Astronomy and Astrophysics – Astronomy
Scientific paper
Apr 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991azh....68..349c&link_type=abstract
Astronomicheskii Zhurnal (ISSN 0004-6299), vol. 68, Mar.-Apr. 1991, p. 349-361. In Russian.
Astronomy and Astrophysics
Astronomy
2
Emission Spectra, Stellar Envelopes, Supernova 1987A, Symmetry, Gamma Ray Spectra, H Lines, Metallicity, Red Shift, Stellar Mass, Stellar Models
Scientific paper
Consideration is given to the origin of the anomalous structure in the profiles of the emission lines observed in the spectrum of SN 1987A; namely, the redshift of maxima and the fine structure of hydrogen lines. At least two of the three proposed hypotheses for the redshift have serious drawbacks. The most favourable is the third, which points to the asymmetric distribution of Ni-56 and of the iron-peak elements. The cloud of Ni-56 responsible for the redshifted emission has a mass of about 0.01 solar mass and lies at the level 1000-2000 km/s. The asymmetric distribution of the iron-peak elements suggested by the redshift model can be tested by observing the profile of the gamma-ray line 1159 KeV from decay (Ti-44)-(Sc-44)-(Ca-44) at the transparent phase t is greater than 4 yrs. It is suggested that the hydrogen lines' fine structure is due to the asymmetric cloud distribution of Ni-56 at the level 4000-5000 km/s. The cloud responsible for the redshifted component of the fine structure has the greatest Ni-56 mass; namely, 0.00001-0.001 solar mass.
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