Reduction in haze formation rate on prebiotic Earth in the presence of hydrogen.
Recent attempts to resolve the faint young Sun paradox have focused on an early Earth atmosphere with elevated levels of the greenhouse gases methane (CH(4)) and carbon dioxide (CO(2)) that could have provided adequate warming to Earth's surface. On Titan, the photolysis of CH(4) has been shown to create a thick haze layer that cools its surface. Unlike Titan, however, early Earth's atmosphere likely contained high amounts of CO(2) and hydrogen (H(2)). In this work, we examine haze formation in an early Earth atmosphere composed of CO(2), H(2), N(2), and CH(4), with a CO(2)/CH(4) ratio of 10 and a H(2)/CO(2) ratio of up to 15. To initiate aerosol formation, a broad-spectrum ultraviolet (UV) energy source with emission at Lyman-alpha was used to simulate the solar spectrum. Aerosol composition and total aerosol mass produced as a function of reagent gas were measured with an aerosol mass spectrometer (AMS). Results show an order of magnitude decrease in haze production with the addition of H(2), with no significant change in the chemical composition of the haze. We calculate that the presence of H(2) on early Earth could thus have favored warmer surface temperatures and yet allowed photochemical haze formation to deliver complex organic species to early Earth's surface.
DeWitt
H Langley
HL
Department of Chemistry and Biochemistry, University of Colorado, Boulder, Colorado, USA.
Trainer
Melissa G
MG
Pavlov
Alex A
AA
Hasenkopf
Christa A
CA
Aiken
Allison C
AC
Jimenez
Jose L
JL
McKay
Christopher P
CP
Toon
Owen B
OB
Tolbert
Margaret A
MA
D000336:Aerosols / Q000737:chemistry*; D003198:Computer Simulation; D018534:Earth, Planet; D006859:Hydrogen / Q000737:chemistry*; D013058:Mass Spectrometry; D008970:Molecular Weight; D052638:Particulate Matter; D010782:Photolysis; D013499:Surface Properties; D013696:Temperature
D000336:Aerosols; D052638:Particulate Matter; D006859:Hydrogen