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br-j01
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 .
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br-j01
Of the remaining planets , only Mars and Saturn have been observed as radio sources , and not very much information is available .
<NONE>
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br-j01
Mars has been observed twice at about 3 - cm wave length , and the intensity of the observed radiation is in reasonable agreement with the thermal radiation which might be predicted on the basis of the known temperature of Mars .
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br-j01
The low intensity of the radiation from Saturn has limited observations , but again the measured radiation seems to be consistent with a thermal origin .
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br-j01
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 .
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br-j01
In spite of this , the very large radio reflectors and improved amplifying techniques which are now becoming available should make it possible to observe the radio emission of most of the planets in a few years .
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br-j01
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).
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br-j01
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).
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br-j01
They deduced from their measurements that the radio emission from the whole disk of the moon varied during a lunation in a roughly sinusoidal fashion; 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); 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 .
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br-j01
Piddington and Minnett explained their observations by pointing out that rocklike materials which are likely to make up the surface of the moon would be partially transparent to radio waves , although opaque to infrared radiation .
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br-j01
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 .
<NONE>
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br-j01
Since the absorption of radio waves in rocklike material varies with wave length , it should be possible to sample the temperature variation at different depths beneath the surface and possibly detect changes in the structure or composition of the lunar surface material .
<NONE>
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br-j01
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 .
<NONE>
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br-j01
This sporadic type of planetary radiation is discussed by Burke (chap. 13) and Gallet (chap. 14).
<NONE>
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br-j01
Steady radiation which was presumably of thermal origin was observed from Venus at 3.15 and 9.4 cm , and from Mars and Jupiter at 3.15 cm in 1956 (Mayer , McCullough , and Sloanaker , 1958 a , b , c), and from Saturn at 3.75 cm in 1957 (Drake and Ewen , 1958).
<NONE>
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br-j01
In the relatively short time since these early observations , Venus has been observed at additional wave lengths in the range from 0.8 to 10.2 cm , and Jupiter has been observed over the wave-length range from 3.03 to 68 cm .
<NONE>
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br-j01
The observable characteristics of planetary radio radiation are the intensity , the polarization , and the direction of arrival of the waves .
<NONE>
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br-j01
The maximum angular diameter of any planetary disk as observed from the earth is about 1 minute of arc .
<NONE>
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br-j01
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 .
<NONE>
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br-j01
It should be possible , however , to put useful limits on the diameters of the radio sources by observing with large reflectors or with interferometers .
<NONE>
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br-j01
Measurements of polarization are presently limited by apparatus sensitivity and will remain difficult because of the low intensity of the planetary radiation at the earth .
<NONE>
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br-j01
There have been few measurements specifically for the determination of the polarization of planetary radiation .
<NONE>
<NONE>
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br-j01
The measurements made with the NRL 50 - foot reflector , which is altitude azimuth mounted , would have shown a systematic change with local hour angle in the measured intensities of Venus and Jupiter if a substantial part of the radiation had been linearly polarized .
<NONE>
<NONE>
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br-j01
Recent interferometer measurements (Radhakrishnan and Roberts , 1960) have shown the 960 - Mc emission of Jupiter to be partially polarized and to originate in a region of larger diameter than the visible disk .
<NONE>
<NONE>
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br-j01
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 .
<NONE>
<NONE>
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br-j01
The concept of apparent black-body temperature is used to describe the radiation received from the moon and the planets .
<NONE>
<NONE>
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br-j01
The received radiation is compared with the radiation from a hypothetical black-body which subtends the same solid angle as the visible disk of the planet .
<NONE>
<NONE>
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br-j01
The apparent black-body disk temperature is the temperature which must be assumed for the black body in order that the intensity of its radiation should equal that of the observed radiation .
<NONE>
<NONE>
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br-j01
The use of this concept does not specify the origin of the radiation , and only if the planet really radiates as a black body , will the apparent black-body temperature correspond to the physical temperature of the emitting material .
<NONE>
<NONE>
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br-j01
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 .
<NONE>
<NONE>
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br-j01
The quiescent level of centimeter wave-length solar radiation would increase the average disk brightness temperature by less than 1 ` K .
<NONE>
<NONE>
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br-j01
At meter wave lengths and increase of the order of 10 ` K in the average disk temperatures of the nearer planets would be expected .
<NONE>
<NONE>
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br-j01
Therefore , neglecting the extreme outbursts , reflected solar radiation is not expected to cause sizable errors in the measurements of planetary radiation in the centimeter - and decimeter wave-length range .
