The Optical Spectrum of Nova Gq-Muscae 1983 from 1984 TO 1988

Details The Optical Spectrum of Nova Gq-Muscae 1983 from 1984 TO 1988 The Optical Spectrum of Nova Gq-Muscae 1983 from 1984 TO 1988

Apr 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...271..219p&link_type=abstract

Astronomy and Astrophysics, Vol.271, NO. 1/APRI, P. 219, 1993

Astronomy and Astrophysics

Astrophysics

15

Atomic And Molecular Data: Recombination, Lines: Identification, Interstellar Medium: Nebulae, Stars: Novae: Gq Mus 1983, Spectrophotometry: Optical

Scientific paper

A detailed comparison of theoretical synthetic spectra, comprising more than 500 lines, with five optical spectra of Nova GQ Muscae 1983 in its nebular and coronal stages allows the identification of numerous lines, particularly from N IV, N V, O IV, O V, and O VI, some of which never detected or identified before in astrophysics, providing a basis for a template spectrum of warm highly ionized nebulae. Intensities and upper limits are obtained for many forbidden lines, notably from high-ionization species.
Due to the large expansion velocity, the lines are frequently blended. The observed and synthesized spectra are superimposed on different scales to allow a direct evaluation of the quality of the fit and the actual detectability of individual lines.
Incomplete knowledge of atomic energy levels appears as a significant limitation to the spectral analysis.
Lines λ458.5 and λ501.7 nm are identified with [Ni IX], whose levels are not yet known. Hydrogenic lines of elements in the ionization stages VII and perhaps VIII are suspected in late spectra. Dielectronic O II lines are introduced on the basis of inexplicable features of the 1984 spectrum. The electron density is determined from [Fe VI] and [Fe VII] lines. Observation favours the theoretical [Fe VI] results of Nussbaumer & Storey (1978).
The resulting data set can put important constraints on the detailed modelling of the evolution of a nova shell. The absence of [Fe X] in 1984 and the lack of coronal line beyond [Fe X] and [Fe XI] until 1988 is confirmed, favouring the assumption of photoionization by the hot post-nova white dwarf (Krautter & Williams 1989).
The N III 464.0 nm Bowen lines cannot be explained by classical Bowen fluorescence. Similarly the 3s-3p lines of the 1s22s sequence are probably not entirely due to self-fluorescence.
Elemental abundances derived from recombination lines are smaller than those obtained previously.
Although the bulk of the gas is expanding at 800 km s-1, warm material is also detected with velocities up to 4400 km s-1 in early spectra and the ejection is asymmetrical.
Localized continuum enhancements observed in 1985 and 1986 are interpreted as broad high-ionization lines arising from the vicinity of the hot post-nova white dwarf. In 1988, lines may be partly emitted by the central binary object, explaining the relative flatness of the Balmer decrement.

Affiliated with

Also associated with

No associations

Rating

The Optical Spectrum of Nova Gq-Muscae 1983 from 1984 TO 1988 does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with The Optical Spectrum of Nova Gq-Muscae 1983 from 1984 TO 1988, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and The Optical Spectrum of Nova Gq-Muscae 1983 from 1984 TO 1988 will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1367854