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Lunar differential flux scans at 22 microns

Profile image of Wendell MendellWendell Mendell

1972

Abstract

The nighttime lunar surface has been scanned at a variety of phases both before and after new Moon. A differential chopping technique was used which records the flux difference between adjacent resolution elements along a scan. In principle the differential scan can be integrated to provide the flux distribution, but slow drifts in the sensor null level frustrated this procedure. However, some cold limb temperatures have been calculated using the planet Jupiter for calibration. The measurements were made with a resolution element of 27 arc seconds on the 28-inch telescope at the University of Arizona. Scan positions were determined by noting features on the illuminated portion of the Moon through a bore-sighted guide telescope. Positional accuracies are within two reso¬ lution elements. The technique is particularly sensitive to the detection of nighttime anomalies, and more than 150 of these have been identified. Prior to new Moon is seen large scale thermal structure, correspondin...

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References (46)

  1. Adams, John B., and Robert L. Jones, Spectral Reflectivity of Lunar Samples, Science, 167, 737, 1970.
  2. Allen, D. A., and E. P. Ney, Lunar Thermal Anomalies: Infrared Observations, Science, 164, 419, 1969.
  3. Armstrong, Ken, Infrared Radiometry of the Planets, Masters Thesis, Space Science Dept., Rice University, 1971.
  4. Ashby, Neil, Energy Balance on the Lunar Surface, Publ. of the Astron. Soc. of the Pacific, 78, 254, 1966.
  5. Carslaw, H. S., and J. C. Jaeger, Conduction of Heat in Solids, Oxford University Press, 1959.
  6. Dicke, R. H., and R. Beringer, Microwave Radiation from the Sun and Moon, Astrophys. J., 103, 375, 1946.
  7. Geoffrion, Ann R., Majorie Korner, and William M. Sinton, Isothermal Contours of the Moon, Lowe11 Observatory Bull., 5, 1, 1960.
  8. Jaeger, J. C., and A. F. A. Harper, Nature of the Surface of the Moon, Nature, 166, 1026, 1950.
  9. Jaeger, J. C., The Surface Temperature of the Moon, Australian Jour, of Physics, _6, 10, 1953.
  10. Krotikov, V. D., and 0. B. Shchuko, The Heat Balance of the Lunar Surface Layer During a Lunation, Soviet Astron. - AJ, l_ a 228, 1963 (English Translation).
  11. Linsky, Jeffrey L., Models of the Lunar Surface Including Temperature-Dependent Thermal Properties, Harvard College Observatory Scientific Report No. _8, 1966.
  12. Low, Frank J., Low-Temperature Germanium Bolometer, J. O. _S. A., 51, 1300, 1961.
  13. Low, Frank J., Lunar Observations atX = 10/u and 1.2 mm., Astron. J. , 6_9, 143, 1964.
  14. Low, Frank J., Lunar Nighttime Temperatures Measured at 20 Microns, Astrophys. J., 142, 806, 1965.
  15. Low, F. J., Thermal Detection Radiometry at Short Milli¬ meter Wavelengths, Proc. IEEE, 54, .477, 1966.
  16. Low, F. J., and W. W. Mendell, Lunar Infrared Flux Measure¬ ments at 22 Microns, paper presented at the Planetary Subgroup of the American Astronomical Society, Austin, Texas, December, 1968.
  17. Maxwell, A. D., Correction of the Variation per Hour of the Moon's Declination for Rate of Change of Parallax and Refraction of the Moon, Publ. of the Observatory of the Univ. of Mich., _4, 66, 1931.
  18. McCord, Thomas B., Color Differences on the Lunar Surface, J. Geophys♦ Res., 74, 3131, 1969.
  19. Mendell, W. W., and F. J. Low, Low-Resolution Differential Drift Scans of the Moon at 22 Microns, J. Geophys. Res., 75, 3319, 1970.
  20. Murray, Bruce C., and Robert L. Wildey, Surface Temperature Variations During the Lunar Nighttime, Astrophys. J., 139, 734, 1964.
