Astronomy and Astrophysics – Astrophysics
Scientific paper
Jan 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...253..447b&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 253, no. 2, Jan. 1992, p. 447-450.
Astronomy and Astrophysics
Astrophysics
16
Line Spectra, Peculiar Stars, Planetary Nebulae, Stellar Mass Ejection, Emission Spectra, Helium, Radiation Pressure, Stellar Winds
Scientific paper
The mass loss rate from the central star of NGC 40 was determined with two methods. By fitting the UV P Cygni profiles of C IV, Si IV, and He II, a value of log mass loss rate not greater than -5 solar mass/yr, was derived, assuming solar abundances. The star is a WC type, therefore He and C are likely to be overabundant, making the above value an upper limit. By comparing the He I and He II optical and UV emission lines with grids of models for pure He atmospheres of WR stars, log mass loss rate of about -6 was derived, and this value could be considered a lower limit. Therefore, the mass loss rate can be of this order. The measured values of terminal velocity, temperature, and mass loss rate, compared with the radiation pressure driven wind theory, confirm that the nucleus of NGC 40 is extremely massive (1 solar mass) for a central star of Planetary Nebula.
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