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We investigate the dynamics and stability of post-shock plasma streaming along nonuniform stellar magnetic fields at the impact region of accretion columns. We study how the magnetic field configuration and strength determine the structure, geometry, and location of the shock-heated plasma. METHODS. We model the impact of an accretion stream onto the chromosphere of a CTTS by 2D axisymmetric magnetohydrodynamic simulations. Our model takes into account the gravity, the radiative cooling, and the magnetic-field-oriented thermal conduction. RESULTS. The structure, stability, and"},"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":"1309.5038","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2013-09-19T16:18:26Z","cross_cats_sorted":[],"title_canon_sha256":"c808946a78e591961f33b15985e4028b1c1f0cb5b25672c10b93aa3afcaa817e","abstract_canon_sha256":"37c5a6434affa963a06811402c55f1cc8f310fe140ec22936a1a2e9b652ef34e"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:47:35.396328Z","signature_b64":"quCQVMok6JLAQ+Uj+JzP/rMbM1gjtkF6Bk08PfqnmftLFM+MqLxpZEeXnqiKlBNAKh9xRBCVivM8TwLT9Fg7AQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"81d336094abcb8b8ff3a51abbd66e360c18607208dd9f3cfa67ffbc73b1768f7","last_reissued_at":"2026-05-18T01:47:35.395591Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:47:35.395591Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Radiative accretion shocks along nonuniform stellar magnetic fields in classical T Tauri stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"C. Argiroffi, C. Stehl\\'e, F. Reale, G. Peres, J.P. Chi\\`eze, L. de S\\'a, L. Ibgui, M. Miceli, R. Bonito, S. Orlando, T. Lanz, T. Matsakos","submitted_at":"2013-09-19T16:18:26Z","abstract_excerpt":"(abridged) AIMS. We investigate the dynamics and stability of post-shock plasma streaming along nonuniform stellar magnetic fields at the impact region of accretion columns. We study how the magnetic field configuration and strength determine the structure, geometry, and location of the shock-heated plasma. METHODS. We model the impact of an accretion stream onto the chromosphere of a CTTS by 2D axisymmetric magnetohydrodynamic simulations. Our model takes into account the gravity, the radiative cooling, and the magnetic-field-oriented thermal conduction. RESULTS. 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