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This emission has been attributed to shock-heated accreting material impacting onto the stellar surface. Aims. We investigate the observability of the shock-heated accreting material in the X-ray band as a function of the accretion stream properties (velocity, density, and metal abundance) in the case of plasma-beta<<1 in the post-shock zone. Methods. We use a 1-D hydrodynamic model describing the impact of an accretion stream onto the chro"},"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":"1007.2423","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2010-07-14T20:13:15Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"aa0eacc552e31948bf1e2796489eb7fe50ad392187c530d27415a162bfc7f7e9","abstract_canon_sha256":"9e7f6a80328f11e46692ca163f7a63c9faa3d36b52b36ca4fbdd1b20bb95ab03"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:06:21.914050Z","signature_b64":"TudFXWT3HYb23RR0HwRk1Cmttt6tAxxSgH1L9QMWBXIg0QnaQ0aSZTr6pLUbz6y0EHqwpmtWdRRUfR/VITt+Cw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"3b01a1b74728b6ef8f730683ad87b7cf2ffa8d5eb7fe9199872ba8a72c3e2697","last_reissued_at":"2026-05-18T02:06:21.913375Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:06:21.913375Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"On the observability of T Tauri accretion shocks in the X-ray band","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.SR","authors_text":"A. Maggio, C. Argiroffi, F. Reale, G. G. Sacco, G. Peres, R. L. Curran, S. Orlando","submitted_at":"2010-07-14T20:13:15Z","abstract_excerpt":"Context. High resolution X-ray observations of classical T Tauri stars (CTTSs) show a soft X-ray excess due to high density plasma (n_e=10^11-10^13 cm^-3). This emission has been attributed to shock-heated accreting material impacting onto the stellar surface. Aims. We investigate the observability of the shock-heated accreting material in the X-ray band as a function of the accretion stream properties (velocity, density, and metal abundance) in the case of plasma-beta<<1 in the post-shock zone. Methods. 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