The properties could be explained by a non-solar carbon-to-oxygen ratio, meaning that it formed inside a disk around L 34–26.

In the second scenario L 34-26 is not actually young, but mimics youth due to tidal and/or magnetic interactions with an unseen companion.

[9] Another study found that their preferred model showed a metallicity that is lower than the host star, which is inconsistent with in-situ binary-like formation.

[2][4] Due to its large orbital separation, COCONUTS-2b is a great laboratory to study the atmosphere and composition of young gas-giant exoplanets.

Additionally the atmosphere shows a diabatic thermal structure, meaning the pressure-temperature profile is non-adiabatic.

[14] The star is seen almost equator-on with i = 81.8±5.8 deg and might belong to the proposed Ursa Major corona, which is 400 million years old.