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

M-stars comprise 80% of main-sequence stars, and so their planetary systemsprovide the best chance for finding habitable planets, i.e.: those with surfaceliquid water. We have modelled the broadband albedo or reflectivity of waterice and snow for simulated planetary surfaces orbiting two observed red dwarfstars (or M-stars) using spectrally resolved data of the Earth's cryosphere.The gradual reduction of the albedos of snow and ice at wavelengths greaterthan 1 ?m, combined with M-stars emitting a significant fraction of theirradiation at these same longer wavelengths, mean that the albedos of ice andsnow on planets orbiting M-stars are much lower than their values on Earth. Ourresults imply that the ice/snow albedo climate feedback is significantly weakerfor planets orbiting M-stars than for planets orbiting G-type stars such as theSun. In addition, planets with significant ice and snow cover will havesignificantly higher surface temperatures for a given stellar flux if thespectral variation of cryospheric albedo is considered, which in turn impliesthat the outer edge of the habitable zone around M-stars may be 10-30% furtheraway from the parent star than previously thought.

Suppression of the water ice and snow albedo feedback on planets orbiting red dwarf stars and the subsequent widening of the habitable zone