English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

The presence of titanium oxide (TiO) and vanadium oxide (VO) gas phasespecies is searched for in the atmosphere of the hot Jupiter HD209458b. Wecompared a model for the planets transmitted spectrum to multi-wavelengtheclipse-depth measurements (from 3000 to 10000 Angstrom), obtained by Sing etal. (2008a) using archived HST-STIS time series spectra. We make use of theseobservations to search for spectral signatures from extra absorbers in theplanet atmosphere between 6000 and 8000 Angstrom. Along with sodium depletionand Rayleigh scattering recently published for this exoplanet atmosphere, anextra absorber of uncertain origin, redward of the sodium lines, resides in theatmosphere of the planet. Furthermore, this planet has a stratosphereexperiencing a thermal inversion caused by the capture of optical stellar fluxby absorbers that resides at altitude. Recent models have predicted that thepresence of TiO and VO in the atmosphere of HD209458b may be responsible forthis temperature inversion. Although no specific TiO and VO spectral band headsignatures have been identified unambiguously in the observed spectrum, wesuggest here that the opacities of those molecules are possible candidates toexplain the remaining continuous broad band absorption observed between 6200and 8000 Angstrom. To match reasonably well the data, the abundances of TiO andVO molecules are evaluated from ten to one thousand times below solar. Thisupper limit result is in agreement with expected variations with altitude dueto depletion effects such as condensation.

TiO and VO broad band absorption features in the optical spectrum of the atmosphere of the hot-Jupiter HD209458b