Abstract

Observations have shown that planets similar to Neptune are rarely found orbiting Sun-like stars with periods up to similar to 4 days. This defines the so-called Neptune desert region. The detection of each individual planet in this region therefore holds a high value by providing detailed insights into the formation and evolution of this population. We report the detection of TOI-333b, a Neptune-desert planet with a mass, radius, and bulk density of 20.1 +/- 2.4 M-circle plus, 4.26 +/- 0.11 R-circle plus, and 1.42 +/- 0.21 g cm(-3). The planet orbits an F7V star every 3.78 d, whose mass, radius, and effective temperature are of 1.2 +/- 0.1 M-circle dot, 1.10 +/- 0.03 R-circle dot, and 6241(-62)(+73) K, respectively. TOI-333bis likely younger than 1 Gyr, which is supported by the doublet Li line around 6707.856 & Aring; and its comparison to Li abundances in open clusters with well-constrained ages. The planet is expected to host only a 8.5(-8.3)(+10.9)% gas-to-core mass ratio for an H/He envelope. On the other hand, models of irradiated ocean worlds predict a 20(-10)(+11)% H2O mass fraction with a core fraction of 35(-23)(+20)%. We therefore expect that the internal composition of TOI-333bis dominated by a pure rocky composition with almost no H/He envelope, or a rocky world with almost equal mass fraction of water. Finally, TOI-333bis more massive and larger than 77% and 82% of its Neptune-desert counterparts, and its host ranks among the hottest known stars for Neptune-desert planets. This makes this system a unique laboratory for studying the evolution of these planets around hot stars.