Relevant bibliographies by topics / Atmosphere

Academic literature on the topic 'Atmosphere'

Author: Grafiati
Published: 4 June 2021
Last updated: 31 July 2024

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Journal articles on the topic "Atmosphere"

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Sergeev, Denis E., Nathan J. Mayne, Thomas Bendall, Ian A. Boutle, Alex Brown, Iva Kavčič, James Kent, et al. "Simulations of idealised 3D atmospheric flows on terrestrial planets using LFRic-Atmosphere." Geoscientific Model Development 16, no. 19 (October 10, 2023): 5601–26. http://dx.doi.org/10.5194/gmd-16-5601-2023.

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Abstract. We demonstrate that LFRic-Atmosphere, a model built using the Met Office's GungHo dynamical core, is able to reproduce idealised large-scale atmospheric circulation patterns specified by several widely used benchmark recipes. This is motivated by the rapid rate of exoplanet discovery and the ever-growing need for numerical modelling and characterisation of their atmospheres. Here we present LFRic-Atmosphere's results for the idealised tests imitating circulation regimes commonly used in the exoplanet modelling community. The benchmarks include three analytic forcing cases: the standard Held–Suarez test, the Menou–Rauscher Earth-like test, and the Merlis–Schneider tidally locked Earth test. Qualitatively, LFRic-Atmosphere agrees well with other numerical models and shows excellent conservation properties in terms of total mass, angular momentum, and kinetic energy. We then use LFRic-Atmosphere with a more realistic representation of physical processes (radiation, subgrid-scale mixing, convection, clouds) by configuring it for the four TRAPPIST-1 Habitable Atmosphere Intercomparison (THAI) scenarios. This is the first application of LFRic-Atmosphere to a possible climate of a confirmed terrestrial exoplanet. LFRic-Atmosphere reproduces the THAI scenarios within the spread of the existing models across a range of key climatic variables. Our work shows that LFRic-Atmosphere performs well in the seven benchmark tests for terrestrial atmospheres, justifying its use in future exoplanet climate studies.
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Ragossnig, Florian, Alexander Stökl, Ernst Dorfi, Colin P. Johnstone, Daniel Steiner, and Manuel Güdel. "Interaction of infalling solid bodies with primordial atmospheres of disk-embedded planets." Astronomy & Astrophysics 618 (October 2018): A19. http://dx.doi.org/10.1051/0004-6361/201832681.

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Context. Planets that form early enough to be embedded in the circumstellar gas disk accumulate thick atmospheres of nebular gas. Models of these atmospheres need to specify the surface luminosity (i.e. energy loss rate) of the planet. This luminosity is usually associated with a continuous inflow of solid bodies, where the gravitational energy released from these bodies is the source of energy. However, if these bodies release energy in the atmosphere instead of at the surface, this assumption might not be justified. Aims. Our aim is to explore the interactions of infalling planetesimals with primordial atmospheres at an embedded phase of evolution. We investigate effects of atmospheric interaction on the planetesimals (mass loss) and the atmosphere (heating/cooling). Methods. We used atmospheric parameters from a snapshot of time-dependent evolution simulations for embedded atmospheres and simulated purely radial, infall events of siliceous planetesimals in a 1D, explicit code. We implemented energy transfer between friction, radiation transfer by the atmosphere and the body, and thermal ablation; this gives us the possibility to examine the effects on the planetesimals and the atmosphere. Results. We find that a significant amount of gravitational energy is indeed dissipated into the atmosphere, especially for larger planetary cores, which consequently cannot contribute to the atmospheric planetary luminosity. Furthermore, we examine that planetesimal infall events for cores, MC > 2M⊕, which actually result in a local cooling of the atmosphere; this is totally in contradiction with the classical model.
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Chouqar, J., Z. Benkhaldoun, A. Jabiri, J. Lustig-Yaeger, A. Soubkiou, and A. Szentgyorgyi. "Properties of sub-Neptune atmospheres: TOI-270 system." Monthly Notices of the Royal Astronomical Society 495, no. 1 (May 2, 2020): 962–70. http://dx.doi.org/10.1093/mnras/staa1198.

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ABSTRACT We investigate the potential for the James Webb Space Telescope (JWST) to detect and characterize the atmospheres of the sub-Neptunian exoplanets in the TOI-270 system. Sub-Neptunes are considered more likely to be water worlds than gas dwarfs. We model their atmospheres using three atmospheric compositions – two examples of hydrogen-dominated atmospheres and a water-dominated atmosphere. We then simulate the infrared transmission spectra of these atmospheres for JWST instrument modes optimized for transit observation of exoplanet atmospheres: NIRISS, NIRSpec, and MIRI. We then predict the observability of each exoplanet’s atmosphere. TOI-270c and d are excellent targets for detecting atmospheres with JWST transmission spectroscopy, requiring only 1 transit observation with NIRISS, NIRSpec, and MIRI; higher signal-to-noise ratio can be obtained for a clear H-rich atmosphere. Fewer than three transits with NIRISS and NIRSpec may be enough to reveal molecular features. Water-dominated atmospheres require more transits. Water spectral features in water-dominated atmospheres may be detectable with NIRISS in two or three transits. We find that the detection of spectral features in a cloudy, H-rich atmosphere does not require integrations as long as those required for the water-dominated atmosphere, which is consistent with the differences in atmospheric mean molecular weight. TOI-270c and d could be prime targets for JWST transit observations of sub-Neptune atmospheres. These results provide useful predictions for observers who may propose to use JWST to detect and characterize the TOI-270 planet atmospheres.
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Sysoeva, Yu V. "Проблема атмосферы у Г. Беме и ее отношение к цифровой культуре." Studia Culturae, no. 56 (November 2, 2023): 120. http://dx.doi.org/10.31312/2310-1245-2023-56-120-143.

