High resolution spectroscopy of the inner ring of SN 1987A
Stockholm University, Faculty of Science, Department of Astronomy2008 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, Vol. 479, no 3, 761-777 p.Article in journal (Refereed) Published
We discuss high resolution VLT/UVES observations (FWHM similar to 6 kms(-1)) from October 2002 (day similar to 5700 past explosion) of the shock interaction of SN 1987A and its circumstellar ring. A large number of narrow emission lines from the unshocked ring, with ion stages from neutral up to Ne V and Fe VII, have been identified. A nebular analysis of the narrow lines from the unshocked gas indicates gas densities of (similar to 1.5 - 5.0) x 10(3) cm(-3) and temperatures of similar to 6.5 x 10(3) - 2.4 x 104 K. This is consistent with the thermal widths of the lines. From the shocked component we observe a large range of ionization stages from neutral lines to [FeXIV]. From a nebular analysis we find that the density in the low ionization region is 4 x 10(6) - 10(7) cm-3. There is a clear difference in the high velocity extension of the low ionization lines and that of lines from [Fe X - XIV], with the latter extending up to similar to- 390 km s(-1) in the blue wing for [Fe XIV], while the low ionization lines extend to typically similar to- 260 km s(-1). For H alpha a faint extension up to similar to- 450 km s(-1) can be seen probably arising from a small fraction of shocked high density clumps. We discuss these observations in the context of radiative shock models, which are qualitatively consistent with the observations. A fraction of the high ionization lines may originate in gas which has yet not had time to cool, explaining the difference in width between the low and high ionization lines. The maximum shock velocities seen in the optical lines are similar to 510 km s(-1). We expect the maximum width of especially the low ionization lines to increase with time.
Place, publisher, year, edition, pages
2008. Vol. 479, no 3, 761-777 p.
Astronomy, Astrophysics and Cosmology
IdentifiersURN: urn:nbn:se:su:diva-25563DOI: 10.1051/0004-6361:20077604ISI: 000253454600015OAI: oai:DiVA.org:su-25563DiVA: diva2:199982
Part of urn:nbn:se:su:diva-82902008-11-132008-11-132012-05-28Bibliographically approved