QZ Serpentis (abbreviated QZ Ser) is a binary star system consisting of an orange dwarf and a white dwarf, located approximately 1050 light-years away from us in the constellation Serpens. It is considered a dwarf nova because the white dwarf draws the outer layers of hydrogen from the star. The two stars orbit each other once every 119.752 minutes or 2 hours, and they may also be accompanied by a third substellar companion, whose mass is only about half that of Jupiter. QZ Ser was discovered by Katsumi Haseda in 1998.
Planetary system
In 2022, Carlos E. Chavez et al. decided to test the third-body hypothesis in cataclysmic variables using very long photometric periods, and based their study on four systems. During their research, they found additional evidence supporting this hypothesis in three systems, including QZ Serpentis. The candidate planet is in a circular orbit with a mass of 0.63 MJ and a semi-major axis of 0.019 AU. The mass and semi-major estimates assume that the planetary orbit is in the plane of the binary star orbit.
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