JOHNSTON, Simon; SMITH, D.A.; KARASTERGIOU, A.; KRAMER, M.

doi:10.1093/mnras/staa2110

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JOHNSTON, Simon

SMITH, D.A.
Centre d'Etudes Nucléaires de Bordeaux Gradignan [CENBG]

KARASTERGIOU, A.

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Monthly Notices of the Royal Astronomical Society. 2020, vol. 497, n° 2, p. 1957-1965

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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.< Réduire

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pulsars: general

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The Galactic population and properties of young, highly-energetic pulsars

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