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The Line Emission from the Circumstellar Gas Around SN 1987A | | P. Lundqvist
; C. Fransson
; | | Date: |
6 Dec 1995 | | Abstract: | The narrow emission lines from the inner ring around SN 1987A during the first $sim 2000$ days are modeled. The analysis extends that in Lundqvist & Fransson (1991) to include an improved description for the geometry, a multi-density structure of the emitting gas, results from improved calculations for the evolu- tion of the EUV radiation from the outburst, and updated atomic data. The ring has to be optically thick to the ionizing radiation, as is the case for a ring geometry, but not for a spherical shell. The density of the observed gas in the ring ranges from $(6.0pm1.0)EE{3} cm3$ to $3.3EE{4} cm3$. The early ($t lesssim 410$ days) UV line emission is dominated by the gas with the high- est density. Gas of lower density than $sim 6EE{3} cm3$ may be present in the ring, but will not dominate the emission until after $sim 2000$ days. The ionized mass observed up to day 1882 is $sim 4.5EE{-2} Msun$. The He/H ratio is $0.25pm0.05$, and the overall abundance of C, N and O is $0.30pm0.05$ times solar with relative abundances ${
m N/C} = 5.0pm2.0$ and ${
m N/O} = 1.1pm0. 4$. The peak effective temperature of the burst is in the range $(5-8)EE{5}$ K. The corresponding color temperature is $(1.0-1.5)EE6$ K. To model the $NV$~ $lambda$1240 light curve, resonance scattering in a medium external to the ring is needed. It is shown that the $NV$ line scattering can be used to discrimi- nate between models for the formation of the inner ring and the extended nebula. | | Source: | arXiv, astro-ph/9512025 | | Services: | Forum | Review | PDF | Favorites | |
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