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This article is devoted to a relatively new aesthetic concept, the concept of atmosphere. In the second half of the 20th century, due to the overcoming of the understanding of the aesthetic as a field of art and the emergence of the tendency to appeal to sensual experience, the idea that aesthetic perception and aesthetic experience are possible not only in the context of art events, but also in the space of everyday life is becoming increasingly relevant. The aesthetics of atmosphere arises from the aesthetics of everyday life. The first to declare the concept of atmosphere as a separate aesthetic theory was H. Böhme (1937–2022). The immediate predecessors of the concept of atmospheres are the theoretical positions of G. Schmitz and W. Benjamin. The aesthetics of atmospheres explores the states that arise in the process of the relationship between the subjective and the objective factors and in their material, emotional interaction. This article analyzes H. Beme’s concept of atmosphere, as presented by him in his works: “‘Atmosphere’ as a fundamental concept of the new aesthetics”, “Atmospheric Architectures: The Aesthetics of Felt Spaces”, “Architektur und Atmosphäre”. A special place in H. Beme’s aesthetic theory of atmospheres is occupied, first, by the concept of “ecstasy of things” introduced by him, which allows us to speak of the relatively objective nature of atmospheres, and, second, by the problem of the production of artificial atmospheres. Most studies of atmosphere as an aesthetic category consider atmosphere in the context of architecture, urban environment, design, etc. This article attempts to explore the atmosphere in digital space. At present, digital space has already lost its representational and in principle auxiliary position in relation to the human being, and has become a space for the realization of possibilities, the functioning of which was not represented in the human being’s being. The specific possibilities of the digital require a special analysis of the aesthetic, capable of exploring the digital space in its entirety. The article suggests that the concept of atmospheres is a productive way to work with digital space, which is shown on the example of such digital space phenomena as metavelves and ASMR-video. The study showed that the concept of atmospheres is convenient for working with digital space, especially due to the fact that with its help it is possible to carry out successful analysis not only of visual and auditory components (characteristic for classical aesthetics), but also of other ways of aesthetic perception.
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Seager, Sara. "Exoplanet atmospheres: A theoretical outlook." Proceedings of the International Astronomical Union 6, S276 (October 2010): 198–207. http://dx.doi.org/10.1017/s1743921311020187.

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AbstractWith over two dozen exoplanet atmospheres observed today, the field of exoplanet atmospheres is solidly established. The highlights of exoplanet atmosphere studies include: detection of molecular spectral features; constraints on atmospheric vertical temperature structure; detection of day-night temperature gradients; and a new numerical approach to atmosphere temperature and abundance retrieval. As hot Jupiter observations and interpretation are maturing, the next frontier is super Earth atmospheres. Theoretical models of super Earth atmospheres are moving forward with observational hopes pinned on the James Webb Space Telescope, scheduled for launch in 2014. Further in the future lies direct imaging attempts to answer the enigmatic and ancient question, “Are we alone?” via atmospheric biosignatures.
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Miller-Ricci, Eliza, Sara Seager, and Dimitar Sasselov. "The Atmospheres of Extrasolar Super-Earths." Proceedings of the International Astronomical Union 4, S253 (May 2008): 263–71. http://dx.doi.org/10.1017/s1743921308026483.

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AbstractExtrasolar super-Earths (1-10 M⊕) are likely to exist with a wide range of atmospheres. While a number of these planets have already been discovered through radial velocities and microlensing, it will be the discovery of the firsttransitingsuper-Earths that will open the door to a variety of follow-up observations aimed at characterizing their atmospheres. Super-Earths may fill a large range of parameter space in terms of their atmospheric composition and mass. Specifically, some of these planets may have high enough surface gravities to be able to retain large hydrogen-rich atmosphseres, while others will have lost most of their hydrogen to space over the planet's lifetime, leaving behind an atmosphere more closely resembling that of Earth or Venus. The resulting composition of the super-Earth atmosphere will therefore depend strongly on factors such as atmospheric escape history, outgassing history, and the level of stellar irradiation that it receives. Here we present theoretical models of super-Earth emission and transmission spectra for a variety of possible outcomes of super-Earth atmospheric composition ranging from hydrogen-rich to hydrogen-poor. We focus on how observations can be used to differentiate between the various scenarios and constrain atmospheric composition.
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Bisikalo, Dmitri, Valery Shematovich, and Benoit Hubert. "The Kinetic Monte Carlo Model of the Auroral Electron Precipitation into N2-O2 Planetary Atmospheres." Universe 8, no. 8 (August 22, 2022): 437. http://dx.doi.org/10.3390/universe8080437.

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Auroral events are the prominent manifestation of solar/stellar forcing on planetary atmospheres. They are closely related to the energy deposition by and evolution of planetary atmospheres, and their observations are widely used to analyze the composition, structure, and chemistry of the atmosphere under study, as well as energy fluxes of the precipitating particles that affect the atmosphere. A numerical kinetic Monte Carlo model had been developed, allowing us to study the processes of precipitation of high-energy auroral electrons into the N2-O2 atmospheres of the rocky planets in the Solar and exosolar planetary systems. This model describes on a molecular level the collisions of auroral electrons and atmospheric gas, taking into account the stochastic nature of collisional scattering at high kinetic energies. The current status of the kinetic model is illustrated in the applications to the auroral events on the Earth such as the production of suprathermal nitrogen atoms due to the electron impact dissociation of N2. It was found that electron impact dissociation of N2 can potentially be an important source of suprathermal N atoms in the auroral regions of the N2-O2 atmosphere of terrestrial-type planets. Such research will allow us to study the odd nitrogen chemistry as an atmospheric marker of the N2-O2 atmosphere of rocky exoplanets.
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Kurosaki, Kenji, and Shu-ichiro Inutsuka. "Giant Impact Events for Protoplanets: Energetics of Atmospheric Erosion by Head-on Collision." Astrophysical Journal 954, no. 2 (September 1, 2023): 196. http://dx.doi.org/10.3847/1538-4357/ace9ba.

