  Several chemical networks have been developed to study warm (exo)planetary
atmospheres. The kinetics of the reactions related to the methanol chemistry
included in these schemes have been questioned. The goal of this paper is to
update the methanol chemistry for such chemical networks thanks to recent
publications in the combustion literature. We aim also at studying the
consequences of this update on the atmospheric compositions of (exo)planetary
atmospheres and brown dwarfs. We have performed an extensive review of
combustion experimental studies and revisited the sub-mechanism describing
methanol combustion in the scheme of Venot et al. (2012, A&A 624, A58). The
updated scheme involves 108 species linked by a total of 1906 reactions. We
have then applied our 1D kinetic model with this new scheme to several case
studies (HD 209458b, HD 189733b, GJ 436b, GJ 1214b, ULAS J1335+11, Uranus,
Neptune), and compared the results obtained with those obtained with the former
scheme. The update of the scheme has a negligible impact on hot Jupiters
atmospheres. However, the atmospheric composition of warm Neptunes and brown
dwarfs is modified sufficiently to impact observational spectra in the
wavelength range JWST will operate. Concerning Uranus and Neptune, the update
of the chemical scheme modifies the abundance of CO and thus impacts the deep
oxygen abundance required to reproduce the observational data. For future 3D
kinetics models, we also derived a reduced scheme containing 44 species and 582
reactions. Chemical schemes should be regularly updated in order to maintain a
high level of reliability on the results of kinetic models and be able to
improve our knowledge on planetary formation.
