Constraining pulsar birth properties with supernova X-ray observations
| Autor: | Elena Amato, Niccolò Bucciantini, Y. A. Gallant, Rino Bandiera |
|---|---|
| Přispěvatelé: | Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), ITA, FRA |
| Jazyk: | angličtina |
| Rok vydání: | 2017 |
| Předmět: |
supernovae
Astrophysics::High Energy Astrophysical Phenomena Astrophysics Magnetar 01 natural sciences Pulsar wind nebula Binary pulsar neutron stars Luminosity Pulsar 0103 physical sciences X-rays Astrophysics::Solar and Stellar Astrophysics 010303 astronomy & astrophysics Astrophysics::Galaxy Astrophysics ComputingMilieux_MISCELLANEOUS acceleration of particles Physics 010308 nuclear & particles physics [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE] Astronomy Astronomy and Astrophysics Galaxy Supernova Neutron star Space and Planetary Science pulsars |
| Zdroj: | IAU Symposium 331 : SN 1987A, 30 Years Later IAU Symposium 331 : SN 1987A, 30 Years Later, Feb 2017, Saint-Gilles-les-Bains, La Réunion, France. pp.63-68, ⟨10.1017/S1743921317004756⟩ |
| DOI: | 10.1017/S1743921317004756⟩ |
| Popis: | A large fraction of core-collapse supernovae are thought to result in the birth of a rotation-powered pulsar, which is later observable as a radio pulsar up to great ages. The birth properties of these pulsars, and in particular the distribution of their initial rotation periods, are however difficult to infer from studies of the radio pulsar population in our Galaxy. Yet the distributions of their birth properties is an important assumption for scenarios in which ultra-high-energy cosmic rays (UHECRs) originate in very young, extragalactic pulsars with short birth periods and/or high magnetic fields.Using a model of the very young pulsar wind nebula’s dynamical and spectral evolution, with pulsar wind and accelerated particle parameters assumed similar to those inferred from modeling young pulsar wind nebulae (PWNe) in our Galaxy, we show that X-ray observations of supernovae, a few years to decades after the explosion, constitute a favored window to obtain meaningful constraints on the initial spin-down luminosity of the newly-formed pulsar. We examine the expected emerging PWN spectral component, taking into account the X-ray opacity of the expanding supernova ejecta, and find that it is typically best detectable in < 10 keV X-rays some years after the explosion. We use this framework to assess available X-ray observations and flux upper limits on supernovae, building on the work of Pernaet al.(2008). We note that a resulting limit on spin-down luminosity corresponds univocally to a limit on the maximum magnetospheric acceleration potential, irrespective of the specific combination of magnetic field and rotation period that achieves it. We use available X-ray observations of supernovae to place constraints on the birth spin-down luminosity and period distribution of classical pulsars. We also examine the case of magnetars, born with much higher magnetic fields, and show that their much shorter initial spin-down time implies that any plausible signature of young magnetar wind nebulae can only be observed in harder X-ray or gamma-rays. |
| Databáze: | OpenAIRE |
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