Atmospherics

@article{wormell1948atmospherics,
    author = "Wormell, T.W. and Pierce, E.T.",
    title = "Atmospherics",
    year = "1948",
    journal = "Journal of the Institution of Electrical Engineers - Part III: Radio and Communication Engineering",
    url = "https://doi.org/10.1049/ji-3-2.1948.0078",
    doi = "10.1049/ji-3-2.1948.0078",
    number = "37",
    pages = "331-332",
    volume = "95"
}

@book{brown1949rare4,
    author = "Brown, H",
    title = "Rare Gases and the Formation of the Earth's Atmosphere, in Kuiper, G. P., ed., The Atmospheres of the Earth and Planets",
    year = "1949",
    publisher = "Chicago, Ill., University of Chicago Press",
    note = "talkorigins\_source = {true}; raw\_reference = {Brown, H., 1949, Rare Gases and the Formation of the Earth's Atmosphere, in Kuiper, G. P., ed., The Atmospheres of the Earth and Planets: Chicago, Ill., University of Chicago Press.}"
}

@book{kuiper1949the8,
    author = "Kuiper, G. P",
    title = "The Atmospheres of the Earth and Planets",
    year = "1949",
    publisher = "Chicago, Ill., University of Chicago Press",
    note = "talkorigins\_source = {true}; raw\_reference = {Kuiper, G. P., 1949, The Atmospheres of the Earth and Planets: Chicago, Ill., University of Chicago Press.}"
}

@book{byers1954the5,
    author = "Byers, H. G",
    title = "The atmosphere up to 30 kilometers, in Kuiper, G. P., ed., The Earth as a Planet",
    year = "1954",
    publisher = "Chicago, University of Chicago Press",
    note = "talkorigins\_source = {true}; raw\_reference = {Byers, H. G., 1954, The atmosphere up to 30 kilometers, in Kuiper, G. P., ed., The Earth as a Planet: Chicago, University of Chicago Press.}"
}

@book{berkner1964in2,
    author = "Berkner, L. V. and Marshall, L. C",
    title = "in Brancazio, P. J., and Cameron, A. G. W., eds., The Origin and Evolution of the Atmosphere and Oceans",
    year = "1964",
    publisher = "New York, John Wiley and Sons, p. 102-126",
    note = "talkorigins\_source = {true}; raw\_reference = {Berkner, L. V., and Marshall, L. C., 1964,, in Brancazio, P. J., and Cameron, A. G. W., eds., The Origin and Evolution of the Atmosphere and Oceans: New York, John Wiley and Sons, p. 102-126.}"
}

@inproceedings{brekner1965history3,
    author = "Brekner, L. V. and Marshall, L. C",
    title = "History of the Major Atmospheric Components, in Symposium on the Evolution of the Earth's Atmosphere",
    year = "1965",
    booktitle = "v. 53, No.6, p. 1215-1226; Proceedings of the National Academy of Sciences",
    note = "talkorigins\_source = {true}; raw\_reference = {Brekner, L. V., and Marshall, L. C., 1965, History of the Major Atmospheric Components, in Symposium on the Evolution of the Earth's Atmosphere: v. 53, No.6, p. 1215-1226; Proceedings of the National Academy of Sciences.}"
}

@misc{connes1967traces7,
    author = "Connes, P. and Connes, J. and Benedict, W. S. and Kaplan, L. D",
    title = "Traces of HCl and HF in the Atmosphere of Venus",
    year = "1967",
    howpublished = "Ap. J., v. 147, p. 1230",
    note = "talkorigins\_source = {true}; raw\_reference = {Connes, P., Connes, J., Benedict, W. S., and Kaplan, L. D., 1967, Traces of HCl and HF in the Atmosphere of Venus: Ap. J., v. 147, p. 1230.}"
}

@book{openalexw1667069063,
    author = "Safronov, Viktor Sergeevich",
    title = "Evolution of the protoplanetary cloud and formation of the earth and the planets",
    year = "1972",
    journal = "Medical Entomology and Zoology",
    openalex = "W1667069063"
}

@misc{ruderman1974possible10,
    author = "Ruderman, M. A",
    title = "Possible consequences of nearby supernova explosions for atmospheric ozone and terrestrial life",
    year = "1974",
    howpublished = "Science, v. 184, p. 1079-1081",
    note = "talkorigins\_source = {true}; raw\_reference = {Ruderman, M. A., 1974, Possible consequences of nearby supernova explosions for atmospheric ozone and terrestrial life: Science, v. 184, p. 1079-1081.}"
}

@misc{ninkovich1976explosive9,
    author = "Ninkovich, D. and Donn, W. L",
    title = "Explosive Cenozoic volcanism and climatic implications",
    year = "1976",
    howpublished = "Science, v. 194, p. 899-906",
    note = "talkorigins\_source = {true}; raw\_reference = {Ninkovich, D., and Donn, W. L., 1976, Explosive Cenozoic volcanism and climatic implications: Science, v. 194, p. 899-906.}"
}

@misc{walker1977evolution11,
    author = "Walker, J. C. G",
    title = "Evolution of the Atmosphere",
    year = "1977",
    howpublished = "New York, Macmillan",
    note = "talkorigins\_source = {true}; raw\_reference = {Walker, J. C. G., 1977, Evolution of the Atmosphere: New York, Macmillan.}"
}

@article{doi1010160019103581901019,
    author = "Watson, Andrew and Donahue, T. M. and Walker, James C. G.",
    title = "The dynamics of a rapidly escaping atmosphere: Applications to the evolution of Earth and Venus",
    year = "1981",
    journal = "Icarus",
    url = "https://doi.org/10.1016/0019-1035(81)90101-9",
    doi = "10.1016/0019-1035(81)90101-9",
    openalex = "W2106231443"
}

Combined inferences from seismology, high-pressure experiment and theory, geomagnetism, fluid dynamics, and current views of terrestrial planetary evolution lead to models of the earth's core with the following properties. Core formation was contemporaneous with earth accretion; the core is not in chemical equilibrium with the mantle; the outer core is a fluid iron alloy containing significant quantities of lighter elements and is probably almost adiabatic and compositionally uniform; the more iron-rich inner solid core is a consequence of partial freezing of the outer core, and the energy release from this process sustains the earth's magnetic field; and the thermodynamic properties of the core are well constrained by the application of liquid-state theory to seismic and laboratory data.

@article{doi101126science2144521611,
    author = "Stevenson, D. J.",
    title = "Models of the Earth's Core",
    year = "1981",
    journal = "Science",
    abstract = "Combined inferences from seismology, high-pressure experiment and theory, geomagnetism, fluid dynamics, and current views of terrestrial planetary evolution lead to models of the earth's core with the following properties. Core formation was contemporaneous with earth accretion; the core is not in chemical equilibrium with the mantle; the outer core is a fluid iron alloy containing significant quantities of lighter elements and is probably almost adiabatic and compositionally uniform; the more iron-rich inner solid core is a consequence of partial freezing of the outer core, and the energy release from this process sustains the earth's magnetic field; and the thermodynamic properties of the core are well constrained by the application of liquid-state theory to seismic and laboratory data.",
    url = "https://doi.org/10.1126/science.214.4521.611",
    doi = "10.1126/science.214.4521.611",
    openalex = "W2074267811"
}

@misc{austin1982did1,
    author = "Austin, S. A",
    title = "Did the Earth have a reducing atmosphere?",
    year = "1982",
    howpublished = "ICR Impact Series, no. 109, p. i-iv",
    note = "talkorigins\_source = {true}; raw\_reference = {Austin, S. A., 1982, Did the Earth have a reducing atmosphere?: ICR Impact Series, no. 109, p. i-iv.}"
}

