The 600 images collected during the observing session were analyzed photometrically using the capabilities of the MAXIM DL5 software. There are numerous reference/comparison stars available for the analysis as shown on an AAVSO finder chart obtained at http://www.aavso.org/vsp/chart under the name HT Cas.
Finder chart from AAVSO "Variable Star Plotter" for HT Cas
The analysis used the star identified in the AAVSO data base as 000-BBC-408, at magnitude 12.8. A magnitude 12.3 check star (000-BBC-458) was also measured. Here is the light curve.
Light curve complete cycle in about 106 minutes.
The sharp dip corresponds to the time when the white dwarf star (presently in nova outburst) is hidden by its red giant companion. Note the interesting other structure to the light curve. After the deepest part of the eclipse, a relatively long period of constant light is seen before a rise to maximum before the next eclipse. A couple of smaller dips are seen on the way to maximum. Is this due to the accretion disc? I hope to learn more about the structure of this system in the weeks ahead.
Thoughts or comments anyone?
Clear Skies!
Randy B