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Abstract Numerous exoplanets with masses ranging from Earth to Neptune and radii larger than Earth have been found through observations. These planets possess atmospheres that range in mass fractions from 1% to 30%, reflecting the diversity of atmospheric mass fractions. Such diversities are supposed to be caused by differences in the formation processes or evolution. Here, we consider head-on giant impacts onto planets causing atmosphere losses in the later stage of their formation. We perform smoothed particle hydrodynamic simulations to study the impact-induced atmosphere loss of young super-Earths with 10%–30% initial atmospheric mass fractions. We find that the kinetic energy of the escaping atmosphere is almost proportional to the sum of the kinetic impact energy and self-gravitational energy released from the merged core. We derive the relationship between the kinetic impact energy and the escaping atmosphere mass. The giant impact events for planets of comparable masses are required in the final stage of the popular scenario of rocky planet formation. We show it results in a significant loss of the atmosphere, if the impact is a head-on collision with comparable masses. This latter fact provides a constraint on the formation scenario of rocky planets with substantial atmospheres.
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Johnstone, Colin P. "The Influences of Stellar Activity on Planetary Atmospheres." Proceedings of the International Astronomical Union 12, S328 (October 2016): 168–79. http://dx.doi.org/10.1017/s1743921317003775.

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AbstractOn evolutionary timescales, the atmospheres of planets evolve due to interactions with the planet's surface and with the planet's host star. Stellar X-ray and EUV (=’XUV’) radiation is absorbed high in the atmosphere, driving photochemistry, heating the gas, and causing atmospheric expansion and mass loss. Atmospheres can interact strongly with the stellar winds, leading to additional mass loss. In this review, I summarise some of the ways in which stellar output can influence the atmospheres of planets. I will discuss the importance of simultaneously understanding the evolution of the star's output and the time dependent properties of the planet's atmosphere.
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Chowdhury, Sohini, Yadaiah Nirsanametla, and Muralidhar Manapuram. "Investigation on keyhole mode fiber laser welding of SS 316 in a self-protected atmosphere." Proceedings of the Institution of Mechanical Engineers, Part C: Journal of Mechanical Engineering Science 233, no. 18 (July 19, 2019): 6602–15. http://dx.doi.org/10.1177/0954406219864137.

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This work focuses on examining the influence of welding parameters under different welding atmospheres and evaluation of keyhole profile during fiber laser welding operation. The experiments are carried out in two different welding atmospheres, namely self-protected atmosphere of Ar gas and open atmospheric conditions. The effect of these two atmospheric conditions on weld profile formation and dimensions, and microstructural evolution for SS 316 plates are examined. In addition, the keyhole profile is evaluated by using a semi-analytical mathematical model, a point-by-point energy balance determination at the keyhole wall, which is mapped with experimentally measured weld macrographs for similar welding conditions. It has been determined that the weld quality is profound in the case of a self-protected atmosphere with respect to aspect ratio, weld defects, and microstructural characterization. Moreover, better weld bead profile and cleaner weld seam on the upper surface is determined in samples welded in a self-protected atmosphere.
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Dissertations / Theses on the topic "Atmosphere"

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McElroy, Kenneth L. "The atmospheric emission method of calculating the neutral atmosphere and changed particle densities in the upper atmosphere." Thesis, Monterey, California. Naval Postgraduate School, 1992. http://hdl.handle.net/10945/23548.

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Martello, Robert 1968. "Land atmosphere interaction and atmospheric mixed layer height evolution." Thesis, Massachusetts Institute of Technology, 1996. http://hdl.handle.net/1721.1/38774.

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Erculiani, Marco. "Atmosphere in a test tube: laboratory investigations about exoplanet atmospheres." Doctoral thesis, Università degli studi di Padova, 2015. http://hdl.handle.net/11577/3424370.