@article{clemmey1982oxygen6,
    author = "Clemmey, H. and Badham, N",
    title = "Oxygen in the Precambrian atmosphere",
    year = "1982",
    journal = "an evaluation of the geologic evidence: The Geographical Review, v. 10, p. 141-146",
    note = "talkorigins\_source = {true}; raw\_reference = {Clemmey, H., and Badham, N., 1982, Oxygen in the Precambrian atmosphere: an evaluation of the geologic evidence: The Geographical Review, v. 10, p. 141-146.}"
}

@article{doi1010160019103582900793,
    author = "Pollack, James B. and Black, David C.",
    title = "Noble gases in planetary atmospheres: Implications for the origin and evolution of atmospheres",
    year = "1982",
    journal = "Icarus",
    url = "https://doi.org/10.1016/0019-1035(82)90079-3",
    doi = "10.1016/0019-1035(82)90079-3",
    openalex = "W2044634350"
}

In this first full-scale attempt to reconstruct the chemical evolution of the Earth's atmosphere and oceans, Heinrich Holland assembles data from a wide spectrum of fields to trace the history of the ocean-atmosphere system. A pioneer in an increasingly important area of scholarship, he presents a comprehensive treatment of knowledge on this subject, provides an extensive bibliography, and outlines problems and approaches for further research. The first four chapters deal with the turbulent first half billion years of Earth history. The next four chapters, devoted largely to the Earth from 3.9 to 0.6 b.y.b.p., demonstrate that changes in the atmosphere and oceans during this period were not dramatic. The last chapter of the book deals with the Phanerozoic Eon; although the isotopic composition of sulfur and strontium in seawater varied greatly during this period of Earth history, the chemical composition of seawater did not.

@book{doi1015159780691220239,
    author = "Holland, Heinrich",
    title = "The Chemical Evolution of the Atmosphere and Oceans",
    year = "1984",
    booktitle = "Princeton University Press eBooks",
    abstract = "In this first full-scale attempt to reconstruct the chemical evolution of the Earth's atmosphere and oceans, Heinrich Holland assembles data from a wide spectrum of fields to trace the history of the ocean-atmosphere system. A pioneer in an increasingly important area of scholarship, he presents a comprehensive treatment of knowledge on this subject, provides an extensive bibliography, and outlines problems and approaches for further research. The first four chapters deal with the turbulent first half billion years of Earth history. The next four chapters, devoted largely to the Earth from 3.9 to 0.6 b.y.b.p., demonstrate that changes in the atmosphere and oceans during this period were not dramatic. The last chapter of the book deals with the Phanerozoic Eon; although the isotopic composition of sulfur and strontium in seawater varied greatly during this period of Earth history, the chemical composition of seawater did not.",
    url = "https://doi.org/10.1515/9780691220239",
    doi = "10.1515/9780691220239",
    openalex = "W1638884317"
}

@article{doi1010160019103588900310,
    author = "Zahnle, Kevin and Kasting, James F. and Pollack, James B.",
    title = "Evolution of a steam atmosphere during earth's accretion",
    year = "1988",
    journal = "Icarus",
    url = "https://doi.org/10.1016/0019-1035(88)90031-0",
    doi = "10.1016/0019-1035(88)90031-0",
    openalex = "W1998781690",
    references = "doi1010079781461261674, doi101007bf00151270, doi1010160019103581901019, doi1010160019103583900325, doi1010160019103583902415, doi1010160019103585901460, doi1010160019103587901047, doi1010160019103588901169, doi101126science2144521611, openalexw1667069063, openalexw2341059552"
}

@article{doi1010160019103588901169,
    author = "Kasting, James F.",
    title = "Runaway and moist greenhouse atmospheres and the evolution of Earth and Venus",
    year = "1988",
    journal = "Icarus",
    url = "https://doi.org/10.1016/0019-1035(88)90116-9",
    doi = "10.1016/0019-1035(88)90116-9",
    openalex = "W1968152463",
    references = "doi1010160019103578900210, doi1010160019103588900310"
}

@article{crossref1989atmospherics,
    title = "Atmospherics",
    year = "1989",
    journal = "Europhysics News",
    url = "https://doi.org/10.1051/epn/19892010154b",
    doi = "10.1051/epn/19892010154b",
    number = "10",
    pages = "154-154",
    volume = "20"
}

@article{doi101016001910359190036s,
    author = "Pepin, Robert O.",
    title = "On the origin and early evolution of terrestrial planet atmospheres and meteoritic volatiles",
    year = "1991",
    journal = "Icarus",
    url = "https://doi.org/10.1016/0019-1035(91)90036-s",
    doi = "10.1016/0019-1035(91)90036-s",
    openalex = "W2044377375",
    references = "doi1010160019103583900325, doi1010160032063363901132, doi101029jb087ib07p05611, doi101038338487a0, doi101126science2214611651"
}

The competition between impact erosion and impact supply of volatiles to planetary atmospheres can determine whether a planet or satellite accumulates an atmosphere. In the absence of other processes (e.g., outgassing), we find either that a planetary atmosphere should be thick, or that there should be no atmosphere at all. The boundary between the two extreme cases is set by the mass and velocity distributions and intrinsic volatile content of the impactors. We apply our model specifically to Titan, Callisto, and Ganymede. The impacting population is identified with comets, either in the form of stray Uranus-Neptune planetesimals or as dislodged Kuiper belt comets. Systematically lower impact velocities on Titan allow it to retain a thick atmosphere, while Callisto and Ganymede get nothing. Titan's atmosphere may therefore be an expression of a late-accreting, volatile-rich veneer. An impact origin for Titan's atmosphere naturally accounts for the high D/H ratio it shares with Earth, the carbonaceous meteorites, and Halley. It also accounts for the general similarity of Titan's atmosphere to those of Triton and Pluto, which is otherwise puzzling in view of the radically different histories and bulk compositions of these objects.

@article{doi101016001910359290187c,
    author = "Zahnle, K and Pollack, J B and Grinspoon, D and Dones, L",
    title = "Impact-generated atmospheres over Titan, Ganymede, and Callisto.",
    year = "1992",
    journal = "Icarus",
    abstract = "The competition between impact erosion and impact supply of volatiles to planetary atmospheres can determine whether a planet or satellite accumulates an atmosphere. In the absence of other processes (e.g., outgassing), we find either that a planetary atmosphere should be thick, or that there should be no atmosphere at all. The boundary between the two extreme cases is set by the mass and velocity distributions and intrinsic volatile content of the impactors. We apply our model specifically to Titan, Callisto, and Ganymede. The impacting population is identified with comets, either in the form of stray Uranus-Neptune planetesimals or as dislodged Kuiper belt comets. Systematically lower impact velocities on Titan allow it to retain a thick atmosphere, while Callisto and Ganymede get nothing. Titan's atmosphere may therefore be an expression of a late-accreting, volatile-rich veneer. An impact origin for Titan's atmosphere naturally accounts for the high D/H ratio it shares with Earth, the carbonaceous meteorites, and Halley. It also accounts for the general similarity of Titan's atmosphere to those of Triton and Pluto, which is otherwise puzzling in view of the radically different histories and bulk compositions of these objects.",
    url = "https://pubmed.ncbi.nlm.nih.gov/11538396/",
    doi = "10.1016/0019-1035(92)90187-c",
    openalex = "W2080496895",
    pmid = "11538396",
    references = "doi101016001670378990286x, doi1010160019103583900325, doi1010160019103588900310, doi1010160022286070900190, doi1010160734743x87900698, doi101038338487a0, doi101038343129a0, doi101126science11538074, doi101130spe190, doi102307jctv1v3gr3r6"
}

Ideas about atmospheric composition and climate on the early Earth have evolved considerably over the last 30 years, but many uncertainties still remain. It is generally agreed that the atmosphere contained little or no free oxygen initially and that oxygen concentrations increased markedly near 2.0 billion years ago, but the precise timing of and reasons for its rise remain unexplained. Likewise, it is usually conceded that the atmospheric greenhouse effect must have been higher in the past to offset reduced solar luminosity, but the levels of atmospheric carbon dioxide and other greenhouse gases required remain speculative. A better understanding of past atmospheric evolution is important to understanding the evolution of life and to predicting whether Earth-like planets might exist elsewhere in the galaxy.

