Barium in SN 1987A and SNe II-P.

Details Barium in SN 1987A and SNe II-P. Barium in SN 1987A and SNe II-P.

Nov 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...303..118m&link_type=abstract

Astronomy and Astrophysics, v.303, p.118

Astronomy and Astrophysics

Astrophysics

20

Supernovae: General, Supernovae: Individual: Sn 1987A, Supernovae: Individual: Sn 1990H, Stars: Evolution, Abundances, Lines: Formation

Scientific paper

The problem of the dramatic difference in the intensity of the Ba II lines between SN 1987A (type II-pec) and normal SNe II-P in the photospheric epoch is studied by means of synthetic spectra computations. The evolution of the Ba II 6141A line in SN 1987A, including both the period between days 20 and 80, when the line was very strong, and epochs before and after that, when the line was weaker, is well reproduced for the Ba overabundance factor f=X/X_i_=5 (metal abundance X_i_=(1/2.75)xsolar for the LMC), in agreement with previous calculations for the early phase. It is found that the Ba overabundance is necessary for all layers in the ejecta with velocity between 1500 and 9000km/s, which include almost all the ejected mass. On the other hand, the Ba II lines in normal SNe II-P at the same epochs are well reproduced assuming a Ba overabundance factor 1

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