Central Stars of Planetary Nebulae: CYCLE3MED

Details Central Stars of Planetary Nebulae: CYCLE3MED Central Stars of Planetary Nebulae: CYCLE3MED

Jul 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993hst..prop.4844k&link_type=abstract

HST Proposal ID #4844

Computer Science

Hst Proposal Id #4844

Scientific paper

It has proved impossible to detect the very hot exciting stars of some planetary neblae from the ground. This is probably because these stars emit a great many ionizing photons for each visible quantum. The ionized nebula is therefore so extensive that the nebular emission, both line and continuum, completely dominate the visual continuum emission of the central star, which becomes lost in the noise. Observing above the atmosphere increases the possibility of detection of these central star by a factor of at least 400. A factor ~ 100 because the light of the central star is within an image of. 1" instead of the ~ 1" ground seeing limitation allowing better discrimination of the star against the diffuse nebular continuum and a further factor ~ 4 occurs because the star is that much brighter, relative to the nebula, in the ultraviolet than it is in the visible. With the spherical abberation of HST, the above mentioned factor of 100 is reduced to about 15, but as the UV adventage remains, detectability is still several magnitudes beyond groundobservations.

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