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The aim of this thesis is to understand if cyanobacteria, grown on an Earth-like planet orbiting around the habitable zone of an M star can survive and use the light coming from the star in a fruitful way, in particular analyzing their gaseous by-products. The organisms chosen usually don't have photopigments capable to photosynthesize the NIR part of the radiation, but can modify their photosynthetic apparatus in order to adapt to different light conditions if exposed in NIR light conditions, producing chlorophyll d and f. The two bacteria highlighted for our purpose are Chlorogloeopsis fritschii and Cyanobacterium Aponinum. The first is known to be able to change its photosynthetic apparatus to cope with new radiation conditions. In particular is capable to generate chlorophyll d and f if exposed to NIR light (720 nm). This feature is call FarLip acclimation. The second bacterium is a well known bacterium but no one has ever tried to understand if it has the same capability. Efforts have been done in order to find the best culture medium and the best growth conditions of temperature and pH. In order to understand how photosynthetic life can handle different radiation doses we ideated and realized a novel and pioneering LED radiation source with dynamical features. Its wavelength intervals (365nm-940nm) overlap the limits of photosynthetic pigment absorption range (280-850 nm) of most common photosynthetic bacteria. Our simulator is composed by an array of 25 different channels corresponding to 25 different wavelengths. Each channel can host a maximum of about 15 LEDs. This simulator has been built thinking to modularity. In fact it is endowed by a mosaic of circuit boards arranged in a pie-chart shape, on the surface of which will be welded the LEDs. This solution allows a rapid change of the damaged LEDs and an easy implementations with other wavelengths. This simulator is capable to reproduce the spectra of main sequence F, G, K and M stars as well as the most common commercial lamps within its wavelength intervals. The control system is composed by a Laptop which controls a LED box and an STS-VIS spectrograph from Ocean Optics with cosine corrector. The first system generate the best fit of the input spectrum and give information to the simulator on how to reproduce it. The spectrometer has the task to control the goodness of the fit and, by means of a closed loop system, to adjust it tuning the LED's power in real time. The stellar simulator bas been subjected to several tests. The power emanated from the radiation source has been estimated to be 106.22 W while the thermal power has been calculated to be 434.05 W. The stellar simulator have been characterized in flux, analyzing the radiation at different distances from the device, from the exit of the source up to 25 cm. Then uniformity measurements have been done, analyzing the flux on a distance of 6.5 cm from the centre. Finally, I calculated the absorption of the optics of the radiation source analyzing the spectra coming out from the stellar simulator and compared it with respect to the spectrum of the single LEDs. In order to lodge the bacteria we built new concept incubator made of a stainless steel cell with the potential to flux a desired gaseous mixture inside it and fill the cell with the desired gas mixture. Four wedged optical windows opens on the lateral surface and needs to allow the oxygen and carbon dioxide concentration inside by means of a Tunable Diode Laser Absorption Spectroscopy (TDLAS) system. The cell is topped by a BOROFLOAT uncoated window to collect the light from the stellar simulator. The cell has been characterized in void and oxygen and carbon dioxide detecting limits have been found. During the experiment, bacteria have been grown in white light conditions at for 24 days at 20 micromol photons/m^2/s and at 30°C in order to understand the growth times and the behaviour in optimal conditions. After that, a new growth experiment have been performed by growing both cyanobacteria species at 30°C and 20 micromol photons/m^2/s and oxymetric measurements have been done after 6 days from the culture start, thus during their exponential growth phases. Then, for the main part of the experiment, eight samples have been used. Two samples of Cyanobacterium aponinum have been grown at 20 micromol photons/m^2/s in white light for 6 days and then at 100 micromol photons/m^2/s for the residual 3 days in white light. Two samples of Chlorogloeopsis fritschii have been grown at 20 micromol photons/m^2/s for 6 days in white light and then at 100 micromol photons/m^2/s for the residual 3 days in white light. Two samples of Cyanobacterium aponinum have been grown at 20 micromol photons/m^2/s for 6 days in white light and then at 100 micromol photons/m^2/s for the residual 3 days using the radiation spectrum of an M7 type star. Two samples of Chlorogloeopsis fritschii have been grown at 20 micromol photons/m^2/s for 6 days in white light and then at 100 micromol photons/m^2/s for the residual 3 days using the radiation spectrum of an M7 type star. The temperature has been kept at 30°C for the samples not exposed to M7 light and at a temperature oscillating from 35°C to 38°C for the samples exposed to M7 light. The higher environmental temperature under the stellar simulator has been due to the over-heating of the LEDs. During the 3 days of different exposure measurements of optical density have been done in order to collect data about the different growth curves. Moreover, O2 production have been calculated for each sample. Finally, a chromatic response have been done, in order to understand if the colour would reflect the vitality of the bacteria
Lo scopo di questa tesi è quello di capire come dei cianobatteri, cresciuti su un pianeta di tipo terrestre orbitante attorno alla zona di abitabilità di una stella M possano sopravvivere ed usare la luce proveniente dalla stella stessa in modo fruttuoso per la loro esistenza. In particolare ci focalizzeremo sullo studio dei gas da essi prodotti. Gli organismi scelti non hanno pigmenti in grado di fotosintetizzare la parte NIR dello spettro di radiazione, ma riescono a modificare il loro apparato fotosintetico per far fronte alle nuove condizioni di luce, se esposti a luce NIR, producendo clorofilla d ed f. I due batteri scelti per i nostri esperimenti sono Chlorogloeopsis fritschii e Cyanobacterium Aponinum. Il primo batterio è certamente in grado di variare il suo apparato fotosintetico in differenti situazioni luminose. In particolare è in grado di produrre clorofilla e ed f se esposto a luce NIR (720 nm). Questa proprietà si chiama acclimatamento FarLip. Il secondo batterio è è abbastanza noto ma non è stata ancora studiata la sua predisposizione a questo tipo di pratica. Per questi batteri sono stati ricercati i terreni di coltura, di temperatura e pH che meglio permettessero il loro sviluppo. Per capire come il foto-acclimatamento possa aver luogo abbiamo ideato e realizzato un nuovo tipo di sorgente a LED con peculiarità dinamiche. L'intervallo di lunghezze d'onda che copre (365nm-940nm) si sovrappone ai limiti di assorbimento dei pigmenti fotosintetici (280-850 nm) dei più comuni batteri. Il simulatore è composto da 25 differenti canali corrispondenti a 25 differenti lunghezze d'onda. Ogni canale può ospitare un massimo di 15 LED. Il simulatore come detto è stato concepito secondo il concetto di modularità. Infatti è composto da un mosaico di piastre in corma circolare divisa a spicchi e su ognuna di tali piastre sono saldati i LED. Questa soluzione permette di cambiare rapidamente i LED danneggiati e permette una facile implementazione con altre lunghezze d'onda. Il simulatore stellare è in grado di riprodurre lo spettro di varie stelle di sequenza principale, F, G, K e M e molte delle più comuni lampade. Il sistema di controllo è composto da un PC che ha il compito di gestire i LED e da uno spettrometro con relativo correttore di coseno che STS-VIS della ditta Ocean Optics. Il PC genera il miglior fit dello spettro da ricreare con l'illuminatore e lgi da informazioni su come riprodurlo. Lo spettrometro invece controlla la bontà del fit ed attraverso un sistema a circuito chiuso, regola la luminosità dei LED in tempo reale. Abbiamo fatto dei test per verificare il corretto funzionamento del simulatore e stimato la potenza totale emanata, 106.22 W e quella termica, 434.05 W. Inoltre la nostra sorgente di radiazione è stata caratterizzata in flusso, analizzando la radiazione a diverse distanze, dalla bocca di apertura fino a 25 cm da essa. Poi sono state fatte misure di uniformità del flusso entro 6.5 cm dal centro. Infine è stato calcolato l'assorbimento dovuto alle ottiche frapposte fra i LED e i campioni. Per alloggiare i batteri abbiamo ideato e costruito in incubatore in acciaio inox con la possibilità di avere un continuo flussaggio di gas o di essere riempita con una miscela desiderata. Sui lati si aprono quattro finestre ottiche che servono per permettere la misura di concentrazione di ossigeno e di anidride carbonica all'interno attraverso un sistema laser chiamato Tunable Diode Laser Absorption Spectroscopy (TDLAS). L'incubatore è dotato anche di una finestra superiore in borosilicato per permettere alla luce di entrarvi. La cella è stata caratterizzata termicamente e sono stati calcolati le quantità minime osservabili sia di ossigeno che di anidride carbonica. Durante la prima fase dell'esperimento, i batteri selezionati sono stati fatti crescere per 24 giorni Durante l'esperimento, i batteri sono stati fatti crescere a 24 days at 20 micromol fotoni/m^2/s e a 30 °C per costruire le curve di crescita ed il loro comportamento in condizioni ottimali. Dopo ciò, è stato condotto un secondo esperimento facendo crescere entrambe se specie di cianobatteri a 30°C e 20 micromol fotoni/m^2/s in luce bianca ed acquisendo dopo 6 giorni le misure di produttività di ossigeno durante la fase esponenziale. Passati sei giorni sono stati ripartite otto colture, quattro di Cyanobacterium aponinum e quattro di Chlorogloeopsis fritschii. Due colture di Cyanobacterium aponinum sono state fattie crescere prima a micromol fotoni/m^2/s per sei giorni e poi a 100 micromol fotoni/m^2/s per altri tre giorni, sempre in luce bianca. La stessa cosa è stata fatta per due campioni di Chlorogloeopsis fritschii. Due colture di Cyanobacterium aponinum sono state fattie crescere prima a micromol fotoni/m^2/s per sei giorni e poi a 100 micromol fotoni/m^2/s per altri tre giorni,con una radiazione che simulava quella di una stella di tipo M7 incidente su un pianeta terrestre. La stessa cosa è stata fatta per Chlorogloeopsis fritschii. La temperatura è stata mantenuta a 30°C per i campioni in luce bianca e fra 35°C e 38°C per gli esemplari illuminati con luce M7. La maggior temperatura nel secondo caso è stata dovuta al calore prodotto dai LED. Durante i tre giorni in cui i campioni sono stati sottoposti a 100 micromol fotoni/m^2/s sono state prese misure di densità ottica e calcolate le curve di crescita. Inoltre per ogni campione è stata calcolata la produzione di ossigeno. Infine i campioni sono stati analizzati anche dal punto di vista del cromatismo per capire come il loro colore fosse collegato alla vitalità
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Tice, Dane Steven. "Ground-based near-infrared remote sounding of ice giant clouds and methane." Thesis, University of Oxford, 2014. http://ora.ox.ac.uk/objects/uuid:4f09f270-a25c-4d36-96d3-13070a594eaa.

