A1 Refereed original research article in a scientific journal
Two new nova shells associated with V4362 Sagittarii and DO Aquilae
Authors: E. J. Harvey ,M. P. Redman, P. Boumis , S. Akras , K. Fitzgerald , S. Dulaimi, S. C. Williams, M. J. Darnley, M. C. Lam, M. Kopsacheilli, S. Derlopa
Publisher: OXFORD UNIV PRESS
Publication year: 2020
Journal: Monthly Notices of the Royal Astronomical Society
Journal name in source: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Journal acronym: MON NOT R ASTRON SOC
Volume: 499
Issue: 2
First page : 2959
Last page: 2976
Number of pages: 18
ISSN: 0035-8711
eISSN: 1365-2966
DOI: https://doi.org/10.1093/mnras/staa2896
Self-archived copy’s web address: https://research.utu.fi/converis/portal/detail/Publication/50628137
A classical nova is an eruption on the surface of a white dwarf in an accreting binary system. The material ejected from the white dwarf surface generally forms an axisymmetric shell. The shaping mechanisms of nova shells are probes of the processes that take place at energy scales between planetary nebulae and supernova remnants. We report on the discovery of nova shells surrounding the post-nova systems V4362 Sagittarii (1994) and more limited observations of DO Aquilae (1925). Distance measurements of 0.5+1.4 -0.2 kpc for V4362 Sgr and 6.7 +/- 3.5 kpc for DO Aql are found based on the expansion parallax method. The growth rates are measured to be 0.07 arcsec yr-1 for DO Aql and 0.32 arcsec yr-1 for V4362 Sgr. A preliminary investigation into the ionization structure of the nova shell associated with V4362 Sgr is presented. The observed ionization structure of nova shells depends strongly on their morphology and the orientation of the central component towards the observer. X-ray, IR, and UV observations as well as optical integral field unit spectroscopy are required to better understand these interesting objects.
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