The observed intensity of the radio emission of Venus is much higher than the expected thermal intensity, although the spectrum indicated by measurements at wave lengths near 3 cm and 10 cm is like that of a black body at about 600-degrees.

The study of the radio emission of the moon and planets began with the detection of the thermal radiation of the moon at 1.25-cm wave length by Dicke and Beringer ( 1946 ).

This was followed by a comprehensive series of observations of the 1.25-cm emission of the moon over three lunar cycles by Piddington and Minnett ( 1949 ).

that the amplitude of the variation was considerably less than the amplitude of the variation in the infrared emission as measured by Pettit and Nicholson ( 1930 ) and Pettit ( 1935 ) ; ;

The constant-temperature contours are much smoother than those observed at 4.3 mm by Coates ( 1959 ) and apparently the emission at 8 mm is not nearly so sensitive to differences in surface features.

The input light distributions considered are P-11 and P-20 phosphor emission and the so-called `` night light '' ( N.L. ) as given by H.W. Babcock and J. J. Johnson.

Naturally occurring with a half-life of 1. 25 years, decays to stable ( 11. 2 %) by electron capture or positron emission, and also to stable ( 88. 8 %) via beta decay.

In the subsurface environment, it is also produced through neutron capture by or alpha emission by calcium.

It decays by emission of a α-particle to < sup > 237 </ sup > Np ; the half-life of this decay was first determined as 510 ± 20 years but then corrected to 432. 2 years.

Even touching an alpha source is usually not harmful, though many alpha sources also are accompanied by beta-emitting radio daughters, and alpha emission is also accompanied by gamma photon emission.

( b ) illustrates the same process using spectroscopic notation,. The Auger effect () is a physical phenomenon in which the filling of an inner-shell vacancy of an atom is accompanied by the emission of an electron from the same atom.

Auger electron spectroscopy involves the emission of Auger electrons by bombarding a sample with either X-rays or energetic electrons and measures the intensity of Auger electrons as a function of the Auger electron energy.

The Auger emission process was discovered in 1922 by Lise Meitner, an Austrian-Swedish physicist, as a side effect in her competitive search for the nuclear beta electrons with the British physicist Charles Drummond Ellis.

This process forms an atomized form of the analyte, which can then be measured by absorption or emission spectrometry.

In LS AAS the high resolution that is required for the measurement of atomic absorption is provided by the narrow line emission of the radiation source, and the monochromator simply has to resolve the analytical line from other radiation emitted by the lamp.

The advantage of this technique is that total and background absorption are measured with the same emission profile of the same lamp, so that any kind of background, including background with fine structure can be corrected accurately, unless the molecule responsible for the background is also affected by the magnetic field ; the disadvantage is the increased complexity of the spectrometer.

Arcturus is a type K1. 5 IIIpe orange giant star — the letters " pe " stand for " peculiar emission ," which indicates that the spectrum of light given off by the star is unusual and full of emission lines.

This emission can be observed, for example, after dispersing berkelium ions in a silicate glass, by melting the glass in presence of berkelium oxide or halide.

* In Ghent, first recorded instance of emission of life annuities by a town in the Low Countries, this event confirms a trend of consolidation of local public debt in north-western Europe initiated in 1218 by Rheims.

For the case of Jupiter, the radio emission spectrum is definitely not like the spectrum of a black-body radiator, and it seems very likely that the radiation reaching the earth is a combination of thermal radiation from the atmosphere and non-thermal components.

No attempts to measure the radio emission of the remaining planets have been reported, and, because of their distances, small diameters, or low temperatures, the thermal radiation at radio wave lengths reaching the earth from these sources is expected to be of very low intensity.

and that the maximum of the radio emission came about 3-1/2 days after Full Moon, which is again in contrast to the infrared emission, which reaches its maximum at Full Moon.

The infrared emission could then be assumed to originate at the surface of the moon, while the radio emission originates at some depth beneath the surface, where the temperature variation due to solar radiation is reduced in amplitude and shifted in phase.

This is much smaller than the highest resolution of even the very large reflectors now under construction, and consequently the radio emission of different regions of the disk cannot be resolved.

Other than this very significant result, most of the information now available about the radio emission of the planets is restricted to the intensity of the radiation.

