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

Protoplanets growing within the protoplanetary disk by pebble accretionacquire hydrostatic gas envelopes. Due to accretion heating, the temperature inthese envelopes can become high enough to sublimate refractory minerals whichare the major components of the accreted pebbles. Here we study the sublimationof different mineral species and determine whether sublimation plays a roleduring the growth by pebble accretion. For each snapshot in the growth process,we calculate the envelope structure and sublimation temperature of a set ofmineral species representing different levels of volatility. Sublimation linesare determined using and equilibrium scheme for the chemical reactionsresponsible for destruction and formation of the relevant minerals. We findthat the envelope of the growing planet reaches temperatures high enough tosublimate all considered mineral species when the mass is larger than 0.4 Earthmasses. The sublimation lines are located within the gravitionally boundenvelope of the planet. We make a detailed analysis of the sublimation of FeSat around 720 K, beyond which the mineral is attacked by H2 to form gaseous H2Sand solid Fe. We calculate the sulfur concentration in the planet under theassumption that all sulfur released as H2S is lost from the planet by diffusionback to the protoplanetary disk. Our calculated values are in good agreementwith the slightly depleted sulfur abundance of Mars, while the modeloverpredicts the extensive sulfur depletion of Earth by a factor ofapproximately 2. We show that a collision with a sulfur-rich body akin to Marsin the moon-forming impact lifts the Earth's sulfur abundance to approximately10% of the solar value for all impactor masses above 0.05 Earth masses.

Sublimation of refractory minerals in the gas envelopes of accreting rocky planets