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Extremely irradiated hot Jupiters, exoplanets reaching dayside temperatures${>}$2000 K, stretch our understanding of planetary atmospheres and the modelswe use to interpret observations. While these objects are planets in everyother sense, their atmospheres reach temperatures at low pressures comparableonly to stellar atmospheres. In order to understand our \textit{a priori}theoretical expectations for the nature of these objects, we self-consistentlymodel a number of extreme hot Jupiter scenarios with the PHOENIX modelatmosphere code. PHOENIX is well-tested on objects from cool brown dwarfs toexpanding supernovae shells and its expansive opacity database from the UV tofar-IR make PHOENIX well-suited for understanding extremely irradiated hotJupiters. We find several fundamental differences between hot Jupiters attemperatures ${>}$2500 K and their cooler counterparts. First, absorption byatomic metals like Fe and Mg, molecules including SiO and metal hydrides, andcontinuous opacity sources like H$^-$ all combined with the short-wavelengthoutput of early-type host stars result in strong thermal inversions, withoutthe need for TiO or VO. Second, many molecular species, including H$_2$O, TiO,and VO are thermally dissociated at pressures probed by eclipse observations,biasing retrieval algorithms that assume uniform vertical abundances. Wediscuss other interesting properties of these objects, as well as futureprospects and predictions for observing and characterizing this unique class ofastrophysical object, including the first self-consistent model of the hottestknown jovian planet, KELT-9b.

Extremely Irradiated Hot Jupiters: Non-Oxide Inversions, H- Opacity, and Thermal Dissociation of Molecules