Other
Scientific paper
Feb 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apjs...66..125m&link_type=abstract
Astrophysical Journal Supplement Series (ISSN 0067-0049), vol. 66, Feb. 1988, p. 125-138. NSERC-supported research.
Other
55
Emission Spectra, H Ii Regions, Hydrogen Recombinations, Line Spectra, Radiative Recombination, Stellar Radiation, Hydrogen Ions, Nova, Recombination Coefficient
Scientific paper
The radiative recombination of hydrogenic ions is calculated in the limit of low density by the 'nl-method', extending the results of Pengelly (1964) to much lower temperatures (both case A and case B). A strong motivation is the detection of the emission-line spectrum of the old shell of Nova DQ Her 1934 reported by Williams et al. (1978), which revealed an electron temperature T(e) of about 500 K. The results are compared with the 1959 result of Seaton using the 'n-method', with those of Hummer and Storey (1987), which allow for the effects of collisions at finite density, and with the data for three cold old nova shells. Another motivation is the detection of relatively strong optical radiative recombination lines of C, N, and O in these shells. The abundances of these elements (recombining ions of charge Z) can be derived using a hydrogenic approximation to the effective radiative recombination coefficients, requiring the recombination coefficients of H(+) at even lower temperatures.
No associations
LandOfFree
Hydrogenic radiative recombination at low temperature and density 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 Hydrogenic radiative recombination at low temperature and density, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Hydrogenic radiative recombination at low temperature and density will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1225177