{"paper":{"title":"Doppler tomography of the circumstellar disk of {\\pi} Aquarii","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"A. Favaro, A. S. Miroshnichenko, B. Mauclaire, C. Buil, C. J. Sawicki, E. Pollmann, G. Martineau, H. Kalbermatten, J. Guarro Flo, J. N. Terry, K. S. Bjorkman, N. D. Morrison, O. Garde, S. Danford, S. Ubaud, S. V. Zharikov, T. Blank, T. Garrel, V. Desnoux, Y. Buchet","submitted_at":"2013-10-24T07:01:03Z","abstract_excerpt":"The work is aimed at a study of the circumstellar disk of the bright classical binary Be star {\\pi} Aqr. We analysed variations of a double-peaked profile of the H{\\alpha} emission line in the spectrum of {\\pi} Aqr that was observed in many phases during ~40 orbital cycles in 2004--2013. We applied the Discrete Fourier Transform (DFT) method to search for periodicity in the peak intensity (V/R) ratio. Doppler tomography was used to study the structure of the disk around the primary. The dominant frequency in the power spectrum of the H{\\alpha} V/R ratio is 0.011873 day^-1 that correspond to a "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1310.6499","kind":"arxiv","version":2},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"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"}