc.contributor.author | KRAMER, M. | |
| dc.date.issued | 2020 | |
| dc.identifier.issn | 0035-8711 | |
| dc.description.abstractEn | The population of young, non-recycled pulsars with spin-down energies |$\dot{E} \gt 10^{35}$| erg s^−1 is sampled predominantly at γ-ray and radio wavelengths. A total of 137 such pulsars are known, with partial overlap between the sources detectable in radio and γ-rays. We use a very small set of assumptions in an attempt to test whether the observed pulsar sample can be explained by a single underlying population of neutron stars. For radio emission we assume a canonical conal beam with a fixed emission height of 300 km across all spin periods and a luminosity law which depends on |$\dot{E}^{0.25}$|. For γ-ray emission we assume the outer-gap model and a luminosity law which depends on |$\dot{E}^{0.5}$|. We synthesize a population of fast-spinning pulsars with a birth rate of one per 100 yr. We find that this simple model can reproduce most characteristics of the observed population with two caveats. The first is a deficit of γ-ray pulsars at the highest |$\dot{E}$| which we surmise to be an observational selection effect due to the difficulties of finding γ-ray pulsars in the presence of glitches without prior knowledge from radio frequencies. The second is a deficit of radio pulsars with interpulse emission, which may be related to radio emission physics. We discuss the implications of these findings. | |
| dc.language.iso | en | |
| dc.publisher | Oxford University Press (OUP): Policy P - Oxford Open Option A | |
| dc.subject.en | pulsars: general | |
| dc.title.en | The Galactic population and properties of young, highly-energetic pulsars | |
| dc.type | Article de revue | |
| dc.identifier.doi | 10.1093/mnras/staa2110 | |
| dc.subject.hal | Physique [physics]/Astrophysique [astro-ph] | |
| dc.identifier.arxiv | 2007.08681 | |
| bordeaux.journal | Monthly Notices of the Royal Astronomical Society | |
| bordeaux.page | 1957-1965 | |
| bordeaux.volume | 497 | |
| bordeaux.issue | 2 | |
| bordeaux.peerReviewed | oui | |
| hal.identifier | hal-02927699 | |
| hal.version | 1 | |
| hal.popular | non | |
| hal.audience | Internationale | |
| hal.origin.link | https://hal.archives-ouvertes.fr//hal-02927699v1 | |
| bordeaux.COinS | ctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.jtitle=Monthly%20Notices%20of%20the%20Royal%20Astronomical%20Society&rft.date=2020&rft.volume=497&rft.issue=2&rft.spage=1957-1965&rft.epage=1957-1965&rft.eissn=0035-8711&rft.issn=0035-8711&rft.au=JOHNSTON,%20Simon&SMITH,%20D.A.&KARASTERGIOU,%20A.&KRAMER,%20M.&rft.genre=article |
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