Doppler tomography of the circumstellar disk of π Aquarii

Abstract

The work is aimed at a study of the circumstellar disk of the bright classical binary Be star π Aqr. We analysed variations of a double-peaked profile of the Hα emission line in the spectrum of π 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 Hα 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.

11 pages, 7 figures, 2 tables, published in A&A

References in corpus (3)

• FUV Detection of the Suspected Subdwarf Companion to the Be Star 59 Cygni
• Detection of a Hot Subdwarf Companion to the Be Star FY Canis Majoris
• The 2011 Periastron Passage of the Be Binary delta Scorpii

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