<NONE>
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br-j01
Radio observations of the moon have been made over the range of wave lengths from 4.3 mm to 75 cm , and the results are summarized in Table 1 .
<NONE>
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br-j01
Observations have also been made at 1.5 mm using optical techniques (Sinton , 1955 , 1956 ,; see also chap. 11).
<NONE>
<NONE>
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br-j01
Not all the observers have used the same procedures or made the same assumptions about the lunar brightness distribution when reducing the data , and this , together with differences in the methods of calibrating the antennae and receivers , must account for much of the disagreement in the measured radio brightness temperatures .
<NONE>
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br-j01
In the observations at 4.3 mm (Coates , 1959 a), the diameter of the antenna beam , 6 ' .7 , was small enough to allow resolution of some of the larger features of the lunar surface , and contour diagrams have been made of the lunar brightness distribution at three lunar phases .
<NONE>
<NONE>
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br-j01
These observations indicate that the lunar maria heat up more rapidly and also cool off more rapidly than do the mountainous regions .
<NONE>
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br-j01
Mare Imbrium seems to be an exception and remains cooler than the regions which surround it .
<NONE>
<NONE>
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br-j01
These contour diagrams also suggest a rather rapid falloff in the radio brightness with latitude .
<NONE>
<NONE>
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br-j01
Very recently , observations have been made at 8 - mm wave length with a reflector 22 meters in diameter with a resultant beam width of only about 2 ' (Amenitskii , Noskova , and Salomonovich , 1960).
<NONE>
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br-j01
The constant temperature contours are much smoother than those observed at 4.3 mm by Coates (1959 a), and apparently the emission at 8 mm is not nearly so sensitive to differences in surface features .
<NONE>
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br-j01
Such high-resolution observations as these are needed at several wave lengths in order that the radio emission of the moon can be properly interpreted .
<NONE>
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br-j01
The observations of Mayer , McCullough , and Sloanaker at 3.15 cm and of Sloanaker at 10.3 cm have not previously been published and will be briefly described .
<NONE>
<NONE>
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br-j01
Measurements at 3.15 cm were obtained on 11 days spread over the interval May 3 to June 19 , 1956 , using the 50 - foot reflector at the U.S. Naval Research Laboratory in Washington .
<NONE>
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br-j01
The half-intensity diameter of the antenna beam was about 9 ' , and the angle subtended by the moon included the entire main beam and part of the first side lobes .
<NONE>
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br-j01
The antenna patterns and the power gain at the peak of the beam were both measured (Mayer , McCullough , and Sloanaker , 1958 b), so that the absolute power sensitivity of the antenna beam over the solid angle of the moon was known .
<NONE>
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br-j01
The ratio of the measured antenna temperature change during a drift scan across the moon to the average brightness temperature of the moon over the antenna beam (assuming that the brightness temperature of the sky is negligible) was found , by graphical integration of the antenna directivity diagram , to be 0.85 .
<NONE>
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br-j01
The measured brightness temperature is a good approximation to the brightness temperature at the center of the lunar disk because of the narrow antenna beam and because the temperature distribution over the central portion of the moon 's disk is nearly uniform .
<NONE>
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br-j01
The result of the observations is (in ` K) **f where the phase angle , |qt , is measured in degrees from new moon and the probable errors include absolute as well as relative errors .
<NONE>
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br-j01
This result is plotted along with the 8.6 - mm observations of Gibson (1958) in figure 1 , a .
<NONE>
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br-j01
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).
<NONE>
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br-j01
In the discussion which follows , the time average of the radio emission will be referred to as the constant component , and the superimposed periodic variation will be called the variable component .
<NONE>
<NONE>
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br-j01
The 10.3 - cm observation of Sloanaker was made on May 20 , 1958 , using the 84 - foot reflector at the Maryland Point Observatory of the U.S. Naval Research Laboratory .
<NONE>
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br-j01
The age of the moon was about 2 days .
<NONE>
<NONE>
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br-j01
The half-intensity diameter of the main lobe of the antenna was about 18 ' .5 , and the brightness temperature was reduced by assuming a Gaussian shape for the antenna beam and a uniformly bright disk for the moon .
<NONE>
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br-j02
Experiments were made on an electric arc applying a porous graphite anode cooled by a transpiring gas (Argon).
<NONE>
<NONE>
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br-j02
Thus , the energy transferred from the arc to the anode was partly fed back into the arc .
<NONE>
<NONE>
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br-j02
It was shown that by proper anode design the net energy loss of the arc to the anode could be reduced to approximately 15% of the total arc energy A detailed energy balance of the anode was established .
