Doppler tomography of the circumstellar disk of {\pi} Aquarii
| Autor: | Zharikov, S. V., Miroshnichenko, A. S., Pollmann, E., Danford, S., Bjorkman, K. S., Morrison, N. D., Favaro, A., Flo, J. Guarro, Terry, J. N., Desnoux, V., Garrel, T., Martineau, G., Buchet, Y., Ubaud, S., Mauclaire, B., Kalbermatten, H., Buil, C., Sawicki, C. J., Blank, T., Garde, O. |
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| Rok vydání: | 2013 |
| Předmět: | |
| Zdroj: | A&A 560, A30 (2013) |
| Druh dokumentu: | Working Paper |
| DOI: | 10.1051/0004-6361/201322114 |
| Popis: | 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 period of 84.2(2) days and is in agreement with the earlier determined orbital period of the system, Porb=84.1 days. The V/R ratio shows a sinusoidal variation phase-locked with the orbital period. Doppler maps of all our spectra show a non-uniform structure of the disk around the primary: a ring with the inner and outer radii at Vin~ 450 km/s and Vout~ 200km/s, respectively, along with an extended stable region (spot) at V_x ~ 225 km/s and V_y~100 km/s. The disk radius of ~ 65 Rsun = 0.33 AU was estimated assuming Keplerian motion of a particle on a circular orbit at the disk outer edge. Comment: 11 pages, 7 figures, 2 tables, published in A&A |
| Databáze: | arXiv |
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