Ultraviolet and Optical Observations of the Supernova 1987A with HST and IUE

Details Ultraviolet and Optical Observations of the Supernova 1987A with HST and IUE Ultraviolet and Optical Observations of the Supernova 1987A with HST and IUE

Jul 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998phdt........20p&link_type=abstract

Thesis (PHD). HARVARD UNIVERSITY , Source DAI-B 59/01, p. 260, Jul 1998, 195 pages.

Computer Science

Hubble Space Telescope, International Ultraviolet Explorer, Large Magellanic Cloud

Scientific paper

Supernova 1987A (SN 1987A) in the Large Magellanic Cloud provides a unique opportunity for the study of supernovae. Its proximity and brightness make it an ideal object for testing theories of supernovae, and of stellar evolution in general. Studies of SN 1987A are greatly enhanced by the space based observatories which extends the ground based results both in wavelength (International Ultraviolet Explorer IUE and Hubble Space Telescope HST) and in time coverage (HST). The spectroscopic and imaging observations obtained by IUE and HST on the SN 1987A debris are presented. In Chapter I, we study the evolution the ultraviolet spectrum of SN 1987A by generating a complete catalogue of the IUE data (day 1-1248). Special attention is paid on the correct background flux subtraction from neighboring stars. The bolometric luminosity of SN 1987A is re-calculated to properly include contribution from the UV flux, which becomes increasingly important in late times. Study of the UV color shows that the supernova debris gets bluer in UV around the time of dust formation, which may imply that the dust formed is metal rich. UV and optical observations of SN 1987A with HST started (day 1278) when it became difficult to observe it with IUE and from the ground. In Chapter II, we study the properties of the supernova debris by fitting the observed image profiles with a brightness function derived from the spectroscopic data. The size of the debris is measured over time and it is found to be expanding homologously at ~2800 km s-1 in all optical wavebands. The measured velocity reflects that of the radioactive Fe core and its magnitude suggests mixing of the newly synthesized Ni to the outer layers of the supernova envelope. With the post-service mission images, the shape and asymmetry of the debris can also be studied. The supernova atmosphere is asymmetric at ~10-15% and its major axis is aligned with the axis of the circumstellar ring system. In the last HST images taken in 1997 July (day 3792), small scale structures of the debris are observed. In Chapter III, the geometry and dynamics of these structures are shown to be consistent with a model where clump of materials are ejected above and below the plane of the circumstellar ring. This provides for the first time direct connection between the supernova explosion debris and its circumstellar gas and imposes important constraints on the progenitor models and explosion dynamics of the supernova.

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