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Observation of atmospheric neutrinos
Reviews of Modern Physics, 2001Atmospheric neutrinos arise from the decay of secondaries (π, K and μ) produced by primary cosmic-ray interactions in the atmosphere. In the energy range below 1GeV, where all secondaries decay, we roughly expect that (v μ + v μ )/(v e + v e ) ≃2. This is because a π-decay produces a v μ and a μ; the μ, when it decays, produces another v μ and a v e ...
Takaaki Kajita, Yoji Totsuka
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Atmospheric glories: simulations and observations
Applied Optics, 2005Mie theory can be used to provide full-color simulations of atmospheric glories. Comparison of such simulations with images of real glories suggests that most glories are caused by spherical water droplets with radii between 4 and 25 microm. This paper also examines the appearance of glories taking into account the size of the droplets and the width of
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Observations by Atmospheric Radar
2013Atmospheric radars are capable of continuously monitoring echo power spectrum in the vicinity of the zenith. From the spectrum, echo intensity, Doppler velocity, and velocity spectrum width are derivable over the wide altitude range 1–100 km in the Earth’s atmosphere. In this chapter, observations by atmospheric radar are discussed.
Shoichiro Fukao, Kyosuke Hamazu
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Atmospheric Changes and Observations
2019Earth’s atmosphere is usually air layer of the solid Earth outer, which is an important part of the Earth’s natural environment. It is the condition indispensable to the survival of life on Earth and also protective for life on Earth. With developments and advances in space technologies, human activities are involving into the upper atmosphere and ...
Shuanggen Jin, R. Jin, X. Liu
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2003
The aim of this chapter is to give an overview of the techniques used to observe the atmosphere, and the physical principles involved. In particular, we attempt to highlight characteristics of different observation types that need to be taken into account when using them in an atmospheric data assimilation system.
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The aim of this chapter is to give an overview of the techniques used to observe the atmosphere, and the physical principles involved. In particular, we attempt to highlight characteristics of different observation types that need to be taken into account when using them in an atmospheric data assimilation system.
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Atmospheric turbulence and surface atmospheric electricity observations
2004Durable and low maintenance atmospheric electricity sensors are required if measurements which span long (year to decade) timescales are to be obtained. A passive spherical sensor, together with a high impedance electrometer, presents one method of monitoring the vertical Potential Gradient at the surface.
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Satellite Observations of Atmospheric Water Vapor
Applied Optics, 1974Observations in the spectral window at 11-12 microm, in the carbon dioxide band at 13.3-13.4 microm, and in the water vapor rotation band at 18.7-18.8 microm have been made by the satellite infrared spectrometer and the vertical temperature profile radiometer on the Nimbus 4 and NOAA-2 satellites.
D Q, Wark, J H, Lienesch, M P, Weinreb
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Mid-ocean observations of atmospheric radiation
Quarterly Journal of the Royal Meteorological Society, 1979AbstractMid‐ocean (35°N 155°W) observations of the various components of radiative flux were made from the R/P FLIP during the period 2 through 13 February 1974. Cloud cover ranged from clear skies to overcast, and water vapour pressure varied between 9 and 18 mb, with sea surface temperature near 15.0°C.The net longwave radiative fluxes reported here ...
James J. Simpson, Clayton A. Paulson
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Titan's atmosphere from voyager infrared observations
Icarus, 1989Abstract We have studied the 900–1200 cm−1 range in three different selections of ∼30 Voyager 1 IRIS spectra recorded in Titan's equatorial region. In particular, we have reanalyzed the 8.6-μm emission feature attributed to both C3H8 and CH3D bands. Observations were compared to synthetic spectra generated from an atmospheric model which incorporates
A. Coustenis, B. Bézard, D. Gautier
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Observing Through Atmospheric Turbulence
2010Astronomical observations from the ground are limited in sensitivity – not so much in performance – by atmospheric turbulence. Removing the sensitivity limit by observing a reference star close to the object of interest, to freeze the turbulence and to permit long integration times, one is then restricted to a small field of less than 1 arcmin around ...
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