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Title: Exoplanet Volatile Carbon Content as a Natural Pathway for Haze Formation
Abstract We explore terrestrial planet formation with a focus on the supply of solid-state organics as the main source of volatile carbon. For the water-poor Earth, the water ice line, or ice sublimation front, within the planet-forming disk has long been a key focal point. We posit that the soot line, the location where solid-state organics are irreversibly destroyed, is also a key location within the disk. The soot line is closer to the host star than the water snow line and overlaps with the location of the majority of detected exoplanets. In this work, we explore the ultimate atmospheric composition of a body that receives a major portion of its materials from the zone between the soot line and water ice line. We model a silicate-rich world with 0.1% and 1% carbon by mass with variable water content. We show that as a result of geochemical equilibrium, the mantle of these planets would be rich in reduced carbon but have relatively low water (hydrogen) content. Outgassing would naturally yield the ingredients for haze production when exposed to stellar UV photons in the upper atmosphere. Obscuring atmospheric hazes appear common in the exoplanetary inventory based on the presence of often featureless transmission spectra. Such hazes may be powered by the high volatile content of the underlying silicate-dominated mantle. Although this type of planet has no solar system counterpart, it should be common in the galaxy with potential impact on habitability.  more » « less
Award ID(s):
1931736 2009095
NSF-PAR ID:
10436111
Author(s) / Creator(s):
; ; ; ; ; ; ;
Publisher / Repository:
AAS Journals
Date Published:
Journal Name:
The Astrophysical Journal Letters
Volume:
949
Issue:
1
ISSN:
2041-8205
Page Range / eLocation ID:
L17
Format(s):
Medium: X
Sponsoring Org:
National Science Foundation
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