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We compute the Br{\\gamma} line profile originating from accretion columns for models with different magnetic obliquities. We also derive monochromatic synthetic images of the Br{\\gamma} line emitting region across the line profile. This spectral line is a prime diagnostics of magnetospheric accretion in young stars and is accessible with the long baseline near-infrared interferometer GRAVITY installed at the ESO Very Large Telescope Interferometer.\n  Results. We derive B"},"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":"2301.11628","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.SR","submitted_at":"2023-01-27T10:14:56Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"99bbb9261fc5d563e7e1e3a949781794884451a0b0cccba7640f7680b4799eb6","abstract_canon_sha256":"962cf6b0d97e34769adf787331d88fdc12f91e48060f9064d65afdc71c4f524e"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T05:50:59.903260Z","signature_b64":"lLfz+3d2+brYRI3T5f00/Q08kdfFPEdk/wRliQPtSsYjFuAHV15ErvefUM1DZdc1FbSRVfhsH+pwfaX1GzTGDw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"36859d7a17409b1356851a2d770537aeeefffa57fb59751cd2bd8f34c57d39df","last_reissued_at":"2026-07-05T05:50:59.902713Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T05:50:59.902713Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Spectroscopic and interferometric signatures of magnetospheric accretion in young stars","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.SR","authors_text":"A. Soulain, B. Tessore, C. Pinte, G. Pantolmos, J. Bouvier, K. Perraut","submitted_at":"2023-01-27T10:14:56Z","abstract_excerpt":"Methods. We use the code MCFOST to solve the non-LTE problem of line formation in non-axisymmetric accreting magnetospheres. We compute the Br{\\gamma} line profile originating from accretion columns for models with different magnetic obliquities. We also derive monochromatic synthetic images of the Br{\\gamma} line emitting region across the line profile. This spectral line is a prime diagnostics of magnetospheric accretion in young stars and is accessible with the long baseline near-infrared interferometer GRAVITY installed at the ESO Very Large Telescope Interferometer.\n  Results. 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