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 Tools annual

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 monthly

Global: Zendy Plus monthly

Presents the access of premium content as premium feature

Premium Content

Global: Zendy Plus annual

Global: Zendy Free Plan

The water ice or snow line is one of the key properties of protoplanetarydisks that determines the water content of terrestrial planets in the habitablezone. Its location is determined by the properties of the star, the massaccretion rate through the disk, and the size distribution of dust suspended inthe disk. We calculate the snow line location from recent observations of massaccretion rates and as a function of stellar mass. By taking the observeddispersion in mass accretion rates as a measure of the dispersion in initialdisk mass, we find that stars of a given mass will exhibit a range of snow linelocations. At a given age and stellar mass, the observed dispersion in massaccretion rates of 0.4 dex naturally leads to a dispersion in snow linelocations of 0.2 dex. For ISM-like dust sizes, the one-sigma snow line locationamong solar mass stars of the same age ranges from 2 to 5 au. For morerealistic dust opacities that include larger grains, the snow line is locatedup to two times closer to the star. We use these locations and the outcome ofN-body simulations to predict the amount of water delivered to terrestrialplanets that formed in situ in the habitable zone. We find that the dispersionin snow line locations leads to a large range in water content. For ISM-likedust sizes, a significant fraction of habitable-zone terrestrial planets aroundsun-like stars remain dry, and no water is delivered to the habitable zones oflow-mass M stars (less than half a solar mass) as in previous works. Thecloser-in snow line in disks with larger grains enables water delivery to thehabitable zone for a significant fraction of M stars and all FGK stars.Considering their larger numbers and higher planet occurrence, M stars may hostmost of the water-rich terrestrial planets in the galaxy if these planets areable to hold on to their water in their subsequent evolution.

The snow line in viscous disks around low-mass stars: implications for water delivery to terrestrial planets in the habitable zone