{"paper":{"title":"Rectangular core-collapse supernova remnants: application to Puppis A","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.GA","astro-ph.SR"],"primary_cat":"astro-ph.HE","authors_text":"04053, 04510, 1428, 14476 Potsdam, 15236, 15738 Zeuthen, 28040 Madrid, 3 Observatorna str. Kyiv, 4), 6), 7), 79060 Lviv, A. Castellanos-Ramirez (11), A. Chiotellis (5), A. Esquivel (2) ((1) Universitat Potsdam, Ap. 70-264, Argentina (10) Departamento de Materiales y Tecnolog\\'ia, Argentina (11) Universidad Nacional Aut\\'onoma de M\\'exico, Astrophysics, Av. Int. G\\\"uiraldes 2620, Av. V\\'elez Sarsfield 1611, Buenos Aires, CDMX, Ciudad Universitaria, C\\'ordoba, CP 04510, D-85748 Garching, Data Facility (MPCDF), D. M.-A. Meyer (1), E.M. Reynoso (9), E.M. Schneiter (10), F. Camps-Farina (2, FCEFyN-UNC, Germany (2) Instituto de Ciencias Nucleares, Germany (7) Departamento de F\\'isica de la Tierra y Astrof\\'isica, Germany (9) Instituto de Astronom\\'ia y Fisica del Espacio (IAFE), Gie{\\ss}enbachstrasse 2, Greece (6) DESY Platanenallee 6, Institut fur Physik und Astronomie, Instituto de Astronom\\'ia, J.C. Toledo-Roy (2), Karl-Liebknecht-Strasse 24/25, Mathematics, M\\'exico), Mexico (3) Institute for Applied Problems in Mechanics, Mexico City, M. Petrov (8), M. Pohl (1, NAS of Ukraine, National Observatory of Athens, Naukova 3-b, O. Petruk (3, Pabell\\'on IAFE, Penteli, P.F. Velazquez (2), Remote Sensing, Space Applications, Spain (8) Max Planck Computing, Ukraine (4) Astronomical Observatory of Taras Shevchenko National University of Kyiv, Ukraine (5) Institute for Astronomy, Universidad Complutense de Madrid, Universidad Nacional Autonoma de Mexico","submitted_at":"2022-06-29T09:32:39Z","abstract_excerpt":"Core-collapse supernova remnants are the gaseous nebulae of galactic interstellar media (ISM) formed after the explosive death of massive stars. Their morphology and emission properties depend both on the surrounding circumstellar structure shaped by the stellar wind-ISM interaction of the progenitor star and on the local conditions of the ambient medium. In the warm phase of the Galactic plane (n = 1/cm3, T = 8000 K), an organised magnetic field of strength 7 microG has profound consequences on the morphology of the wind bubble of massive stars at rest. In this paper we show through 2.5D magn"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2206.14495","kind":"arxiv","version":1},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2206.14495/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}