@article{doi101126science11536547,
    author = "Kasting, James F.",
    title = "Earth's Early Atmosphere",
    year = "1993",
    journal = "Science",
    abstract = "Ideas about atmospheric composition and climate on the early Earth have evolved considerably over the last 30 years, but many uncertainties still remain. It is generally agreed that the atmosphere contained little or no free oxygen initially and that oxygen concentrations increased markedly near 2.0 billion years ago, but the precise timing of and reasons for its rise remain unexplained. Likewise, it is usually conceded that the atmospheric greenhouse effect must have been higher in the past to offset reduced solar luminosity, but the levels of atmospheric carbon dioxide and other greenhouse gases required remain speculative. A better understanding of past atmospheric evolution is important to understanding the evolution of life and to predicting whether Earth-like planets might exist elsewhere in the galaxy.",
    url = "https://doi.org/10.1126/science.11536547",
    doi = "10.1126/science.11536547",
    openalex = "W2001363398",
    references = "doi101006icar19931010, doi101007bf00151270, doi101016001670379290064p, doi1010160019103588900310, doi101029gm032, doi101029jc086ic10p09776, doi101038321832a0, doi101038331612a0, doi101038342139a0, doi101038343129a0, doi101111j150239311988tb02083x, doi101126science11536492, doi101126science11538074, doi101126science1173046528, doi101126science1303370245, doi101126science1585174, doi101126science1631544, doi101126science177404352, doi101130001676061951621111ghosw20co2, doi1015159780691220239, doi102475ajs2837641, miller1953a, openalexw2026796374"
}

@incollection{crossref1999atmospherics,
    title = "Atmospherics",
    year = "1999",
    booktitle = "Shakespeare: The Comedies",
    url = "https://doi.org/10.5040/9781350391055.ch-001",
    doi = "10.5040/9781350391055.ch-001"
}

We present our NextGen Model Atmosphere grid for low-mass stars for effective temperatures larger than 3000 K. These LTE models are calculated with the same basic model assumptions and input physics as the VLMS part of the NextGen grid so that the complete grid can be used, e.g., for consistent stellar evolution calculations and for internally consistent analysis of cool star spectra. This grid is also the starting point for a large grid of detailed NLTE model atmospheres for dwarfs and giants. The models were calculated from 3000 to 10,000 K (in steps of 200 K) for 3.5 ≤ log g ≤ 5.5 (in steps of 0.5) and metallicities of -4.0 ≤ [M/H] ≤ 0.0.

@article{doi101086306745,
    author = "Hauschildt, P. H. and Allard, F. and Baron, E.",
    title = "The NextGen Model Atmosphere Grid for \documentclass{aastex} \usepackage{amsbsy} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{bm} \usepackage{mathrsfs} \usepackage{pifont} \usepackage{stmaryrd} \usepackage{textcomp} \usepackage{portland,xspace} \usepackage{amsmath,amsxtra} \usepackage[OT2,OT1]{fontenc} \newcommand\cyr{\renewcommand\rmdefault{wncyr} \renewcommand\sfdefault{wncyss} \renewcommand\encodingdefault{OT2} \normalfont \selectfont} \DeclareTextFontCommand{\textcyr}{\cyr} \pagestyle{empty} \DeclareMathSizes{10}{9}{7}{6} \begin{document} \landscape $3000\leq T\_{\mathrm{eff}\,}\leq \mathrm{10,000}\,$ \end{document} K",
    year = "1999",
    journal = "The Astrophysical Journal",
    abstract = "We present our NextGen Model Atmosphere grid for low-mass stars for effective temperatures larger than 3000 K. These LTE models are calculated with the same basic model assumptions and input physics as the VLMS part of the NextGen grid so that the complete grid can be used, e.g., for consistent stellar evolution calculations and for internally consistent analysis of cool star spectra. This grid is also the starting point for a large grid of detailed NLTE model atmospheres for dwarfs and giants. The models were calculated from 3000 to 10,000 K (in steps of 200 K) for 3.5 ≤ log g ≤ 5.5 (in steps of 0.5) and metallicities of -4.0 ≤ [M/H] ≤ 0.0.",
    url = "https://doi.org/10.1086/306745",
    doi = "10.1086/306745",
    openalex = "W4292406868"
}

Abstract— In the primordial solar system, the most plausible sources of the water accreted by the Earth were in the outer asteroid belt, in the giant planet regions, and in the Kuiper Belt. We investigate the implications on the origin of Earth's water of dynamical models of primordial evolution of solar system bodies and check them with respect to chemical constraints. We find that it is plausible that the Earth accreted water all along its formation, from the early phases when the solar nebula was still present to the late stages of gas‐free sweepup of scattered planetesimals. Asteroids and the comets from the Jupiter‐Saturn region were the first water deliverers, when the Earth was less than half its present mass. The bulk of the water presently on Earth was carried by a few planetary embryos, originally formed in the outer asteroid belt and accreted by the Earth at the final stage of its formation. Finally, a late veneer, accounting for at most 10% of the present water mass, occurred due to comets from the Uranus‐Neptune region and from the Kuiper Belt. The net result of accretion from these several reservoirs is that the water on Earth had essentially the D/H ratio typical of the water condensed in the outer asteroid belt. This is in agreement with the observation that the D/H ratio in the oceans is very close to the mean value of the D/H ratio of the water inclusions in carbonaceous chondrites.

@article{doi101111j194551002000tb01518x,
    author = "Morbidelli, Alessandro and Chambers, John and Lunine, J. I. and Petit, Jean-Marc and Robert, F. and Valsecchi, G. B. and Cyr, K. E.",
    title = "Source regions and timescales for the delivery of water to the Earth",
    year = "2000",
    journal = "Meteoritics and Planetary Science",
    abstract = "Abstract— In the primordial solar system, the most plausible sources of the water accreted by the Earth were in the outer asteroid belt, in the giant planet regions, and in the Kuiper Belt. We investigate the implications on the origin of Earth's water of dynamical models of primordial evolution of solar system bodies and check them with respect to chemical constraints. We find that it is plausible that the Earth accreted water all along its formation, from the early phases when the solar nebula was still present to the late stages of gas‐free sweepup of scattered planetesimals. Asteroids and the comets from the Jupiter‐Saturn region were the first water deliverers, when the Earth was less than half its present mass. The bulk of the water presently on Earth was carried by a few planetary embryos, originally formed in the outer asteroid belt and accreted by the Earth at the final stage of its formation. Finally, a late veneer, accounting for at most 10\% of the present water mass, occurred due to comets from the Uranus‐Neptune region and from the Kuiper Belt. The net result of accretion from these several reservoirs is that the water on Earth had essentially the D/H ratio typical of the water condensed in the outer asteroid belt. This is in agreement with the observation that the D/H ratio in the oceans is very close to the mean value of the D/H ratio of the water inclusions in carbonaceous chondrites.",
    url = "https://doi.org/10.1111/j.1945-5100.2000.tb01518.x",
    doi = "10.1111/j.1945-5100.2000.tb01518.x",
    openalex = "W2014359877",
    references = "doi101006icar19941039, doi101006icar19960190, doi101006icar19986007, doi101006icar19996299, doi1010079781461261674, doi101007bf00642464, doi1010160019103588900310, doi101016001910359190036s, doi101017cbo9780511545986, doi101126science25550501391, doi101126science27653191670"
}