<NONE>
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br-j02
The anode ablation could be reduced to a negligible amount .
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br-j02
The dependence of the arc voltage upon the mass flow velocity of the transpirating gas was investigated for various arc lengths and currents between 100 Amp and 200 Amp .
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br-j02
Qualitative observations were made and high-speed motion pictures were taken to study flow phenomena in the arc at various mass flow velocities .
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br-j02
The high heat fluxes existing at the electrode surfaces of electric arcs necessitate extensive cooling to prevent electrode ablation .
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br-j02
The cooling requirements are particularly severe at the anode .
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br-j02
In free burning electric arcs , for instance , approximately 90% of the total arc power is transferred to the anode giving rise to local heat fluxes in excess of **f as measured by the authors - the exact value depending on the arc atmosphere .
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br-j02
In plasma generators as currently commercially available for industrial use or as high temperature research tools often more than 50% of the total energy input is being transferred to the cooling medium of the anode .
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br-j02
The higher heat transfer rates at the anode compared with those at the cathode can be explained by the physical phenomena occurring in free burning arcs .
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br-j02
In plasma generators the superimposed forced convection may modify the picture somewhat .
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br-j02
The heat transfer to the anode is due to the following effects: 1 .
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br-j02
Heat of condensation (work function) plus kinetic energy of the electrons impinging on the anode .
<NONE>
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br-j02
This energy transfer depends on the current , the temperature in the arc column , the anode material , and the conditions in the anode sheath .
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br-j02
2 .
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br-j02
Heat transfer by molecular conduction as well as by radiation from the arc column .
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br-j02
The heat transfer to the anode in free burning arcs is enhanced by a hot gas jet flowing from the cathode towards the anode with velocities up **f .
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br-j02
This phenomenon has been experimentally investigated in detail by Maecker (Ref. 1).
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br-j02
The pressure gradient producing the jet is due to the nature of the magnetic field in the arc (rapid decrease of current density from cathode to the anode).
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br-j02
Hence , the flow conditions at the anode of free burning arcs resemble those near a stagnation point .
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br-j02
it is apparent from the above and from experimental evidence that the cooling requirements for the anode of free burning arcs are large compared with those for the cathode .
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br-j02
The gas flow through a plasma generator will modify these conditions; however , the anode is still the part receiving the largest heat flux .
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br-j02
An attempt to improve the life of the anodes or the efficiency of the plasma generators must , therefore , aim at a reduction of the anode loss .
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br-j02
The following possibilities exist for achieving this: 1 .
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br-j02
The use of high voltages and low currents by proper design to reduce electron heat transfer to the anode for a given power output .
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br-j02
2 .
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br-j02
Continuous motion of the arc contact area at the anode by flow or magnetic forces .
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br-j02
3 .
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br-j02
Feed back of the energy transferred to the anode by applying gas transpiration through the anode .
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br-j02
The third method was , to our knowledge , successfully applied for the first time by C. Sheer and co-workers (Ref. 2).
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br-j02
The purpose of the present study is to study the thermal conditions and to establish an energy balance for a transpiration cooled anode as well as the effect of blowing on the arc voltage .
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br-j02
Gas injection through a porous anode (transpiration cooling) not only feeds back the energy transferred to the anode by the above mentioned processes , but also modifies the conditions in the arc itself .
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br-j02
A detailed study of this latter phenomenon was not attempted in this paper .
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br-j02
Argon was used as a blowing gas to exclude any effects of dissociation or chemical reaction .
<NONE>
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br-j02
The anode material was porous graphite .
<NONE>
<NONE>
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br-j02
Sintered porous metals should be usable in principle .
<NONE>
<NONE>
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br-j02
However , technical difficulties arise by melting at local hot spots .
<NONE>
<NONE>
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br-j02
The experimental arrangement as described below is based on the geometry of free burning arcs .
<NONE>
<NONE>
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br-j02
Thus , direct comparisons can be drawn with free burning arcs which have been studied in detail during the past years and decades by numerous investigators (Ref. 3).
<NONE>
<NONE>
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br-j02
Figures 1 to 3 show photographic and schematic views of the test stand and of two different models of the anode holder .
<NONE>
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br-j02
The cathode consisted of a 1/4 '' diameter thoriated tungsten rod attached to a water cooled copper tube .
<NONE>
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br-j02
This tube could be adjusted in its axial direction by an electric drive to establish the required electrode spacing .
<NONE>
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br-j02
The anode in figure 2 was mounted by means of the anode holder which was attached to a steel plug and disk .
<NONE>
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