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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_{\\"},"verification_status":{"content_addressed":true,"pith_receipt":true,"author_attested":false,"weak_author_claims":0,"strong_author_claims":0,"externally_anchored":false,"storage_verified":false,"citation_signatures":0,"replication_records":0,"graph_snapshot":true,"references_resolved":false,"formal_links_present":false},"canonical_record":{"source":{"id":"astro-ph/0103171","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2001-03-12T16:59:25Z","cross_cats_sorted":[],"title_canon_sha256":"08dab9163d4ecc19fa224f1aa6da54117ff6f802ad6972e1472ffadf872eaf54","abstract_canon_sha256":"e3aee2b50cf13b4fd7cd49268d97a71f5de9edf2f432ea488390f8185f97dbb9"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:07:45.984466Z","signature_b64":"uEp0P7z+pvO67W2ObBU3izI3SKCmWe+YNTm5tXZAA3T2lFN6AMo7I/+yPHnqvdQXuSnH6FNg/StUarCSXsbWCw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"b612798e43b21c2e4fb1a1348239bc1726ab62bb00f32a53d5e8366cb2ea0d69","last_reissued_at":"2026-05-18T01:07:45.984010Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:07:45.984010Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The X-ray Spectrum of the Vela Pulsar Resolved with Chandra","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"D. 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