▪ Abstract Our understanding of the evolution of organic molecules, and their voyage from molecular clouds to the early solar system and Earth, has changed dramatically. Incorporating recent observational results from the ground and space, as well as laboratory simulation experiments and new methods for theoretical modeling, this review recapitulates the inventory and distribution of organic molecules in different environments. The evolution, survival, transport, and transformation of organics is monitored, from molecular clouds and the diffuse interstellar medium to their incorporation into solar system material such as comets and meteorites. We constrain gas phase and grain surface formation pathways to organic molecules in dense interstellar clouds, using recent observations with the Infrared Space Observatory (ISO) and ground-based radiotelescopes. The main spectroscopic evidence for carbonaceous compounds in the diffuse interstellar medium is discussed (UV bump at 2200 Å, diffuse interstellar bands, extended red emission, and infrared absorption and emission bands). We critically review the signatures and unsolved problemsrelated to the main organic components suggested to be present in the diffuse gas, such as polycyclic aromatic hydrocarbons (PAHs), fullerenes, diamonds, and carbonaceous solids. We also briefly discuss the circumstellar formation of organics around late-typestars. In the solar system, space missions to comet Halley and observations of the bright comets Hyakutake and Hale-Bopp have recently allowed a reexamination of the organic chemistry of dust and volatiles in long-period comets. We review the advances in this area and also discuss progress being made in elucidating the complex organic inventory of carbonaceous meteorites. The knowledge of organic chemistry in molecular clouds, comets, and meteorites and their common link provides constraints for the processes that lead to the origin, evolution, and distribution of life in the Galaxy.

@article{doi101146annurevastro381427,
    author = "Ehrenfreund, P. and Charnley, Steven B.",
    title = "Organic Molecules in the Interstellar Medium, Comets, and Meteorites: A Voyage from Dark Clouds to the Early Earth",
    year = "2000",
    journal = "Annual Review of Astronomy and Astrophysics",
    abstract = "▪ Abstract Our understanding of the evolution of organic molecules, and their voyage from molecular clouds to the early solar system and Earth, has changed dramatically. Incorporating recent observational results from the ground and space, as well as laboratory simulation experiments and new methods for theoretical modeling, this review recapitulates the inventory and distribution of organic molecules in different environments. The evolution, survival, transport, and transformation of organics is monitored, from molecular clouds and the diffuse interstellar medium to their incorporation into solar system material such as comets and meteorites. We constrain gas phase and grain surface formation pathways to organic molecules in dense interstellar clouds, using recent observations with the Infrared Space Observatory (ISO) and ground-based radiotelescopes. The main spectroscopic evidence for carbonaceous compounds in the diffuse interstellar medium is discussed (UV bump at 2200 Å, diffuse interstellar bands, extended red emission, and infrared absorption and emission bands). We critically review the signatures and unsolved problemsrelated to the main organic components suggested to be present in the diffuse gas, such as polycyclic aromatic hydrocarbons (PAHs), fullerenes, diamonds, and carbonaceous solids. We also briefly discuss the circumstellar formation of organics around late-typestars. In the solar system, space missions to comet Halley and observations of the bright comets Hyakutake and Hale-Bopp have recently allowed a reexamination of the organic chemistry of dust and volatiles in long-period comets. We review the advances in this area and also discuss progress being made in elucidating the complex organic inventory of carbonaceous meteorites. The knowledge of organic chemistry in molecular clouds, comets, and meteorites and their common link provides constraints for the processes that lead to the origin, evolution, and distribution of life in the Galaxy.",
    url = "https://doi.org/10.1146/annurev.astro.38.1.427",
    doi = "10.1146/annurev.astro.38.1.427",
    openalex = "W2148340339",
    references = "doi101006icar19996299, doi101038318162a0, doi101038347354a0, doi101038355125a0, doi101038359707a0, doi101086155591, doi101126science11538074, doi101126science2735277924, doi101146annurevaa09090171000245, doi101146annurevaa28090190000345, doi105860choice312093"
}

Laboratory experiments on the trapping of gases by ice forming at low temperatures implicate comets as major carriers of the heavy noble gases to the inner planets. These icy planetesimals may also have brought the nitrogen compounds that ultimately produced atmospheric N2. However, if the sample of three comets analyzed so far is typical, the Earth's oceans cannot have been produced by comets alone, they require an additional source of water with low D/H. The highly fractionated neon in the Earth's atmosphere may also indicate the importance of non-icy carriers of volatiles. The most important additional carrier is probably the rocky material comprising the bulk of the mass of these planets. Venus may require a contribution from icy planetesimals formed at the low temperatures characteristic of the Kuiper Belt.

@article{doi101023a1011809412925,
    author = "Owen, T C and Bar-Nun, A",
    title = "Contributions of icy planetesimals to the Earth's early atmosphere.",
    year = "2001",
    journal = "Origins of life and evolution of the biosphere: the journal of the International Society for the Study of the Origin of Life",
    abstract = "Laboratory experiments on the trapping of gases by ice forming at low temperatures implicate comets as major carriers of the heavy noble gases to the inner planets. These icy planetesimals may also have brought the nitrogen compounds that ultimately produced atmospheric N2. However, if the sample of three comets analyzed so far is typical, the Earth's oceans cannot have been produced by comets alone, they require an additional source of water with low D/H. The highly fractionated neon in the Earth's atmosphere may also indicate the importance of non-icy carriers of volatiles. The most important additional carrier is probably the rocky material comprising the bulk of the mass of these planets. Venus may require a contribution from icy planetesimals formed at the low temperatures characteristic of the Kuiper Belt.",
    url = "https://pubmed.ncbi.nlm.nih.gov/11599179/",
    doi = "10.1023/a:1011809412925",
    openalex = "W2257792074",
    pmid = "11599179",
    references = "doi101006icar19951190, doi1010160012821x76901187, doi101016001670378990286x, doi101016001910359190036s, doi101029js082i028p04341, doi101029js082i028p04635, doi101038190389a0, doi101111j194551001994tb01092x, doi101126science27553081904, doi101146annurevaa32090194001203"
}

Although biomarker, trace element, and isotopic evidence have been used to claim that oxygenic photosynthesis evolved by 2.8 giga-annum before present (Ga) and perhaps as early as 3.7 Ga, a skeptical examination raises considerable doubt about the presence of oxygen producers at these times. Geological features suggestive of oxygen, such as red beds, lateritic paleosols, and the return of sedimentary sulfate deposits after a approximately 900-million year hiatus, occur shortly before the approximately 2.3-2.2 Ga Makganyene "snowball Earth" (global glaciation). The massive deposition of Mn, which has a high redox potential, practically requires the presence of environmental oxygen after the snowball. New age constraints from the Transvaal Supergroup of South Africa suggest that all three glaciations in the Huronian Supergroup of Canada predate the Snowball event. A simple cyanobacterial growth model incorporating the range of C, Fe, and P fluxes expected during a partial glaciation in an anoxic world with high-Fe oceans indicates that oxygenic photosynthesis could have destroyed a methane greenhouse and triggered a snowball event on time-scales as short as 1 million years. As the geological evidence requiring oxygen does not appear during the Pongola glaciation at 2.9 Ga or during the Huronian glaciations, we argue that oxygenic cyanobacteria evolved and radiated shortly before the Makganyene snowball.

