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   PR # 11051
    SN1987A is providing us with a unique opportunity to study a super-
    nova remnant in their very early phase of evolution.  The ejecta is
    now thought to be colliding with the wind remnant of the blue super-
    giant stage of the progenitor. Thermal X-rays from such interaction
    may be detectable depending on the CSM density. Search for the emis-
    sion from the central pulsar is even more important. UV, optical and
    IR bolometric light curve implies some additional energy source other
    than 56Co. If there is indeed such emission from the pulsar, it will
    emerge as intense 6.4 keV Fe line and extremely hard continuum emis-
    sion because of absorption by the ejecta. The pulse period can be
    millisecond or less.

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