2007/03/31 by Vyacheslav E. Zavlin · 1 citation
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysical Phenomena and Observations #Crab Nebula #Flux (metallurgy) #Nebula #Neutron star #Photon #Pulsar #Pulsars and Gravitational Waves Research #RADIUS #Thermal #Vela #astro-ph
paper · pdf · doi:10.1086/521300
Minor changes, including the reference to Esposito et al. (2007 A&A, 467, L45). Accepted by ApJ Letters
arxiv created 2007/07/06 · openalex publication_date 2007/08/02 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
The first short Chandra and XMM-Newton observations of the young and energetic pulsar J1357-6429 provided indications of a tail-like pulsar wind nebula associated with this object as well as pulsations of its X-ray flux with a pulsed fraction p f ≳ 50% and a thermal component dominating at energies E ≲ 2 keV. The putative nebula is very compact in size and might be interpreted as evidence for a pulsar jet. The thermal radiation is most plausibly emitted from the entire neutron star surface of a 10 km radius and a 1.0 ± 0.1 MK temperature, covered with a hydrogen atmosphere. At higher energies, the pulsar's emission is of a nonthermal origin, with a power-law spectrum of a photon index Γ = 1.1 ± 0.2. This makes the properties of PSR J1357-6429 very similar to those of the young pulsars J1119-6127 and Vela with detected thermal radiation.