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In these cases the 1D approximation is not valid and a multi-dimensional MHD approach is necessary.\n  METHODS. We model an accretion stream propagating through the atmosphere of a CTTS and impacting onto its chromosphere, by performing 2D axisymmetric MHD simulations. The model takes into account the stellar magnetic field, the gravity, the radiative cooling, and the thermal conduction (including the effects of heat flux saturation).\n  RESULTS. The dynamics "},"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":"0912.1799","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2009-12-09T16:52:08Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"61a07cbc5427907cfda8760a5ff2d402a5ff0966c92cb11b8f59721039442aa3","abstract_canon_sha256":"3dba02c4b551693bc9b445546c211a2e1db663347291a2b2aee532e64c067892"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:10:25.172084Z","signature_b64":"jmDQAFJB0sYTOAtbLUIuC4WnWdXyRpdnwUkOY7z4Q7b3aHblgv2EdpoO7UtfC1D/g7fay43SyuviSsBHOudhDA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"94cc2054812595e68c42504c3613dd4e00edcbc742f30b7671f8c3aa08da8b72","last_reissued_at":"2026-05-18T02:10:25.171354Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:10:25.171354Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"X-ray emitting MHD accretion shocks in classical T Tauri stars. 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