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The ice giants, Uranus and Neptune, are the two outermost planets in our solar system. With only one satellite flyby each in the late 1980’s, the ice giants are arguably the least understood of the planets orbiting the Sun. A better understanding of these planets’ atmospheres will not only help satisfy the natural scientific curiosity we have about these distant spheres of gas, but also might provide insight into the dynamics and meteorology of our own planet’s atmosphere. Two new ground-based, near-infrared datasets of the ice giants are studied. Both datasets provide data in a portion of the electromagnetic spectrum that provides good constraint on the size of small scattering particles in the atmospheres’ clouds and haze layers. The broad extent of both telescopes’ spectral coverage allows characterisation of these small particles for a wide range of wavelengths. Both datasets also provide coverage of the 825 nm collision-induced hydrogen-absorption feature, allowing us to disentangle the latitudinal variation of CH4 abundance from the height and vertical extent of clouds in the upper troposphere. A two-cloud model is successfully fitted to IRTF SpeX Uranus data, parameterising both clouds with base altitude, fractional scale height, and total opacity. An optically thick, vertically thin cloud with a base pressure of 1.6 bar, tallest in the midlatitudes, shows strong preference for scattering particles of 1.35 μm radii. Above this cloud lies an optically thin, vertically extended haze extending upward from 1.0 bar and consistent with particles of 0.10 μm radii. An equatorial enrichment of methane abundance and a lower cloud of constant vertical thickness was shown to exist using two independent methods of analysis. Data from Palomar SWIFT of three different latitude regions.
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Franks, Stewart William. "The representation of land surface - atmosphere fluxes for atmospheric modelling." Thesis, Lancaster University, 1997. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.387430.

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Rose, Kathleen A. "Environment "atmosphere" /." Online version of thesis, 1989. http://hdl.handle.net/1850/11084.

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Steiner, Allison L. "The influence of atmospheric chemistry and climate on atmosphere-biosphere interactions." Diss., Georgia Institute of Technology, 2003. http://hdl.handle.net/1853/25751.

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Eichelberger, Scott James. "The effects of meridional heating gradients on the atmospheric general circulation and its variability /." Thesis, Connect to this title online; UW restricted, 2005. http://hdl.handle.net/1773/10029.

