Rotating white dwarfs undergoing quasi-radial oscillations can emit gravitational radiation in a frequency range from 0.1 to 0.3 Hz. Assuming that the energy source for the gravitational radiation comes from the oblateness of the white dwarf induced by the rotation, the strain amplitude is found to be âˆ¼10-27 for a white dwarf at âˆ¼50 pc. The Galactic population of these sources is estimated to be âˆ¼107 and may produce a confusion-limited foreground for proposed advanced detectors in the frequency band between space-based and ground-based interferometers. Nearby oscillating white dwarfs may provide a clear enough signal to investigate white dwarf interiors through gravitational wave asteroseismology.
M. Benacquista, et. al., (2003) Gravitational radiation from pulsating white dwarfs.Astrophysical Journal596:2L223. DOI: http://doi.org/10.1086/379532