2005/10/03 by Fabiola M. A. Ribeiro, Fabíola Mariana Aguiar Ribeiro, Marcos P. Diaz · 7 citations
Physics and Astronomy · #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Astrophysics and Star Formation Studies #Binary number #Binary star #Emission spectrum #Emissivity #Galaxies: Formation, Evolution, Phenomena #Geometry #Line (geometry) #Nova (rocket) #Optics #Orbital inclination #Physics #Radial velocity #Roche lobe #Spectral line #Stars #astro-ph
paper · pdf · doi:10.1086/498458
published in Publications of the Astronomical Society of the Pacific 118(839), 84-93 (Institute of Physics) · 8 pages, 8 figures, accepted to appear in PASP
arxiv created 2005/10/03 · openalex publication_date 2006/01/01 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We present the results of spectrophotometric observations of the old nova RR Pictoris performed in two spectral ranges, one centered in the Hα line, and other covering Hβ and Hγ spectral lines. From the Hβ radial velocity study, we found a primary radial semiamplitude of K 1 = 37(1) km s −1 and a systemic velocity of γ = 1.8(2) km s −1 . With these new values, a mass diagram is constructed, constraining the possible mass intervals for the system. The possible orbital inclination range was restricted, given the fact that RR Pic presents shallow eclipses. A secondary mass range below the limit of a main‐sequence star filling its Roche lobe indicates an evolved companion. We also calculated the Hα, Hβ, Hγ, He i λ6678, and He ii λ4686 Doppler tomograms. The most conspicuous differences are found between the He i and He ii tomograms; the former has a ring shape, while the second is filled at low velocities, suggesting that the low‐velocity emission is not coming from the accretion disk. Radial emissivity profiles for these lines were also derived.