The Rapid Rotation of the Strongly Magnetic Ultramassive White Dwarf EGGR 156

The distribution of white dwarf rotation periods provides a means for constraining angular momentum evolution during the late stages of stellar evolution, as well as insight into the physics and remnants of double degenerate mergers. Although the rotational distribution of low-mass white dwarfs is relatively well constrained via asteroseismology, that of high-mass white dwarfs, which can arise from either intermediate-mass stellar evolution or white dwarf mergers, is not. Photometric variability in white dwarfs due to rotation of a spotted star is rapidly increasing the sample size of high-mass white dwarfs with measured rotation periods. We present the discovery of 22.4 minute photometric variability in the light curve of EGGR 156, a strongly magnetic, ultramassive white dwarf. We interpret this variability as rapid rotation, and our data suggest that EGGR 156 is the remnant of a double degenerate merger. Finally, we calculate the rate of period change in rapidly-rotating, massive, magnetic WDs due to magnetic dipole radiation. In many cases, including EGGR 156, the period change is not currently detectable over reasonable timescales, indicating that these WDs could be very precise clocks. For the most highly-magnetic, rapidly-rotating massive WDs, such as ZTF J1901+1450 and RE J0317-853, the period change should be detectable and may help constrain the structure and evolution of these exotic white dwarfs.

Automated summary

The distribution of white dwarf rotation periods is important for understanding angular momentum evolution and the remnants of double degenerate mergers. We discovered rapid rotation in the strongly magnetic white dwarf EGGR 156 based on its photometric variability, suggesting it is a remnant of a double degenerate merger. The rate of period change in rapidly-rotating, massive, magnetic white dwarfs can be detectable and may help constrain their structure and evolution.