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Geißler, Christoph, and Ch Jacobi. "Forcing of the Quarterdiurnal Tide." Universität Leipzig, 2018. https://ul.qucosa.de/id/qucosa%3A31792.

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Ensemble calculations for the period from 2000 to 2010 were carried out with the middle and upper atmosphere model (MUAM), and an analysis of the quarterdiurnal tide is performed. The global temporal and latitudinal distributions of the quarterdiurnal tide are modeled with MUAM, and their forcing mechanisms are examined. The quarterdiurnal tides show a similar distribution over the year in the northern and southern hemisphere, with maxima of the amplitude in late winter and spring as well as in autumn. In the latitude-height distribution is also shown that the largest amplitudes of the quarterdiurnal tide are seen at midlatitudes. Due to the decreasing density with height, there is a general increase of the tidal amplitudes with height. The results of the forcing analyses show that direct solar forcing is most important, but also that non-linear forcing and gravity wave interaction with other tides have a non-negligible influence on the quarterdiurnal tide in the middle and upper atmosphere.
Mit dem Modell für die mittlere und obere Atmosphäre MUAM wurden Ensemble-Berechnungen für den Zeitraum 2000 bis 2010 durchgeführt und die vierteltägigen Gezeiten analysiert. Es wird auf die globale zeitliche und räumliche Verteilung der vierteltägigen Gezeiten eingegangen und deren Anregungsmechanismen untersucht. Die vierteltägigen Gezeiten zeigen einen ähnlichen Verlauf über das Jahr auf der Nord- und Südhalbkugel mit Maxima der Amplitude im späten Winter und Frühjahr sowie im Herbst. Ein ähnliches Bild zeigt sich auch für die Verteilung im Breiten-Höhen-Schnitt, wo die größten Amplituden der vierteltätigen Gezeiten in den mittleren Breiten zu finden sind. Aufgrund der abnehmenden Dichte mit der Höhe ist eine allgemeine Zunahme der Amplituden mit der Höhe zu beobachten. Es zeigte sich, dass der direkte solare Antrieb am stärksten ausgeprägt ist, aber auch, dass der nichtlinearer Antrieb und die Interaktion von Schwerewellen mit anderen Gezeiten einen nicht zu vernachlässigenden Einfluss auf die vierteltägigen Gezeiten in der mittleren und oberen Atmosphäre haben.
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Sefcik, Lesley T. "Biophere-atmosphere interactions Northern hardwood seedling responses to anthropogenic atmospheric resource alteration." Saarbrücken VDM Verlag Dr. Müller, 2001. http://d-nb.info/988972131/04.

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Books on the topic "Atmosphere"

1

Schaefer, Vincent J. The atmosphere. Canada: Houghton Mifflin, 1990.

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Rees, M. H. Physics and chemistry of the upper atmosphere. Cambridge [Cambridgeshire]: Cambridge University Press, 1989.

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Desonie, Dana. Atmosphere. New York: Chelsea House, 2007.

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Lister, Anne. Atmosphere. Vancouver, BC: Program Services, Vancouver School Board, 1990.

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Copyright Paperback Collection (Library of Congress), ed. Atmosphere. New York: Leisure Books, 2002.

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B, Singh H., ed. Composition, chemistry, and climate of the atmosphere. New York: Van Nostrand Reinhold, 1995.

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United States. National Aeronautics and Space Administration, ed. Upper atmosphere research satellite: Remote atmospheric sensors. [Washington, D.C.?: National Aeronautics and Space Administration, 1989.

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F, Keeling Ralph, ed. The atmosphere. Amsterdam: Elsevier, 2006.

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Georgii, H. W. Von der Physik zur Chemie der freien Atmosphäre. Stuttgart: F. Steiner, 1995.

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Groves, Gerald Vann. A global reference atmosphere from 18 to 80 km. Hanscom AFB, MA: Atmospheric Sciences Division, Air Force Geophysics Laboratory, 1985.

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Book chapters on the topic "Atmosphere"

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Gooch, Jan W. "Atmosphere (Standard Atmosphere)." In Encyclopedic Dictionary of Polymers, 53. New York, NY: Springer New York, 2011. http://dx.doi.org/10.1007/978-1-4419-6247-8_879.

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Griffero, Tonino. "Atmosphere." In Lecture Notes in Morphogenesis, 45–47. Cham: Springer International Publishing, 2020. http://dx.doi.org/10.1007/978-3-030-51324-5_7.

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Gambaro, Andrea, Elena Gregoris, and Carlo Barbante. "Atmosphere." In Environmental Analysis by Electrochemical Sensors and Biosensors, 93–104. New York, NY: Springer New York, 2014. http://dx.doi.org/10.1007/978-1-4939-0676-5_4.

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Tawa, Michael. "Atmosphere." In Atmosphere, Architecture, Cinema, 117–55. Cham: Springer International Publishing, 2022. http://dx.doi.org/10.1007/978-3-031-13964-2_5.

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Sadraey, Mohammad H. "Atmosphere." In Aircraft Performance, 1–31. Boca Raton : CRC Press, [2016]: CRC Press, 2017. http://dx.doi.org/10.1201/9781315366913-1.

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Weik, Martin H. "atmosphere." In Computer Science and Communications Dictionary, 71. Boston, MA: Springer US, 2000. http://dx.doi.org/10.1007/1-4020-0613-6_951.

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Mercado, Gustavo. "atmosphere." In The Filmmaker's Eye: The Language of the Lens, 138–39. London; New York: Routledge, 2019.: Routledge, 2019. http://dx.doi.org/10.4324/9780429446894-47.

