{"paper":{"title":"The X-ray Spectrum of the Vela Pulsar Resolved with Chandra","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"D. Sanwal (PSU), G. Garmire (PSU), G.G. Pavlov (PSU), V. Burwitz (MPE), V.E Zavlin (MPE)","submitted_at":"2001-03-12T16:59:25Z","abstract_excerpt":"We report the results of the spectral analysis of two observations of the Vela pulsar with the Chandra X-ray observatory. The spectrum of the pulsar does not show statistically significant spectral lines in the observed 0.25-8.0 keV band. Similar to middle-aged pulsars with detected thermal emission, the spectrum consists of two distinct components. The softer component can be modeled as a magnetic hydrogen atmosphere spectrum - for the pulsar magnetic field $B=3\\times 10^{12}$ G and neutron star mass $M=1.4 M_\\odot$ and radius $R^\\infty =13$ km, we obtain $\\tef^\\infty =0.68\\pm 0.03$ MK, $L_{\\"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0103171","kind":"arxiv","version":1},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}