Novae ejecta as colliding shells
Robert Williams,Elena Mason +1 more
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TLDR
In this article, the authors show that the emission profiles of novae in the nebular phase are distinctly rectangular, i.e., strongly suggestive of emission from a relatively thin, roughly spherical shell.Abstract:
Following on our initial absorption-line analysis of fifteen novae spectra we present additional evidence for the existence of two distinct components of novae ejecta having different origins. As argued in Paper I one component is the rapidly expanding gas ejected from the outer layers of the white dwarf by the outburst. The second component is pre-existing outer, more slowly expanding circumbinary gas that represents ejecta from the secondary star or accretion disk. We present measurements of the emission-line widths that show them to be significantly narrower than the broad P Cygni profiles that immediately precede them. The emission profiles of novae in the nebular phase are distinctly rectangular, i.e., strongly suggestive of emission from a relatively thin, roughly spherical shell. We thus interpret novae spectral evolution in terms of the collision between the two components of ejecta, which converts the early absorption spectrum to an emission-line spectrum within weeks of the outburst. The narrow emission widths require the outer circumbinary gas to be much more massive than the white dwarf ejecta, thereby slowing the latter’s expansion upon collision. The presence of a large reservoir of circumbinary gas at the time of outburst is suggestive that novae outbursts may sometime be triggered by collapse of gas onto the white dwarf, as occurs for dwarf novae, rather than steady mass transfer through the inner Lagrangian point.read more
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Shocks in nova outflows – I. Thermal emission
Brian D. Metzger,Romain Hascoet,Indrek Vurm,Indrek Vurm,Andrei M. Beloborodov,Laura Chomiuk,J. L. Sokoloski,T. J. N. Nelson +7 more
TL;DR: In this article, a one dimensional model for the shock interaction between the fast nova outflow and a dense external shell (DES) and its associated X-ray, optical, and radio emission is presented.
Journal ArticleDOI
The spectroscopic evolution of the recurrent nova T Pyxidis during its 2011 outburst - I. The optically thick phase and the origin of moving lines in novae
TL;DR: In this article, the authors derived the physical properties of the recurrent nova T Pyx and the structure of the ejecta during the early stages of expansion of the 2011 outburst.
Journal ArticleDOI
ORIGIN OF THE “He/N” AND “Fe II” SPECTRAL CLASSES OF NOVAE
TL;DR: In this paper, a finding list of emission lines identified in recent spectroscopic surveys of novae is presented as an aid to future line identification work, and it is shown that most novae may be hybrids that show both types of spectra during decline.
Journal ArticleDOI
The radio light curve of the gamma-ray nova in v407 cyg: thermal emission from the ionized symbiotic envelope, devoured from within by the nova blast
Laura Chomiuk,Laura Chomiuk,Laura Chomiuk,Miriam I. Krauss,Michael P. Rupen,Thomas Nelson,Nirupam Roy,Jennifer L. Sokoloski,Koji Mukai,Koji Mukai,Ulisse Munari,Amy J. Mioduszewski,Jennifer Weston,Tim O'Brien,S. P. S. Eyres,Michael F. Bode +15 more
TL;DR: In this paper, the authors present multi-frequency radio observations of the 2010 nova event in the symbiotic binary V407 Cygni, obtained with the Karl G. Jansky Very Large Array (VLA) and spanning 1.45 GHz and 17.770 days following discovery.
Journal ArticleDOI
The spectroscopic evolution of the recurrent nova T Pyxidis during its 2011 outburst. II. The optically thin phase and the structure of the ejecta in recurrent novae
S. N. Shore,Greg J. Schwarz,I. De Gennaro Aquino,T. Augusteijn,F. M. Walter,Sumner Starrfield,Edward M. Sion +6 more
TL;DR: In this paper, the structure and filling factor of the ejecta were derived from comparison to the optical and ultraviolet line profiles of the nova T Pyx during its 2011 explosion. But the authors did not consider the dynamics of the explosion.
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