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Fink, A. H. "Atmosphere." In Impacts of Global Change on the Hydrological Cycle in West and Northwest Africa, 132–63. Berlin, Heidelberg: Springer Berlin Heidelberg, 2010. http://dx.doi.org/10.1007/978-3-642-12957-5_5.

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Taylor, Carol A., and Simone Fullagar. "Atmosphere." In A Glossary for Doing Postqualitative, New Materialist and Critical Posthumanist Research Across Disciplines, 34–35. London: Routledge, 2021. http://dx.doi.org/10.4324/9781003041153-18.

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Beer, Jürg, Ken McCracken, and Rudolf von Steiger. "Atmosphere." In Cosmogenic Radionuclides, 341–54. Berlin, Heidelberg: Springer Berlin Heidelberg, 2011. http://dx.doi.org/10.1007/978-3-642-14651-0_19.

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Conference papers on the topic "Atmosphere"

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Oakes, Jim. "Understanding Furnace Atmosphere Composition for Neutral and Gas Carburizing Applications." In HT 2015. ASM International, 2015. http://dx.doi.org/10.31399/asm.cp.ht2015p0229.

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Abstract Studying the gas composition of an atmosphere furnace reveals many parameters that can be used to predict metallurgical results of parts being processed. Today’s heat treaters strive for process consistency in order to eliminate variability, rework, and (in the worst case) scrap. In atmosphere heat treating, understanding control parameters and atmosphere composition provides critical insight into expected results. In this presentation, the audience will have the opportunity to observe gas compositions that would typically be found in carbon-neutral or carbon-rich atmospheres; they will also be able to see how atmospheric properties directly affect the metallurgical properties of heat treated parts. The presenter will illustrate examples of common atmospheres based on furnace types and will discuss common characteristics of improperly controlled atmospheres and how those atmospheres can lead to flawed results. Real-world examples of metallurgical results will be used to illustrate what can be expected from an “out of control” situation.
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Strow, L. Larrabee. "A Signal-Processing Approach for the Retrieval of Global Tropospheric CO Using the Atmospheric Infrared Sounder (AIRS)." In Optical Remote Sensing of the Atmosphere. Washington, D.C.: Optica Publishing Group, 1993. http://dx.doi.org/10.1364/orsa.1993.the.9.

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One goal of the Earth Observing Systems (EOS) is to measure concentrations of key atmospheric gases on a global scale in order to understand biogeochemical cycles in both the natural, unpolluted atmosphere, and in regions where anthropogenic activities have perturbed concentrations of gas-phase species. A particular concern in tropospheric chemistry is that increasing levels of carbon monoxide (CO) may lead to a decrease in atmospheric hydroxyl (OH) which would reduce the atmosphere's ability to scavenge other trace gases.
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Sadot, D. "Thermal imaging through the atmosphere: atmospheric MTF." In 16th Congress of the International Commission for Optics: Optics as a Key to High Technology. SPIE, 1993. http://dx.doi.org/10.1117/12.2308551.

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Tag, Benjamin, Takuya Goto, Kouta Minamizawa, Ryan Mannschreck, Haruna Fushimi, and Kai Kunze. "atmoSphere." In UbiComp '17: The 2017 ACM International Joint Conference on Pervasive and Ubiquitous Computing. New York, NY, USA: ACM, 2017. http://dx.doi.org/10.1145/3123024.3123190.

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Fushimi, Haruna, Daiya Kato, Youichi Kamiyama, Kazuya Yanagihara, Kouta Minamizawa, and Kai Kunze. "atmoSphere." In SIGGRAPH '17: Special Interest Group on Computer Graphics and Interactive Techniques Conference. New York, NY, USA: ACM, 2017. http://dx.doi.org/10.1145/3084822.3084845.

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Du, Ruofei, Kent R. Wills, Max Potasznik, and Jon E. Froehlich. "AtmoSPHERE." In CHI '15: CHI Conference on Human Factors in Computing Systems. New York, NY, USA: ACM, 2015. http://dx.doi.org/10.1145/2702613.2732771.

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Bahmann, Dirk. "Making Atmospheres." In Arts Research Africa 2022 Conference Proceedings. Arts Research Africa, 2022. http://dx.doi.org/10.54223/10539/35893.

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This paper discusses a practical methodology, developed for a second-year architectural elective project, that aims to make tangible the qualities of architectural atmospheres. It argues for an embodied practice of making sculptural artefacts. It proposes that these can articulate and make apparent atmospheric qualities. To be able to imagine or recognise atmosphere is a crucial skill for architects since atmosphere determines how people respond to space. The methodology is designed, through iterative cycles of making and critical reflection, to make students increasingly aware of atmosphere and develop their ability to create and articulate certain feeling tones within spaces. This artistic praxis relies upon a nonlinear, bodily knowing that seeks to challenge the dominance of ocularcentric practice in the discipline of architecture.
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Schwemmer, Geary, and Shane Addleman. "Injection Seeding a Multimode Alexandrite Laser Using a Frequency Stabilized Diode Laser." In Optical Remote Sensing of the Atmosphere. Washington, D.C.: Optica Publishing Group, 1990. http://dx.doi.org/10.1364/orsa.1990.tud28.

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Narrowband, frequency stable, pulsed laser sources are required for lidar remote sensing of atmospheric temperature, pressure, water vapor, minor species, or wherever narrow spectral features are essential for the measurement. Spaceborne lidar remote sensing systems require lasers with the highest efficiency possible, due to the constraints of limited power, weight, and size. In many instances, this implies a multi-spatial mode laser system. NASA’s Laboratory for Atmospheres has developed a differential absorption lidar system using pulsed multimode alexandrite lasers to measure atmospheric temperature profiles by measuring oxygen absorption on high J lines in the A band, near 770 nm. These spectral lines have a full width of 0.07 cm-1 at one atmosphere of pressure, and a full doppler width of 0.03 cm-1. This implies a requirement on the laser frequency stability and setting of approximately 0.001 cm-1. In this paper we describe the experimental development of a frequency stabilized diode laser and its use to injection seed a pulsed alexandrite laser.
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Longo, Francesco, and Giovanni Laneve. "Iterative atmospheric parameters estimation of the tropical atmosphere." In Remote Sensing, edited by Klaus Schaefer, Adolfo Comeron, Michel R. Carleer, and Richard H. Picard. SPIE, 2004. http://dx.doi.org/10.1117/12.511007.