@article{doi101073pnas0504878102,
    author = "Kopp, Robert E. and Kirschvink, Joseph L. and Hilburn, Isaac A. and Nash, Cody Z.",
    title = "The Paleoproterozoic snowball Earth: A climate disaster triggered by the evolution of oxygenic photosynthesis",
    year = "2005",
    journal = "Proceedings of the National Academy of Sciences",
    abstract = {Although biomarker, trace element, and isotopic evidence have been used to claim that oxygenic photosynthesis evolved by 2.8 giga-annum before present (Ga) and perhaps as early as 3.7 Ga, a skeptical examination raises considerable doubt about the presence of oxygen producers at these times. Geological features suggestive of oxygen, such as red beds, lateritic paleosols, and the return of sedimentary sulfate deposits after a approximately 900-million year hiatus, occur shortly before the approximately 2.3-2.2 Ga Makganyene "snowball Earth" (global glaciation). The massive deposition of Mn, which has a high redox potential, practically requires the presence of environmental oxygen after the snowball. New age constraints from the Transvaal Supergroup of South Africa suggest that all three glaciations in the Huronian Supergroup of Canada predate the Snowball event. A simple cyanobacterial growth model incorporating the range of C, Fe, and P fluxes expected during a partial glaciation in an anoxic world with high-Fe oceans indicates that oxygenic photosynthesis could have destroyed a methane greenhouse and triggered a snowball event on time-scales as short as 1 million years. As the geological evidence requiring oxygen does not appear during the Pongola glaciation at 2.9 Ga or during the Huronian glaciations, we argue that oxygenic cyanobacteria evolved and radiated shortly before the Makganyene snowball.},
    url = "https://doi.org/10.1073/pnas.0504878102",
    doi = "10.1073/pnas.0504878102",
    openalex = "W2145815106",
    references = "doi101146annurevearth241191, doi102113gsecongeo6871135"
}

We report on the results of the Sun in Time multiwavelength program (X-rays to UV) of solar analogs with ages covering ∼0.1-7 Gyr. The chief science goals are to study the solar magnetic dynamo and to determine the radiative and magnetic properties of the Sun during its evolution across the main sequence. The present paper focuses on the latter goal, which has the ultimate purpose of providing the spectral irradiance evolution of solar-type stars to be used in the study and modeling of planetary atmospheres. The results from the Sun in Time program suggest that the coronal X-ray-EUV emissions of the young main-sequence Sun were ∼100-1000 times stronger than those of the present Sun. Similarly, the transition region and chromospheric FUV-UV emissions of the young Sun are expected to be 20-60 and 10-20 times stronger, respectively, than at present. When we consider the integrated high-energy emission from 1 to 1200 Å, the resulting relationship indicates that about 2.5 Gyr ago the solar high-energy flux was about 2.5 times the present value and about 3.5 Gyr ago was about 6 times the present value (when life supposedly arose on Earth). The strong radiation emissions inferred should have had major influences on the thermal structure, photochemistry, and photoionization of planetary atmospheres and have played an important role in the development of primitive life in the solar system. Some examples of the application of the Sun in Time results on exoplanets and on early solar system planets are discussed.

@article{doi101086427977,
    author = "Ribas, I. and Guinan, E. F. and Güdel, M. and Audard, M.",
    title = "Evolution of the Solar Activity over Time and Effects on Planetary Atmospheres. I. High‐Energy Irradiances (1–1700 A)",
    year = "2005",
    journal = "The Astrophysical Journal",
    abstract = "We report on the results of the Sun in Time multiwavelength program (X-rays to UV) of solar analogs with ages covering ∼0.1-7 Gyr. The chief science goals are to study the solar magnetic dynamo and to determine the radiative and magnetic properties of the Sun during its evolution across the main sequence. The present paper focuses on the latter goal, which has the ultimate purpose of providing the spectral irradiance evolution of solar-type stars to be used in the study and modeling of planetary atmospheres. The results from the Sun in Time program suggest that the coronal X-ray-EUV emissions of the young main-sequence Sun were ∼100-1000 times stronger than those of the present Sun. Similarly, the transition region and chromospheric FUV-UV emissions of the young Sun are expected to be 20-60 and 10-20 times stronger, respectively, than at present. When we consider the integrated high-energy emission from 1 to 1200 Å, the resulting relationship indicates that about 2.5 Gyr ago the solar high-energy flux was about 2.5 times the present value and about 3.5 Gyr ago was about 6 times the present value (when life supposedly arose on Earth). The strong radiation emissions inferred should have had major influences on the thermal structure, photochemistry, and photoionization of planetary atmospheres and have played an important role in the development of primitive life in the solar system. Some examples of the application of the Sun in Time results on exoplanets and on early solar system planets are discussed.",
    url = "https://doi.org/10.1086/427977",
    doi = "10.1086/427977",
    openalex = "W2082329580",
    references = "doi101006icar19931010, doi101038342139a0, doi101086304264"
}

@incollection{furnham2006atmospherics,
    author = "Furnham, Adrian",
    title = "Atmospherics",
    year = "2006",
    booktitle = "Management Mumbo-Jumbo",
    url = "https://doi.org/10.1057/9780230626591\_5",
    doi = "10.1057/9780230626591\_5",
    pages = "23-25"
}

@article{doi101007s1121400894135,
    author = "Lämmer, H. and Kasting, James F. and Chassefière, Éric and Johnson, Robert E. and Kulikov, Yuri N. and Tian, Feng",
    title = "Atmospheric Escape and Evolution of Terrestrial Planets and Satellites",
    year = "2008",
    journal = "Space Science Reviews",
    url = "https://doi.org/10.1007/s11214-008-9413-5",
    doi = "10.1007/s11214-008-9413-5",
    openalex = "W1972266886",
    references = "doi1010160019103583900325"
}

Photoionization heating from UV radiation incident on the atmospheres of hot Jupiters may drive planetary mass loss. We construct a model of escape that includes realistic heating and cooling, ionization balance, tidal gravity, and pressure confinement by the host star wind. We show that mass loss takes the form of a hydrodynamic ("Parker") wind, emitted from the planet's dayside during lulls in the stellar wind. When dayside winds are suppressed by the confining action of the stellar wind, nightside winds might pick up if there is sufficient horizontal transport of heat. A hot Jupiter loses mass at maximum rates of ~2 x 10^12 g/s during its host star's pre-main-sequence phase and ~2 x10^10 g/s during the star's main sequence lifetime, for total maximum losses of ~0.06% and ~0.6% of the planet's mass, respectively. For UV fluxes F_UV < 10^4 erg/cm^2/s, the mass loss rate is approximately energy-limited and is proportional to F_UV^0.9. For larger UV fluxes, such as those typical of T Tauri stars, radiative losses and plasma recombination force the mass loss rate to increase more slowly as F_UV^0.6. Dayside winds are quenched during the T Tauri phase because of confinement by overwhelming stellar wind pressure. We conclude that while UV radiation can indeed drive winds from hot Jupiters, such winds cannot significantly alter planetary masses during any evolutionary stage. They can, however, produce observable signatures. Candidates for explaining why the Lyman-alpha photons of HD 209458 are absorbed at Doppler-shifted velocities of +/- 100 km/s include charge-exchange in the shock between the planetary and stellar winds.

