Hence, some of the monoperiodic variables found within the instability strip may be fast-spinning white dwarfs impersonating ZZ Ceti pulsators. In addition, the discovery of such fast rotators outside of the ZZ Ceti instability strip suggests that some should also exist within the strip. Long-term monitoring of the spin evolution of J2211+1136 and other fast-spinning isolated white dwarfs opens a new discovery space for substellar and planetary mass companions around white dwarfs. Given its large mass, fast rotation, strong magnetic field, unusual atmospheric composition, and relatively large tangential velocity for its cooling age, J2211+1136 displays all of the signatures of a double white dwarf merger remnant. A detailed model atmosphere analysis shows that it has a mixed hydrogen and helium atmosphere with a dipole field strength of Bd = 15 MG. with effective temperature Tef f (11560 70)K and mass M. SDSS J221141.80+113604.4 is a 1.27 M⊙ (assuming a CO core) magnetic white dwarf that shows 2.9% brightness variations in the BG40 filter with a 70.32 ± 0.04 s period, becoming the fastest spinning isolated white dwarf currently known. We studied the photometric variability in white dwarfs, through the use of the Period04. We obtained high-speed photometry of three ultramassive white dwarfs within 100 pc and discovered significant variability in one. We report the discovery of an isolated white dwarf with a spin period of 70 s. Any furtherĭistribution of this work must maintain attribution to the author(s) and the title This binary is the first spectroscopically confirmed widely separated. Of the Creative Commons Attribution 4.0 licence. We present the discovery of the widest known ultracool dwarfwhite dwarf binary. Original content from this work may be used under the terms The Astrophysical Journal Letters, 923(1). An isolated white dwarf with a 70 s spin period.
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