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Lindner, Bernhard Lee. "Probing the Martian Atmosphere in the Ultraviolet." In Optical Remote Sensing of the Atmosphere. Washington, D.C.: Optica Publishing Group, 1993. http://dx.doi.org/10.1364/orsa.1993.tud.7.

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Several fundamental differences in atmospheric chemistry exist between Mars and the Earth. The martian atmosphere is primarily CO2 (95%), with strong vertical mixing, cold temperatures (typically 220K), low pressures (6 mb at the surface), high atmospheric dust and cloud particle content, and no man-made atmospheric constituents. Earlier difficulties in explaining why the atmosphere was not more decomposed into CO and O2 have been placated with models using updated reaction rates, 'moderate' eddy mixing of order 107 cm2s-1, and the odd hydrogen catalytic cycle (Shimazaki, 1989; Krasnopolsky, 1992). Odd nitrogen and sulfur catalytic cycles are of marginal importance, and other catalytic cycles shown to be important in the terrestrial atmosphere are unimportant on Mars (Yung et al., 1977; Krasnopolsky, 1992). Currently, much work is being undertaken to examine the importance of heterogeneous chemistry (e.g., Atreya and Blamont, 1990; Krasnopolsky, 1992), but uncertainties in particle properties make efficiencies difficult to evaluate. Also, atmospheric chemistry may significantly alter atmospheric composition on climatic timescales, particularly during periods of low obliquity (Lindner and Jakosky, 1985).
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Reports on the topic "Atmosphere"

1

Davis, K. J., S. J. Richardson, and N. L. Miles. Regional Ecosystem-Atmosphere CO2 Exchange Via Atmospheric Budgets. Office of Scientific and Technical Information (OSTI), March 2007. http://dx.doi.org/10.2172/900475.

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Stanley, Rachel H. R., Thomas Thomas, Yuan Gao, Cassandra Gaston, David Ho, David Kieber, Kate Mackey, et al. US SOLAS Science Report. Woods Hole Oceanographic Institution, December 2021. http://dx.doi.org/10.1575/1912/27821.

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The Surface Ocean – Lower Atmosphere Study (SOLAS) (http://www.solas-int.org/) is an international research initiative focused on understanding the key biogeochemical-physical interactions and feedbacks between the ocean and atmosphere that are critical elements of climate and global biogeochemical cycles. Following the release of the SOLAS Decadal Science Plan (2015-2025) (Brévière et al., 2016), the Ocean-Atmosphere Interaction Committee (OAIC) was formed as a subcommittee of the Ocean Carbon and Biogeochemistry (OCB) Scientific Steering Committee to coordinate US SOLAS efforts and activities, facilitate interactions among atmospheric and ocean scientists, and strengthen US contributions to international SOLAS. In October 2019, with support from OCB, the OAIC convened an open community workshop, Ocean-Atmosphere Interactions: Scoping directions for new research with the goal of fostering new collaborations and identifying knowledge gaps and high-priority science questions to formulate a US SOLAS Science Plan. Based on presentations and discussions at the workshop, the OAIC and workshop participants have developed this US SOLAS Science Plan. The first part of the workshop and this Science Plan were purposefully designed around the five themes of the SOLAS Decadal Science Plan (2015-2025) (Brévière et al., 2016) to provide a common set of research priorities and ensure a more cohesive US contribution to international SOLAS.
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Leacock, John. Neutron Propagation in Atmosphere. Office of Scientific and Technical Information (OSTI), October 2014. http://dx.doi.org/10.2172/1159564.

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Dorsey, Kathryn, and Daniel Feldman. Surface Atmosphere Integrated Field Laboratory. Office of Scientific and Technical Information (OSTI), October 2020. http://dx.doi.org/10.2172/1669356.

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Marland, G. (Chemistry of the global atmosphere). Office of Scientific and Technical Information (OSTI), September 1990. http://dx.doi.org/10.2172/6539398.

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Kayser, David C., William T. Chater, Charles K. Howey, and James B. Pranke. The Upper Atmosphere Composition Spectrometer. Fort Belvoir, VA: Defense Technical Information Center, September 1986. http://dx.doi.org/10.21236/ada175788.

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Ostashev, V. E., and G. H. Goedecke. Acoustic Tomography of the Atmosphere. Fort Belvoir, VA: Defense Technical Information Center, May 2007. http://dx.doi.org/10.21236/ada470885.

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Rogers, David P. Coupled Ocean-Atmosphere Interaction and the Development of the Marine Atmospheric Boundary Layer. Fort Belvoir, VA: Defense Technical Information Center, October 1997. http://dx.doi.org/10.21236/ada330047.

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Rogers, David P. Coupled Ocean-Atmosphere Interaction and the Development of the Marine Atmospheric Boundary Layer. Fort Belvoir, VA: Defense Technical Information Center, May 2000. http://dx.doi.org/10.21236/ada383683.

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Rogers, David P. Coupled Ocean-Atmosphere Interaction and the Development of the Marine Atmospheric Boundary Layer - Aasert. Fort Belvoir, VA: Defense Technical Information Center, September 1999. http://dx.doi.org/10.21236/ada629629.

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