@article{doi1010880004637x693123,
    author = "Murray‐Clay, Ruth and Chiang, Eugene and Murray, Norman",
    title = "ATMOSPHERIC ESCAPE FROM HOT JUPITERS",
    year = "2009",
    journal = "The Astrophysical Journal",
    abstract = {Photoionization heating from UV radiation incident on the atmospheres of hot Jupiters may drive planetary mass loss. We construct a model of escape that includes realistic heating and cooling, ionization balance, tidal gravity, and pressure confinement by the host star wind. We show that mass loss takes the form of a hydrodynamic ("Parker") wind, emitted from the planet's dayside during lulls in the stellar wind. When dayside winds are suppressed by the confining action of the stellar wind, nightside winds might pick up if there is sufficient horizontal transport of heat. A hot Jupiter loses mass at maximum rates of \textasciitilde 2 x 10^12 g/s during its host star's pre-main-sequence phase and \textasciitilde 2 x10^10 g/s during the star's main sequence lifetime, for total maximum losses of \textasciitilde 0.06\% and \textasciitilde 0.6\% of the planet's mass, respectively. For UV fluxes F\_UV < 10^4 erg/cm^2/s, the mass loss rate is approximately energy-limited and is proportional to F\_UV^0.9. For larger UV fluxes, such as those typical of T Tauri stars, radiative losses and plasma recombination force the mass loss rate to increase more slowly as F\_UV^0.6. Dayside winds are quenched during the T Tauri phase because of confinement by overwhelming stellar wind pressure. We conclude that while UV radiation can indeed drive winds from hot Jupiters, such winds cannot significantly alter planetary masses during any evolutionary stage. They can, however, produce observable signatures. Candidates for explaining why the Lyman-alpha photons of HD 209458 are absorbed at Doppler-shifted velocities of +/- 100 km/s include charge-exchange in the shock between the planetary and stellar winds.},
    url = "https://doi.org/10.1088/0004-637x/693/1/23",
    doi = "10.1088/0004-637x/693/1/23",
    openalex = "W1974543936"
}

@misc{crossref2011atmospherics,
    title = "Atmospherics",
    year = "2011",
    booktitle = "Encyclopedia of Sports Management and Marketing",
    url = "https://doi.org/10.4135/9781412994156.n42",
    doi = "10.4135/9781412994156.n42"
}

“Atmospherics is the tailoring of the designed (sometimes referred to as ‘built’ – see Mehrabian and Russell, 1974) environment to enhance the likelihood of desired effects or outcomes in users” (Greenland and McGoldrick, 1994).

@misc{greenland2015atmospherics,
    author = "Greenland, Steve and Newman, Andrew",
    title = "Atmospherics",
    year = "2015",
    booktitle = "Wiley Encyclopedia of Management",
    abstract = "“Atmospherics is the tailoring of the designed (sometimes referred to as ‘built’ – see Mehrabian and Russell, 1974) environment to enhance the likelihood of desired effects or outcomes in users” (Greenland and McGoldrick, 1994).",
    url = "https://doi.org/10.1002/9781118785317.weom090343",
    doi = "10.1002/9781118785317.weom090343",
    pages = "1-1"
}

@incollection{yung2015solar,
    author = "Yung, Y.L. and Wong, M.L. and Gaidos, E.J.",
    title = "SOLAR SYSTEM/SUN, ATMOSPHERES, EVOLUTION OF ATMOSPHERES | Evolution of Earth's Atmosphere",
    year = "2015",
    booktitle = "Encyclopedia of Atmospheric Sciences",
    url = "https://doi.org/10.1016/b978-0-12-382225-3.00038-4",
    doi = "10.1016/b978-0-12-382225-3.00038-4",
    openalex = "W29049456",
    pages = "163-167",
    references = "doi101006icar19951122, doi1010160019103587900224, doi101038338487a0, doi101073pnas0504878102, doi101093oso97801951050180010001, doi101126science11536547, doi101126science1183260, doi1015159780691220239, doi103402tellusav26i129731"
}

As the search for Earth-like exoplanets gathers pace, in order to understand them, we need comprehensive theories for how planetary atmospheres form and evolve. Written by two well-known planetary scientists, this text explains the physical and chemical principles of atmospheric evolution and planetary atmospheres, in the context of how atmospheric composition and climate determine a planet&apos;s habitability. The authors survey our current understanding of the atmospheric evolution and climate on Earth, on other rocky planets within our Solar System, and on planets far beyond. Incorporating a rigorous mathematical treatment, they cover the concepts and equations governing a range of topics, including atmospheric chemistry, thermodynamics, radiative transfer, and atmospheric dynamics, and provide an integrated view of planetary atmospheres and their evolution. This interdisciplinary text is an invaluable one-stop resource for graduate-level students and researchers working across the fields of atmospheric science, geochemistry, planetary science, astrobiology, and astronomy.

@book{doi1010179781139020558,
    author = "Catling, David C. and Kasting, James F.",
    title = "Atmospheric Evolution on Inhabited and Lifeless Worlds",
    year = "2017",
    booktitle = "Cambridge University Press eBooks",
    abstract = "As the search for Earth-like exoplanets gathers pace, in order to understand them, we need comprehensive theories for how planetary atmospheres form and evolve. Written by two well-known planetary scientists, this text explains the physical and chemical principles of atmospheric evolution and planetary atmospheres, in the context of how atmospheric composition and climate determine a planet\'s habitability. The authors survey our current understanding of the atmospheric evolution and climate on Earth, on other rocky planets within our Solar System, and on planets far beyond. Incorporating a rigorous mathematical treatment, they cover the concepts and equations governing a range of topics, including atmospheric chemistry, thermodynamics, radiative transfer, and atmospheric dynamics, and provide an integrated view of planetary atmospheres and their evolution. This interdisciplinary text is an invaluable one-stop resource for graduate-level students and researchers working across the fields of atmospheric science, geochemistry, planetary science, astrobiology, and astronomy.",
    url = "https://doi.org/10.1017/9781139020558",
    doi = "10.1017/9781139020558",
    openalex = "W2611894198"
}

@article{gebauer2017evolution,
    author = "Gebauer, S. and Grenfell, J.L. and Stock, J.W. and Lehmann, R. and Godolt, M. and von Paris, P. and Rauer, H.",
    title = "Evolution of Earth-like Extrasolar Planetary Atmospheres: Assessing the Atmospheres and Biospheres of Early Earth Analog Planets with a Coupled Atmosphere Biogeochemical Model",
    year = "2017",
    journal = "Astrobiology",
    url = "https://doi.org/10.1089/ast.2015.1384",
    doi = "10.1089/ast.2015.1384",
    number = "1",
    openalex = "W2577254876",
    pages = "27-54",
    volume = "17",
    references = "doi101002aic690010222, doi101002qj49709640815, doi101006icar19931010, doi10102997jd00237, doi101038247181a0, doi1011751520046919670240241teotaw20co2, doi101256004316502320517344, doi1015159780691220239, doi105860choice305638a, openalexw1552913007"
}

