Observation of radio eclipses of the moon at millimeter wavelengths

Kamenskaya, S. A.; Kislyakov, A. G.; Krotikov, V. D.; Naumov, A. P.; Nikonov, V. N.; Porfir'ev, V. A.; Plechkov, V. M.; Strezhneva, K. M.; Troltskii, V. S.; Fedoseev, L. I.; Lubyako, L. V.; Sorokina, E. P.

doi:10.1007/bf01038602

Cited by 3 publications

(8 citation statements)

References 3 publications

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“…Therefore, nothing could be concluded from them. Kamenskaya et al (1965), however, was in much better agreement with the values obtained at 300 GHz by Baldock et al (1965), than Low & Davidson (1965) were.…”

Section: Comparison With Ground-based Measurementssupporting

confidence: 68%

“…On the basis of our simulations of brightness temperatures as shown in Table 5 and Figure 4, we expect ( ) DT T B B max almost everywhere on the lunar surface to be similar to its diskaveraged value-an assumption made already by Kamenskaya et al (1965). The TSIs for the locations displayed in Table 5 are shown in Figure 5.…”

Section: Local and Disk-integrated Temperature Dropsupporting

confidence: 54%

“…Later in that year, a partial eclipse was observed at the same frequency and a temperature drop of 7% was reported (Tyler & Copeland 1961). In order to shed light on this tangle, Baldock et al (1965), Kamenskaya et al (1965), andLow &Davidson (1965) observed radio eclipses of the Moon in 1963 and 1964. Again, no agreement was reached: Low & Davidson (1965) gave a maximum temperature drop at 250 GHz that was less than half of what Kamenskaya et al (1965) claimed at the same frequency.…”

Section: Comparison With Ground-based Measurementsmentioning

confidence: 86%

“…In order to shed light on this tangle, Baldock et al (1965), Kamenskaya et al (1965), andLow &Davidson (1965) observed radio eclipses of the Moon in 1963 and 1964. Again, no agreement was reached: Low & Davidson (1965) gave a maximum temperature drop at 250 GHz that was less than half of what Kamenskaya et al (1965) claimed at the same frequency. Linsky (1966) noted that the data of Low & Davidson and the 1.2 mm data of Kamenskaya et al disagreed significantly with each other and with predictions of all the models.…”

Section: Comparison With Ground-based Measurementsmentioning

confidence: 99%

“…Previous observers of eclipses at frequencies between 200 and 250 GHz have reported values for the temperature drop spanning a range from 10% to 45%. The causes of the wide range of measured values are both random errors, for example related to the subtraction of the atmospheric contribution, and systematic effects, for example related to the very different kinds of equipment and technologies from several decades ago: Kamenskaya et al (1965) struggled with irregular variations of the reference signal due to side-lobe reception, and Sandor & Clancy (1995), 30 yr later, still reported actual absolute calibration errors of up to 10%. The calibration of AMSU-B, on the other hand, has an absolute accuracy better than ±2 K after bias correction, at least in the first few years of the operational phase (Atkinson 2001).…”

Section: Introductionmentioning

confidence: 99%

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Observation of a Lunar Eclipse at 89, 150, and 183 GHz

et al. 2023

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We describe the measurement of the brightness temperature of the Moon from space during a total lunar eclipse by using a microwave sounder aboard a weather satellite. Previous observations of lunar eclipses were inconsistent and did not cover the frequency range between 100 and 200 GHz. In this work, we seek to establish a reliable relationship between frequency and drop in brightness temperature during a total eclipse for millimeter wavelengths. For this purpose, we chose the eclipse on 2004 October 28, because it coincided with appearances of the Moon in the deep space view of the Advanced Microwave Sounding Unit-B on NOAA-15. It was therefore possible to measure its disk-integrated radiance at 89, 150, and 183 GHz at 100 minutes intervals. Our observations are, to the best of our knowledge, the only ones between 100 and 200 GHz, and demonstrate the nearly linear dependency on frequency of the maximum relative drop in effective temperature during an eclipse. The slope of this function is m = 0.00114 ± 0.00017 GHz−1 in the range 88–300 GHz. The good agreement between the variations of the effective lunar temperature and a new radiative-transfer model suggests that the Moon is suitable as a flux standard for microwave observations with beam sizes larger than 0.5°.

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Section: Comparison With Ground-based Measurementssupporting

confidence: 68%

Section: Local and Disk-integrated Temperature Dropsupporting

confidence: 54%

Section: Comparison With Ground-based Measurementsmentioning

confidence: 86%

Section: Comparison With Ground-based Measurementsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Observation of a Lunar Eclipse at 89, 150, and 183 GHz

et al. 2023

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Observations of the total lunar eclipse on February 10, 1971 at 3.1 mm wavelength

Ulich

1972

Icarus

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Remote Probing of the Moon by Infrared and Microwave Emissions and by Radar

Hagfors¹

1970

Radio Science

138

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The results of the remote probing of the moon by means of infrared and microwave emissions and by radar are reviewed. Also, we discuss how the various observational results can help to explain physical parameters of the lunar surface, such as thermal and electrical conductivities, dielectric constant, density, particle sizes in the lunar regolith, depth of the surface layer, roughness of the surface, variation of these parameters from point to point on the surface, and amount of heat generated in the lunar interior. 190 T. HAGFORS ' at several different phase angles in order to obtain maps of isotherms on the moon. The resolution used was 25 seconds of arc as compared with the diameter of the moon which is about 30 minutes of arc. The data in the figure were obtained from the thermal contours at a few different phase angles. The data ascribed to Saari and Shorthill [1967] were obtained in a wavelength interval from 10 to 12t• with an instrument having an angular resolution of 8 seconds of arc. The post-sunset data were obtained by Murray and Wildey [1964] at 8-13t• with a resolution of 26 seconds of arc and by Shorthill and Saari [1965] at 10-12tz with their higher resolution instrument. The pre-sunrise observations are particularly difficult to make because of the high sensitivity required. Having special instrumentation Low [ 1965] was able to determine the pre-sunrise temperature by scanning over the cold limb of the moon at a wavelength of 20t•. He found an average pre-dawn temperature of 90øK and also observed colder localized areas with temperatures down to 70øK.

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Observation of radio eclipses of the moon at millimeter wavelengths

Cited by 3 publications

References 3 publications

Observation of a Lunar Eclipse at 89, 150, and 183 GHz

Observation of a Lunar Eclipse at 89, 150, and 183 GHz

Observations of the total lunar eclipse on February 10, 1971 at 3.1 mm wavelength

Remote Probing of the Moon by Infrared and Microwave Emissions and by Radar

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