Classical Nova V1405 Cas Had M ejecta > M accreted and so is Unlikely to be a Type Ia Supernova Progenitor

Nova 2021 Cassiopeia (V1405 Cas) was an ordinary J(175) neon nova with the white dwarf mass estimated to be M WD =0.60 plus or minus 0.10 M. I found an orbital period of P =0.1884 days, and have tracked 20 times of photometric minima from 2013--2025. I measure that P increased from before to after the eruption with P pre =0.1883919 plus or minus 0.0000018 days and P post =0.1884043 plus or minus 0.0000018 days, for ΔP / P =66-18+21 parts-per-million. With correction for the angular momentum loss by the binary during the eruption, I derive that the nova ejected M ejecta =7.5 times 10-4 M, with an extreme range of (2.9--40) times 10-4 M. The mass accreted during the previous eruption cycle comes from the trigger mass, and is M accreted =(1.6 plus or minus 0.4) times 10-4 M. V1405 Cas provides counterexamples against five claims about CV evolution that have dominated since the 1980s. First, V1405 Cas has positive, and this is contrary to the Magnetic Braking Model. Second, the ΔP is 20 times too small to allow the system to fade into a hibernation state. Third, M WD is decreasing over time, as shown by M ejecta > M accreted and by being a neon nova. Fourth, V1405 Cas is not a Type Ia supernova progenitor, for the same reasons. Fifth, the orbital period of V1405 Cas increased by + 75 ppm from 2013--2025, as a counterexample to the pervasive idea that cataclysmic variables are universally declining in period from evolution. V1405 Cas is the latest of recent measures of ΔP and for 52 cataclysmic variables and 25 X-ray binaries that have together refuted all five claims.