@article{doi101007s001590180108y,
    author = "Lämmer, H. and Zerkle, Aubrey L. and Gebauer, S and Tosi, Nicola and Noack, Lena and Scherf, Manuel and Pilat‐Lohinger, Elke and Güdel, M. and Grenfell, John Lee and Godolt, M. and Nikolaou, Athanasia",
    title = "Origin and evolution of the atmospheres of early Venus, Earth and Mars",
    year = "2018",
    journal = "The Astronomy and Astrophysics Review",
    url = "https://doi.org/10.1007/s00159-018-0108-y",
    doi = "10.1007/s00159-018-0108-y",
    openalex = "W2801411495",
    references = "doi1010160019103583900325, doi1010292006je002784, gebauer2017evolution"
}

@article{gebauer2018evolution,
    author = "Gebauer, S. and Grenfell, J.L. and Lehmann, R. and Rauer, H.",
    title = "Evolution of Earth-like Planetary Atmospheres around M Dwarf Stars: Assessing the Atmospheres and Biospheres with a Coupled Atmosphere Biogeochemical Model",
    year = "2018",
    journal = "Astrobiology",
    url = "https://doi.org/10.1089/ast.2017.1723",
    doi = "10.1089/ast.2017.1723",
    number = "7",
    openalex = "W2883137068",
    pages = "856-872",
    volume = "18",
    references = "doi101006icar19931010, doi101016jsolener200308039, doi10102997jd00237, doi101038247181a0, doi101038nature17448, doi101038nature19106, doi101038nature21360, doi1010510004636120078091, doi101086306745, doi101089ast20141231"
}

Context. The characterisation of the atmosphere of exoplanets is one of the main goals of exoplanet science in the coming decades. Aims. We investigate the detectability of atmospheric spectral features of Earth-like planets in the habitable zone (HZ) around M dwarfs with the future James Webb Space Telescope (JWST). Methods. We used a coupled 1D climate-chemistry-model to simulate the influence of a range of observed and modelled M-dwarf spectra on Earth-like planets. The simulated atmospheres served as input for the calculation of the transmission spectra of the hypothetical planets, using a line-by-line spectral radiative transfer model. To investigate the spectroscopic detectability of absorption bands with JWST we further developed a signal-to-noise ratio (S/N) model and applied it to our transmission spectra. Results. High abundances of methane (CH 4) and water (H 2 O) in the atmosphere of Earth-like planets around mid to late M dwarfs increase the detectability of the corresponding spectral features compared to early M-dwarf planets. Increased temperatures in the middle atmosphere of mid- to late-type M-dwarf planets expand the atmosphere and further increase the detectability of absorption bands. To detect CH 4, H 2 O, and carbon dioxide (CO 2) in the atmosphere of an Earth-like planet around a mid to late M dwarf observing only one transit with JWST could be enough up to a distance of 4 pc and less than ten transits up to a distance of 10 pc. As a consequence of saturation limits of JWST and less pronounced absorption bands, the detection of spectral features of hypothetical Earth-like planets around most early M dwarfs would require more than ten transits. We identify 276 existing M dwarfs (including GJ 1132, TRAPPIST-1, GJ 1214, and LHS 1140) around which atmospheric absorption features of hypothetical Earth-like planets could be detected by co-adding just a few transits. Conclusions. The TESS satellite will likely find new transiting terrestrial planets within 15 pc from the Earth. We show that using transmission spectroscopy, JWST could provide enough precision to be able to partly characterise the atmosphere of TESS findings with an Earth-like composition around mid to late M dwarfs.

@article{doi10105100046361201834504,
    author = "Wunderlich, Fabian and Godolt, M. and Grenfell, John Lee and Städt, Steffen and Smith, A. M. S. and Gebauer, S and Schreier, Franz and Hedelt, Pascal and Rauer, H.",
    title = "Detectability of atmospheric features of Earth-like planets in the habitable zone around M dwarfs",
    year = "2019",
    journal = "Astronomy and Astrophysics",
    abstract = "Context. The characterisation of the atmosphere of exoplanets is one of the main goals of exoplanet science in the coming decades. Aims. We investigate the detectability of atmospheric spectral features of Earth-like planets in the habitable zone (HZ) around M dwarfs with the future James Webb Space Telescope (JWST). Methods. We used a coupled 1D climate-chemistry-model to simulate the influence of a range of observed and modelled M-dwarf spectra on Earth-like planets. The simulated atmospheres served as input for the calculation of the transmission spectra of the hypothetical planets, using a line-by-line spectral radiative transfer model. To investigate the spectroscopic detectability of absorption bands with JWST we further developed a signal-to-noise ratio (S/N) model and applied it to our transmission spectra. Results. High abundances of methane (CH 4) and water (H 2 O) in the atmosphere of Earth-like planets around mid to late M dwarfs increase the detectability of the corresponding spectral features compared to early M-dwarf planets. Increased temperatures in the middle atmosphere of mid- to late-type M-dwarf planets expand the atmosphere and further increase the detectability of absorption bands. To detect CH 4, H 2 O, and carbon dioxide (CO 2) in the atmosphere of an Earth-like planet around a mid to late M dwarf observing only one transit with JWST could be enough up to a distance of 4 pc and less than ten transits up to a distance of 10 pc. As a consequence of saturation limits of JWST and less pronounced absorption bands, the detection of spectral features of hypothetical Earth-like planets around most early M dwarfs would require more than ten transits. We identify 276 existing M dwarfs (including GJ 1132, TRAPPIST-1, GJ 1214, and LHS 1140) around which atmospheric absorption features of hypothetical Earth-like planets could be detected by co-adding just a few transits. Conclusions. The TESS satellite will likely find new transiting terrestrial planets within 15 pc from the Earth. We show that using transmission spectroscopy, JWST could provide enough precision to be able to partly characterise the atmosphere of TESS findings with an Earth-like composition around mid to late M dwarfs.",
    url = "https://doi.org/10.1051/0004-6361/201834504",
    doi = "10.1051/0004-6361/201834504",
    openalex = "W2917710115",
    references = "gebauer2017evolution, gebauer2018evolution"
}

@incollection{schlessinger2019atmospherics,
    author = "Schlessinger, Monroe",
    title = "Atmospherics",
    year = "2019",
    booktitle = "Infrared Technology Fundamentals",
    url = "https://doi.org/10.1201/9780203750834-4",
    doi = "10.1201/9780203750834-4",
    pages = "76-92"
}

@incollection{hannah2021atmospherics,
    author = "Hannah, Dehlia",
    title = "Atmospherics",
    year = "2021",
    booktitle = "Routledge Handbook of Art, Science, and Technology Studies",
    url = "https://doi.org/10.4324/9780429437069-47",
    doi = "10.4324/9780429437069-47",
    pages = "591-645"
}

Kuiper belt objects (KBOs) have diverse surface compositions, and the New Horizons mission to the Pluto-Charon system allows us to test hypotheses on the origin and evolution of these KBO surfaces. Previous work proposed that Charon's organic-rich north pole formed from radiolytically processed volatiles sourced from Pluto's escaping atmosphere. Here, we show an endogenic source of volatiles from Charon's interior is plausible. We calculate that cryovolcanic resurfacing released 1.29 × 1015-3.47 × 1015 kg of methane to Charon's surface from its interior. We modeled volatile transport and found the vast majority of this volcanically released methane migrates to Charon's poles, with deposition rates sufficient to be processed into the observed organic compounds. Irradiated methane products appear on similarly sized KBOs that do not orbit a Pluto-sized object to draw an escaping atmosphere from, so interior-sourced volatiles could be a common and important process across the Kuiper belt.