  21. Pearse, C. A., Photometry and Polarimetry of the Moon and Their Relationship to Physical Properties of the Lunar Surface, Bellcomm Technical Report, TR-63-211-6, August 23, 1963.
  22. Pettit, Edison, and Seth B. Nicholson, Lunar Radiation and Temperatures, Astrophys. J., 7JL, 102, 1930.
  23. Pettit, Edison, Lunar Radiation as Related to Phase, Astrophys. J., 81, 17, 1935.
  24. Pettit, Edison, Radiation Measurements on the Eclipsed Moon, Astrophys♦ J., 9JL, 408, 1940. 110- Pettit, Edison, The Co-Albedo of the Moon, Astrophys. J., 102, 14, 1945.
  25. Piddington, J. H., and H. C. Minneut, Microwave Thermal Radiation from the Moon, Australian J. Sci. Res., A2/ 63, 1949.
  26. Roelof, Edmund C., Thermal Behavior of Rocks on the Lunar Surface, Icarus, .8, 138, 1968.
  27. Rosse, Laurence (Earl of), On the Radiation of Heat from the Moon, Proc. Roy. Soc. London, 17, 436, 1869.
  28. Saari, John M., and Richard W. Shorthill, Infrared Mapping of Lunar Craters During the Full Moon and the Total Eclipse of September 5, 1960, Boeing Sci. Res. Lab. Dl-82-0176, July, 1962.
  29. Saari, J. M., The Surface Temperature of the Antisolar Point of the Moon, Icarus, 3_, 161, 1964.
  30. Saari, J. M., and R. W. Shorthill, Isothermal and Isophotic Atlas of the Moon, NASA CR-855, September, 1967.
  31. Shorthill, R. W., H. C. Borough, and J. M. Conley, Enhanced Lunar Thermal Radiation During a Lunar Eclipse, Publ. Astron. Soc. of the Pacific, 72, 481, 1960.
  32. Shorthill, R. W., and J. M. Saari, Lunar Infrared Temperature Measurements During September 4, 5, & 6, 1960. Boeing Airplane Co. Poet. D7-2550-1, January, 1960.
  33. Shorthill, Richard W., Measurements of Lunar Temperature Variations During an Eclipse and Throughout a Lunation, Boeing Sci. Res. Lab, Dl-82-0196, August, 1962.
  34. Shorthill, Richard W., and John M. Saari, Radiometric and Photometric Mapping of the Moon Through a Lunation, Annals of the New York Acad. Sci., 123, 722, 1965.
  35. Shorthill, R. W., and J. M. Saari, Infrared Observation on the Eclipsed Moon, Boeing Sci♦ Res. Lab. Poet. Dl-82-0778, January, 1969.
  36. Sin ton, William M., Observations of Solar and Lunar Radiation at 1.5 Millimeters, JOSA, 45, 975, 1955.
  37. Sinton, William M., Observation of a Lunar Eclipse at 1.5 mm., Astrophys. J., 123, 325, 1956.
  38. Sinton, William M., A Pyrometer for Planetary Temperature Measurements, Lowell Observatory Bull., 4, 260, 1959.
  39. Sinton, William M., Eclipse Temperatures of the Lunar Crater Tycho, in The Moon, edited by Z. Kopal and Z. K. Mikhailov, p. 469, Academic Press, New York and London, 1962.
  40. Troitskii, V. C., On a Theory of the Radioemission of the Moon (in Russian), Astronomicheskii Zhurnal, 31, 511, 1954.
  41. Wattson, Richard B., and Iobert E. Danielson, The Infrared Spectrum of the Moon, Astrophys. J., 142, 16, 1965.
  42. Weaver, Harold, The Interpretation of Thermal Emission from the Moon, in Solar System Radio Astronomy: NATO Advanced Study Institute of the National Observatory of Athens, Cape Sounion, Greece, August 2-15, 1964, Lectures, p. 295, edited by Jules Aarons, Ionospheric Institute of the National Observatory, Athens, 1965.
  43. Wesselink, A. J., Heat Conductivity and Nature of the Lunar Surface Material, Bull. Astron. Inst, of the Netherlands, 10, 351, 1948.
  44. Wildey, Robert L., Bruce C. Murray, and James A. Westphal, Reconnaissance of Infrared Emission from the Lunar Nighttime Surface, J. Geophys. Res., 72^, 3743, 1967.
  45. Wildey, Robert L., The Nocturnal Heat Sources of the Surface of the Moon, Mon. Not. Royal Astron. Soc., 139, 471, 1968.
  46. Winter, D. F., and J. M. Saari, A Particulate Thermophysical Model of the Lunar Soil, Astrophys. J., 156, 1135, 1969.

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