2009/03/23 by M. Contini, R. Angeloni, P. Rafanelli
Physics and Astronomy · #Accretion (finance) #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Ejecta #Emission spectrum #Galaxy #Gamma-ray bursts and supernovae #Interstellar medium #Millimeter #Nebula #Physics #Shock wave #Spectral energy distribution #Spectral line #Stars #Stellar, planetary, and galactic studies #Supernova #Symbiotic star #White dwarf #astro-ph.HE #astro-ph.SR
paper · pdf · doi:10.1111/j.1365-2966.2009.14792.x
13 pages, 9 figures, 2 tables; accepted for publication in MNRAS
arxiv created 2009/03/23 · openalex publication_date 2009/05/20 · arxiv updated 2015/05/13 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We investigate the symbiotic star BI Crucis (BI Cru) through a comprehensive and self-consistent analysis of the spectra emitted in three different epochs: 1960s, 1970s and late 1980s. In particular, we would like to find out the physical conditions in the shocked nebula and in the dust shells, as well as their location within the symbiotic system, by exploiting both photometric and spectroscopic data from radio to UV. We suggest a model which, on the basis of optical imaging, emission-line ratios and spectral energy distribution profile, is able to account for collision of the winds, formation of lobes and jets by accretion onto the white dwarf (WD), as well as for the interaction of the blast wave from a past, unrecorded outburst with the interstellar medium (ISM). We have found that the spectra observed throughout the years show the marks of the different processes at work within BI Cru, perhaps signatures of a post-outburst evolution. We then call for new infrared and millimeter observations, potentially able to resolve the inner structure of the symbiotic nebula.