The radio radiation of the sun which is reflected from the moon and planets should be negligible compared with their thermal emission at centimeter wave lengths, except possibly at times of exceptional outbursts of solar radio noise.

The variation in the 3-cm emission of the moon during a lunation is very much less than the variation in the 8.6-mm emission, as would be expected from the explanation of Piddington and Minnett ( 1949 ).

It is obvious that the careful choice of photocathode which maximizes Af for a given input E ( in the case of the second stage, for the first phosphor screen emission ) is very important.

( The P-20 input is of interest because it corresponds roughly to the light emission of conventional X-ray fluorescent screens ).

The second longest-lived isotope of astatine, astatine-211, is the only one currently having any commercial application, being employed in medicine to diagnose and treat some diseases via its emission of alpha particles ( helium-4 nuclei ).

The radio emission of a planet was first detected in 1955, when Burke and Franklin ( 1955 ) identified the origin of interference-like radio noise on their records at about 15 meters wave length as emission from Jupiter.

Gamow solved a model potential for the nucleus and derived, from first principles, a relationship between the half-life of the decay, and the energy of the emission, which had been previously discovered empirically, and was known as the Geiger – Nuttall law.

This reaction was studied for the first time in 2008 by the team at RIKEN, Japan, in order to study the decay properties of < sup > 266 </ sup > Bh, which is a decay product in their claimed decay chains of ununtrium .< ref > The decay of < sup > 266 </ sup > Bh by the emission of 9. 05-9. 23 MeV alpha particles was further confirmed in 2010.

In the Clean Development Mechanism, only afforestation and reforestation are eligible to produce certified emission reductions ( CERs ) in the first commitment period of the Kyoto Protocol ( 2008 – 2012 ).

A low-intensity double-slit experiment was first performed by G. Taylor in 1909, by reducing the level of incident light until photon emission / absorption events were mostly nonoverlapping.

In 1917, Albert Einstein established the theoretical foundations for the laser and the maser in the paper Zur Quantentheorie der Strahlung ( On the Quantum Theory of Radiation ); via a re-derivation of Max Planck ’ s law of radiation, conceptually based upon probability coefficients ( Einstein coefficients ) for the absorption, spontaneous emission, and stimulated emission of electromagnetic radiation ; in 1928, Rudolf W. Ladenburg confirmed the existences of the phenomena of stimulated emission and negative absorption ; in 1939, Valentin A. Fabrikant predicted the use of stimulated emission to amplify “ short ” waves ; in 1947, Willis E. Lamb and R. C. Retherford found apparent stimulated emission in hydrogen spectra and effected the first demonstration of stimulated emission ; in 1950, Alfred Kastler ( Nobel Prize for Physics 1966 ) proposed the method of optical pumping, experimentally confirmed, two years later, by Brossel, Kastler, and Winter.

In 1939, Valentin A. Fabrikant predicted the use of stimulated emission to amplify " short " waves ; In 1947, Willis E. Lamb and R. C. Retherford found apparent stimulated emission in hydrogen spectra and effected the first demonstration of stimulated emission ; in 1950, Alfred Kastler ( Nobel Prize for Physics 1966 ) proposed the method of optical pumping, experimentally confirmed, two years later, by Brossel, Kastler, and Winter.

Plato first articulated the emission theory, the idea that visual perception is accomplished by rays emitted by the eyes.

Stimulated emission was first observed in the microwave region of the electromagnetic spectrum, giving rise to the acronym MASER for Microwave Amplification by Stimulated Emission of Radiation.

The first formulation of a quantum theory describing radiation and matter interaction is due to British scientist Paul Dirac, who, during the 1920s, was first able to compute the coefficient of spontaneous emission of an atom.

The parties also began discussing the post-Kyoto mechanism, on how to allocate emission reduction obligation following 2012, when the first commitment period ends.

At the beginning of the 11th Century, the Arabic scientist Alhazen wrote the first comprehensive treatise on optics ; describing refraction, reflection, and the operation of a pinhole lens via rays of light traveling from the point of emission to the eye.

They were the first to notice bright spectral emission lines when viewing the limb of the Sun without the aid of a total solar eclipse.