Podcasts about earth atmosphere

How do we predict our planet's most powerful forces? Neil deGrasse Tyson and comedian Chuck Nice learn about extreme weather, hurricanes, coronal mass ejections, and preparing for space storms hurtling our way with NOAA Administrator Richard Spinrad.NOTE: StarTalk+ Patrons can listen to this entire episode commercial-free.Thanks to our Patrons Dwight N Keown, Nathan Veatch, CURTIS J ESSEN, John Havranek, Vanessa Harding, Aiden Chauvette, Matthew Stork, SpaceTimePete, larry hughes, Anselmo Garcia, Nessa Nova, Tanya Henry, Neil Livingston, oliver stanton, Regis, Micheal Stewart, DP337, Rob Butler, Beth, and Caton Smith for supporting us this week. Subscribe to SiriusXM Podcasts+ on Apple Podcasts to listen to new episodes ad-free and a whole week early.

An experimental and theoretical investigation of HCN production in the Hadean Earth atmosphere by Ben K. D. Pearce et al. on Tuesday 20 September A critical early stage for the origin of life on Earth may have involved the production of hydrogen cyanide (HCN) in a reducing, predominantly H$_2$ atmosphere. HCN is crucial for the origin of life as it is a possible precursor to several biomolecules that make up RNA and proteins including nucleobases, nucleotides, amino acids, and ribose. In this work, we perform an in depth experimental and theoretical investigation of HCN production in reducing atmospheric conditions (89-95% H$_2$) possibly representing the earliest stages of the Hadean eon, ~4.5-4.3 billion years ago. We make use of cold plasma discharges - a laboratory analog to shortwave UV radiation - to simulate HCN production in the upper layers of the atmosphere for CH$_4$ abundances ranging from 0.1-6.5%. We then combine experimental mass spectrum measurements with our theoretical plasma models to estimate the HCN concentrations produced in our experiments. We find that upper atmospheric HCN production scales linearly with CH$_4$ abundance with the relation [HCN] = 0.13 $pm$ 0.01[CH$_4$]. Concentrations of HCN near the surface of the Hadean Earth are expected to be about 2-3 orders of magnitude lower. The addition of 1% water to our experiments results in a ~50% reduction in HCN production. We find that four reactions are primarily responsible for HCN production in our experiments: (i) $^4$N + CH$_3$ -> H$_2$CN + H -> HCN + H$_2$, (ii) $^4$N + CH -> CN + H followed by CN + CH$_4$ -> HCN + CH$_3$, (iii) C$_2$H$_4$ + $^4$N -> HCN + CH$_3$, and (iv) $^4$N + $^3$CH$_2$ -> HCN + H. The most prebiotically favorable Hadean atmosphere would have been very rich in CH$_4$ (> 5%), and as a result of greenhouse effects the surface would be likely very hot. In such a prebiotic scenario, it may have been important to incorporate HCN into organic hazes that could later release biomolecules and precursors into the first ponds. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.09257v1

An experimental and theoretical investigation of HCN production in the Hadean Earth atmosphere by Ben K. D. Pearce et al. on Tuesday 20 September A critical early stage for the origin of life on Earth may have involved the production of hydrogen cyanide (HCN) in a reducing, predominantly H$_2$ atmosphere. HCN is crucial for the origin of life as it is a possible precursor to several biomolecules that make up RNA and proteins including nucleobases, nucleotides, amino acids, and ribose. In this work, we perform an in depth experimental and theoretical investigation of HCN production in reducing atmospheric conditions (89-95% H$_2$) possibly representing the earliest stages of the Hadean eon, ~4.5-4.3 billion years ago. We make use of cold plasma discharges - a laboratory analog to shortwave UV radiation - to simulate HCN production in the upper layers of the atmosphere for CH$_4$ abundances ranging from 0.1-6.5%. We then combine experimental mass spectrum measurements with our theoretical plasma models to estimate the HCN concentrations produced in our experiments. We find that upper atmospheric HCN production scales linearly with CH$_4$ abundance with the relation [HCN] = 0.13 $pm$ 0.01[CH$_4$]. Concentrations of HCN near the surface of the Hadean Earth are expected to be about 2-3 orders of magnitude lower. The addition of 1% water to our experiments results in a ~50% reduction in HCN production. We find that four reactions are primarily responsible for HCN production in our experiments: (i) $^4$N + CH$_3$ -> H$_2$CN + H -> HCN + H$_2$, (ii) $^4$N + CH -> CN + H followed by CN + CH$_4$ -> HCN + CH$_3$, (iii) C$_2$H$_4$ + $^4$N -> HCN + CH$_3$, and (iv) $^4$N + $^3$CH$_2$ -> HCN + H. The most prebiotically favorable Hadean atmosphere would have been very rich in CH$_4$ (> 5%), and as a result of greenhouse effects the surface would be likely very hot. In such a prebiotic scenario, it may have been important to incorporate HCN into organic hazes that could later release biomolecules and precursors into the first ponds. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.09257v1

Two climate engineering technologies have been inscribed into the Intergovernmental Panel on Climate Change's Fifth Assessment Report outlining they'll be crucial in ensuring we don't exceed 2 degrees of global warming. However, with little evidence as to how these technologies work in the field, is this just another attempt to stall more proactive climate action?Featuring:Jonathan Marshall - Future Fellow in the Faculty of Arts and Social Sciences at the University of Technology Sydney. Kerryn Brent - Law Lecturer at the University of Tasmania. Steven Siems - Professor in the School of Earth Atmosphere and Environment at Monash University.

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