@article{doi101038s41467022318468,
    author = "Menten, Stephanie M and Sori, Michael M and Bramson, Ali M",
    title = "Endogenically sourced volatiles on Charon and other Kuiper belt objects.",
    year = "2022",
    journal = "Nature communications",
    abstract = "Kuiper belt objects (KBOs) have diverse surface compositions, and the New Horizons mission to the Pluto-Charon system allows us to test hypotheses on the origin and evolution of these KBO surfaces. Previous work proposed that Charon's organic-rich north pole formed from radiolytically processed volatiles sourced from Pluto's escaping atmosphere. Here, we show an endogenic source of volatiles from Charon's interior is plausible. We calculate that cryovolcanic resurfacing released 1.29 × 1015-3.47 × 1015 kg of methane to Charon's surface from its interior. We modeled volatile transport and found the vast majority of this volcanically released methane migrates to Charon's poles, with deposition rates sufficient to be processed into the observed organic compounds. Irradiated methane products appear on similarly sized KBOs that do not orbit a Pluto-sized object to draw an escaping atmosphere from, so interior-sourced volatiles could be a common and important process across the Kuiper belt.",
    url = "https://pmc.ncbi.nlm.nih.gov/articles/PMC9363412/",
    doi = "10.1038/s41467-022-31846-8",
    openalex = "W4290786844",
    pmcid = "PMC9363412",
    pmid = "35945207",
    references = "doi1010160009254194001404, doi1010160019103584901428, doi101016jepsl200605041, doi101017s0305004100023197, doi101038s41467022318468, doi101086191050, doi101126science1106818, doi101126scienceaad1815, doi101126scienceaad7055, doi101126scienceaad9189, doi1012019781315380476"
}

Abstract Planets orbiting M-dwarf stars are prime targets in the search for rocky exoplanet atmospheres. The small size of M dwarfs renders their planets exceptional targets for transmission spectroscopy, facilitating atmospheric characterization. However, it remains unknown whether their host stars’ highly variable extreme-UV radiation environments allow atmospheres to persist. With JWST, we have begun to determine whether or not the most favorable rocky worlds orbiting M dwarfs have detectable atmospheres. Here, we present a 2.8–5.2 μ m JWST NIRSpec/G395H transmission spectrum of the warm (700 K, 40.3× Earth’s insolation) super-Earth GJ 486b (1.3 R ⊕ and 3.0 M ⊕). The measured spectrum from our two transits of GJ 486b deviates from a flat line at 2.2 σ − 3.3 σ, based on three independent reductions. Through a combination of forward and retrieval models, we determine that GJ 486b either has a water-rich atmosphere (with the most stringent constraint on the retrieved water abundance of H 2 O > 10% to 2 σ) or the transmission spectrum is contaminated by water present in cool unocculted starspots. We also find that the measured stellar spectrum is best fit by a stellar model with cool starspots and hot faculae. While both retrieval scenarios provide equal quality fits (χ ν 2 = 1.0) to our NIRSpec/G395H observations, shorter wavelength observations can break this degeneracy and reveal if GJ 486b sustains a water-rich atmosphere.

@article{doi10384720418213accb9c,
    author = "Moran, Sarah E. and Stevenson, Kevin B. and Sing, David K. and MacDonald, Ryan J. and Kirk, James and Lustig‐Yaeger, Jacob and Peacock, Sarah and Mayorga, L. C. and Bennett, Katherine A. and López‐Morales, Mercedes and May, Erin and Rustamkulov, Zafar and Valenti, Jeff A. and Redai, Jéa Adams and Alam, Munazza K. and Batalha, Natasha E. and Fu, Guangwei and Gonzalez-Quiles, Junellie and Highland, Alicia N. and Kruse, Ethan and Lothringer, Joshua D. and Ceballos, Kevin Ortiz and Sotzen, Kristin S. and Wakeford, Hannah R.",
    title = "High Tide or Riptide on the Cosmic Shoreline? A Water-rich Atmosphere or Stellar Contamination for the Warm Super-Earth GJ 486b from JWST Observations",
    year = "2023",
    journal = "The Astrophysical Journal Letters",
    abstract = "Abstract Planets orbiting M-dwarf stars are prime targets in the search for rocky exoplanet atmospheres. The small size of M dwarfs renders their planets exceptional targets for transmission spectroscopy, facilitating atmospheric characterization. However, it remains unknown whether their host stars’ highly variable extreme-UV radiation environments allow atmospheres to persist. With JWST, we have begun to determine whether or not the most favorable rocky worlds orbiting M dwarfs have detectable atmospheres. Here, we present a 2.8–5.2 μ m JWST NIRSpec/G395H transmission spectrum of the warm (700 K, 40.3× Earth’s insolation) super-Earth GJ 486b (1.3 R ⊕ and 3.0 M ⊕). The measured spectrum from our two transits of GJ 486b deviates from a flat line at 2.2 σ − 3.3 σ, based on three independent reductions. Through a combination of forward and retrieval models, we determine that GJ 486b either has a water-rich atmosphere (with the most stringent constraint on the retrieved water abundance of H 2 O > 10\% to 2 σ) or the transmission spectrum is contaminated by water present in cool unocculted starspots. We also find that the measured stellar spectrum is best fit by a stellar model with cool starspots and hot faculae. While both retrieval scenarios provide equal quality fits (χ ν 2 = 1.0) to our NIRSpec/G395H observations, shorter wavelength observations can break this degeneracy and reveal if GJ 486b sustains a water-rich atmosphere.",
    url = "https://doi.org/10.3847/2041-8213/accb9c",
    doi = "10.3847/2041-8213/accb9c",
    openalex = "W4376983012",
    references = "doi10384715384357aa7846"
}

@article{regoli2023understanding,
    author = "Regoli, Leonardo and Brandt, Pontus and Andre, Mats and Brain, David and Chaffin, Mike and Cohen, Ian and Dandouras, Iannis and Gkioulidou, Matina and Holmstrom, Mats and Ilie, Raluca and Jasinski, Jamie and Keika, Kunihiro and Kollmann, Peter and Lillis, Robert and Nikoukar, Romina and Nordheim, Tom and Rymer, Abigail and Seki, Kanako and Tucker, Orenthal and Vourlidas, Angelos",
    title = "Understanding the Evolution of Planetary Atmospheres: the need for an Earth-based atmospheric escape mission",
    year = "2023",
    journal = "Bulletin of the AAS",
    url = "https://doi.org/10.3847/25c2cfeb.8e5df1cf",
    doi = "10.3847/25c2cfeb.8e5df1cf",
    openalex = "W4386360768",
    references = "doi1010022014ja020714, doi101016jicarus201505012, doi101016jicarus201805030, doi1010179781139020558, doi1010292006ja011823, doi101029jd094id12p14971, doi101126science1058913"
}

@incollection{stewart2023atmospherics,
    author = "STEWART, KATHLEEN",
    title = "Atmospherics",
    year = "2023",
    booktitle = "A to Z of Creative Writing Methods",
    url = "https://doi.org/10.5040/9781350184244.ch-3",
    doi = "10.5040/9781350184244.ch-3"
}

@incollection{lee2024atmospherics,
    author = "Lee, Jason W.",
    title = "Atmospherics",
    year = "2024",
    booktitle = "Encyclopedia of Sport Management",
    url = "https://doi.org/10.4337/9781035317189.ch41",
    doi = "10.4337/9781035317189.ch41",
    pages = "70-72"
}