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Measuring g-mode pulsations of isolated white dwarfs can reveal theirinterior properties to high precision. With a spectroscopic mass of ~0.51M_{\odot} (log g = 7.82), the DAV white dwarf HS 1824+6000 is near thetransition between carbon/oxygen core and helium core white dwarfs, motivatingour photometric search for additional pulsations from the Palomar 60-inchtelescope. We confirmed (with much greater precision) the three frequencies:2.751190 +/- 0.000010 mHz (363.479 sec), 3.116709 +/- 0.6 mHz (320.851sec), 3.495113 +/- 0.9 mHz (286.114 sec), previously found by B. Voss andcollaborators, and found an additional pulsation at 4.443120 +/- 0.000012 mHz(225.067 sec). These observed frequencies are similar to those found in otherZZ Ceti white dwarfs of comparable mass (e.g. log g < 8). We hope that futureobservations of much lower mass ZZ Ceti stars (< 0.4 M_{\odot}) will revealpulsational differences attributable to a hydrogen covered helium core.

Pulsations of the Low Mass ZZ Ceti Star HS 1824+6000