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We find the following abundances (by number) with respect to solar: He/H = 1.0 $\\pm$ 0.4, C/H = 7.0 $^{+7}_{-4}$, N/H = 85 $^{+59}_{-41}$ and O/H = 6 $^{+7}_{-2}$. In addition, there is weak evidence for solar Ne and Mg and twice solar Fe. Previous studies (Saizar et al. 1991 and Andre\\\"{a} et al. 1991, 1994) of PW Vul have yielded considerable differences in their derive"},"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/9705086","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"1997-05-12T21:25:06Z","cross_cats_sorted":[],"title_canon_sha256":"a9cbd27b09441c2ebee6639f220a005bacbc3703029144e5ebc159205df83388","abstract_canon_sha256":"046e6fd67779baa273fc644415afa8d158750e75a20daf03997353ba6438b990"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:40:17.489654Z","signature_b64":"sv6dX6YjchVy18lnDLEYJn8v/DpSPtkibKEoLgvxo9U6URm6e0exksB1TequiUxph5dcuR6eNLel6VOCetDjBQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"8842e71ed3ad8d1d6e166c102ade23e2193644e7ec3637abaca28eabb4177e4e","last_reissued_at":"2026-05-18T01:40:17.489035Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:40:17.489035Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Abundance analysis of the slow nova PW Vulpeculae 1984","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Greg J. 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