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The SN1987A Environment

Published online by Cambridge University Press:  12 April 2016

Lifan Wang  and
E. Joseph Wampler
Lifan Wang
Affiliation:
Beijing Astronomical Observatory, Beijing 100080, P.R. China
E. Joseph Wampler
Affiliation:
European Southern Observatory, Karl-Schwarzschild-straße 2, Garching bei München, D-85748 Germany

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The environment of the SN1987A is quite complex but also very regularly structured. Detailed analyses of direct images taken under good seeing conditions (0.3—0.8 arcsec) from the European Southern Observatory (ESO)'s New Technology Telescope (NTT) show that there are two nebular loops within the 3 arcsec environment of the SN. The inner loop is elliptical in shape. The kinematics of this loop as revealed by spectroscopic data with a spectral resolving power λ/Δλ « 30 000 provide further clues for the three dimensional structure of these two loops. The data show that the overall structure of the nebulosity can be understood by an hourglass-shaped shell with significant mass enhancement on its equatorial plane. A diffuse nebulosity called Napoleon's Hat is observed at a distance of about 5 arcsec to the north of the SN. It showed little size evolution since the first observation on Aug. 1989, until it disappeared on Jan, 1992. The Napoleon's Hat nebula appears to be a bow-shock coming from an interaction between the supernova progenitor's stellar wind and the interstellar medium, as the supernova progenitor moved through the interstellar medium with a velocity of around 5 kms-1. On an even larger scale, there is a huge dark bay of size around 100 arcsec in diameter, we suggested that this bay was also formed by interactions between the supernova progenitor and the interstellar medium.

The narrow emission lines indicate that the electron density and temperature of the emission gas in the loops are steadily decreasing. However, the temperatures inferred from the [OIII] nebular lines remained persistently higher than 2 × 104K. They were around 104cm−3 and 2 × 104K on Aug. 30, 1990. In addition, a global difference in the electron density of the two major axis of the inner loop is observed in the images and spectra taken five years after the supernova explosion. We have also studied the two neighboring stars surrounding the supernova. We find that star 2 is a B star with Hα and Hβ emission lines.

The supernova circumstellar nebulosity is remarkably similar to certain types of planetary nebula, e.g. NGC2392. Asymmetric wind interaction models for the formation of planetary nebula are applied to produce a model in the form of an hourglass shaped shell. This model invokes both a slow wind while the star was in its red supergiant phase and a fast wind during the later blue supergiant stage before explosion. Although such wind interaction models fit the observed nebular structures satisfactorily, they are so idealized that they tell us little about the origin of the seed asymmetry or the amount of seed asymmetry needed to produce the observed real nebula.

Type
Supernovae and Circumstellar Matter
Information
International Astronomical Union Colloquium , Volume 145: Supernovae and Supernova Remnants , 1996 , pp. 299 - 308
Copyright
Copyright © Cambridge University Press 1996

References

Blondin, J. & Lundqvist, P. 1993, ApJ, 405, 337 Google Scholar
Bond, H. E., Gilmozzi, R., Meakes, M. G., & Panagia, N. 1990, ApJL, 347, L65.Google Scholar
Chevalier, R. A. & Emmering, R. T., 1989, ApJL, 342, L75.Google Scholar
Chevalier, R. A. & Luo, D., 1994, ApJ, 421, 225.Google Scholar
Crotts, A. P. S. 1988. IAU Cire. 4561 Google Scholar
Crotts, A. P. S., & Heathcote, S. R. 1991, Nature, 350, 683.Google Scholar
Crotts, A. P. S., & Kunkel, W. E. 1991, ApJL 366, L73.Google Scholar
Crotts, A. P. S., Kunkel, W. E., & McCarthy, P. J. 1989, ApJL, 347, L61.Google Scholar
D'Odorico, S., & Baade., D. 1989, ESO Messenger, 56, 35.Google Scholar
Elias, J. H., Phillips, M. M., Suntzeff, N. B., Walker, A. R., Gregory, B., & Depoy, D. L. 1993, in Massive Stars: Their lives in the Interstellar Medium, Ed. Cassinelli, J. P. & Churchwell, E. B., P408.Google Scholar
Felten, J. E. & Dwek, E., in SN1987A and Other Supernovae, ed. Danziger, I. J. & Kjär, K. P569.Google Scholar
Fransson, C., Cassatella, A., Gilmozzi, R., Kirshner, R. P., Panagia, N., Sonneborn, G., Sauvageot, J. L., & Wamsteker, W., 1989, ApJ, 336, 429.Google Scholar
Gouiffes, C., Rosa, M., Melnick, J., Danziger, I. J., Renny, M., Santini, C., Sauvageot, J. L., Jakobsen, P., & Ruiz, M. T., 1988 A&A 198, L9 Google Scholar
Jakobsen, P., et al 1991 ApJL, L63.Google Scholar
Kahn, F. D., & West, K. A. 1985 MNRAS, 212, 837.Google Scholar
Luo, D., 1992, Ph. D. thesis, University of Colorado.Google Scholar
Luo, D., & McCray, R. 1991, ApJ, 379, 659.Google Scholar
Lundqvist, P., & Fransson, C. 1991, ApJ, 380, 575.Google Scholar
Meikle, W. P. S., Cumming, R. J., Spyromilio, J., Allen, D. A., & Mobasher, B. 1990, in Proceedings of the ESO/EIPC Workshop on SN 1987A and other Supernovae ed. Danziger, I. J., p595.Google Scholar
Nomoto, K., Shigeyama, T., Hashimoto, M., in Proceedings of the ESO/EIPC Workshop on SN 1981A and other Supernovae ed. Danziger, I. J., p325.Google Scholar
Panagia, N., Gilmozzi, R., Macchetto, F., Adorf, H.-M., Kirshner, R.P. 1991, ApJL, 380, L23.Google Scholar
Sonneborn, G., & Wamsteker, W. 1989, ApJ, 336, 429.Google Scholar
Sparks, W. B., Paresce, F., & Macchetto, D. 1989, ApJL, 347, L65.Google Scholar
Wampler, E. J., & Richichi, A. 1989, A&A, 217, L21.Google Scholar
Wampler, E. J., Richichi, A., & Baade, D. 1989, in IAU Colloquium 120, Structure and Dynamics of the Interstellar Medium, ed. Tenorio-Tagle, G. Moles, M., & Melnick, J. (Berlin-Springer), P180.Google Scholar
Wampler, E. J, Wang, L., Baade, D., Banse, K., D'Odorico, S., Gouiffes, C., & Tarenghi, M. 1990, ApJL, 362, L13 (W90).Google Scholar
Wamsteker, W., Gilmozzi, R., Cassatella, A., & Panagia, N. 1987, IAU Circ, No. 4410.Google Scholar
Wang, L. 1991, A&A, 246, L69.Google Scholar
Wang, L., D'Odorico, S., & Wampler, E. J. 1992, IAU Circ. 5449.Google Scholar
Wang, L., Dyson, J. E., & Kahn, F. D. 1993, MNRAS, 261, 391.Google Scholar
Wang, L., & Mazzali, P. A. 1992, Nature, 355, 58.Google Scholar
Wang, L., & Rosa, M. 1992, ESO Messenger, 67, 37.Google Scholar
Wang, L. & Wampler, E. J. 1992, A&A, 262, L9.Google Scholar
Woosley, S., 1988, ApJ, 330, 218.Google Scholar