Lunar Sourcebook : a User's Guide to the Moon

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Lunar Sourcebook : a User's Guide to the Moon REFERENCES Adams J. B. (1974) Visible and near-infrared diffuse chemistry, mineralogy and petrology of some Apollo 11 reflectance spectra of pyroxenes as applied to remote lunar samples. Proc. Apollo 11 Lunar Sci. Conf., pp. 93–128. sensing of solid objects in the solar system. J. Geophys. Ahrens T. J. and Cole D. M. (1974) Shock compression and Res., 79, 4829–4836. adiabatic release of lunar fines from Apollo 17. Proc. Lunar Adams J. B. (1975) Interpretation of visible and near-infrared Sci. Conf. 5th, pp. 2333–2345. diffuse reflectance spectra of pyroxenes and other rock Ahrens T. J. and O’Keefe J. D. (1977) Equations of state and forming minerals. In Infrared and Raman Spectroscopy of impact-induced shock-wave interaction on the Moon. In Lunar and Terrestrial Materials (C. Karr, ed.), pp. 91–116. Impact and Explosion Cratering (D. J. Roddy, R. O. Pepin, Academic, New York. and R. B. Merrill, eds.), pp. 639–656. Pergamon, New York. Adams J. B. and McCord T. B. (1973) Vitrification darkening Albee A. L. and Chodos A. A. (1970) Microprobe investigations in the lunar highlands and identification of Descartes on Apollo 11 samples. Proc. Apollo 11 Lunar Sci. Conf., pp. material at the Apollo 16 site. Proc. Lunar Sci. Conf. 4th, 135–157. pp. 163–177. Albee A. L., Chodos A. A., Gancarz A. J., Haines E. L., Adams J. B., Pieters C., and McCord T. B. (1974) Orange Papanastassiou D. A., Ray L., Tera F., Wasserburg G. J., glass: Evidence for regional deposits of pyroclastic origin and Wen T. (1972) Mineralogy, petrology, and chemistry of on the Moon. Proc. Lunar Sci. Conf. 5th, pp. 171–186. a Luna 16 basaltic fragment, sample B-1. Earth Planet. Sci. Adams J. B., Charette M. P., and Rhodes J. M. (1975) Lett., 13, 353–367. Chemical fractionation of the lunar regolith by impact Aldrin E. E. Jr., Armstrong N. A., and Collins M. (1969) Crew melting. Science, 190, 380–381. observations. In Apollo 11 Preliminary Science Report, pp. Adams J. B., Hörz F., and Gibbons R. V. (1979) Effects of 35–39. NASA SP-214. shock-loading on the reflectance spectra of plagioclase, Alexander E. C. Jr. and Kahl S. B. (1974) 40Ar-39Ar studies of pyroxene and glass (abstract). In Lunar and Planetary lunar breccias. Proc. Lunar Sci. Conf. 5th, pp. 1353–1373. Science X, pp. 1–3. Lunar and Planetary Institute, Alexander E. C. Jr., Coscio M. R. Jr., Dragon J. C., and Saito Houston. K. (1980) K/Ar dating of lunar soils IV: Orange glass from Adams J. H. Jr. and Shapiro M. M. (1985) Irradiation of the 74220 and agglutinates from 14259 and 14163. Proc. Lunar Moon by galactic cosmic rays and other particles. In Lunar Planet. Sci. Conf. 11th, pp. 1663–1677. Bases and Space Activities of the 21st Century (W. W. Alexandrov A. K., Borisov B. M., Garin I. S., Grafov V. I., Mendell, ed.), pp. 315–327. Lunar and Planetary Institute, Ivanov A. G., Kotlov Yu. P., Komarov V. I., Kuleshov A. F., Houston. Mishkin V. K., Nikolayev G. B., Polenov L. N., Semenov P. Adler I. and Trombka J. I. (1977) Orbital chemistry–lunar S., and Yakovlev F. P. (1972) Investigations of mobility of surface analysis from the X-ray and gamma-ray remote Lunokhod 1. In COSPAR Space Research XII, pp. 73–82. sensing experiments. Phys. Chem. Earth, 10, 17–43. Akademie-Verlag, Berlin. Adler I., Trombka J., Gerard J., Schmadabeck R., Lowman P., Ali M. Z. and Ehmann W. D. (1977) Chemical Blodgett H., Yin L, Eller E., Lamoth R., Gorenstein P., characterization of lunar core 60010. Proc. Lunar Sci. Conf. Bjorkholm P., Harris B., and Gursky H. (1972) X-ray 8th, pp. 2967–2981. fluorescence experiment. In Apollo 15 Preliminary Science Allen C. C. (1975) Central peaks in lunar craters. The Moon, Report, pp. 17–1 to 17–17. NASA SP-289. 12, 463–474. Adler I., Trombka J. I., Schmadebeck R., Lowman P., Blodget Allen R. O. Jr., Jovanovic S., and Reed G. W. Jr. (1974) A H., Yin L., Eller E., Podwysocki M., Weidner J. R., Bickel study of 204Pb partition in lunar samples using terrestrial A. L., Lum R. K. L., Gerard J., Gorenstein P., Bjorkholm and meteoritic analogues. Proc. Lunar Sci. Conf. 5th, pp. P., and Harris B. (1973) Results of the Apollo 15 and 16 X- 1617–1623. ray experiment. Proc. Lunar Sci. Conf. 4th, pp. 2783–2791. Allen R. O., Jovanovic S., and Reed G. W. Jr. (1975) Aggarwal H. R. and Oberbeck V. R. (1979) Monte Carlo Agglutinates: Role in element and isotope chemistry and simulation of lunar megaregolith and implications. Proc. inferences regarding volatile-rich rock 66095 and glass Lunar Planet. Sci. Conf. 10th, pp. 2689–2705. 74220. Proc. Lunar Sci. Conf. 6th, pp. 2271–2279. Agosto W. N. (1985) Electrostatic concentration of lunar soil Allton J. H. (1989) Catalog of Apollo Lunar Surface Geological minerals. In Lunar Bases and Space Activities of the 21st Sampling Tools and Containers. NASA JSC Publ. No. 23454. Century (W. W. Mendell, ed.), pp. 453–464. Lunar and 92 pp. Planetary Institute, Houston. Allton J. H. and Waltz S. R. (1980) Depth scales for Apollo 15, Agrell S. O., Peckett A., Boyd F. R., Haggerty S. E., Bunch T. 16, and 17 drill cores. Proc. Lunar Planet. Sci. Conf. 11th, E., Cameron E. N., Dence M. R., Douglas J. A. V., Plant A. pp. 1463–1477. G., Traill R. J., James O. B., Keil K., and Prinz M. (1970a) Alvarez L. W., Alvarez W., Asaro F., and Michel H. V. (1980) Titanian chromite, aluminum chromite, and chromian Extraterrestrial cause for the Cretaceous-Tertiary mass ulvöspinel from Apollo 11 rocks. Proc. Apollo 11 Lunar Sci. extinction. Science, 208, 1095–1108. Conf., pp. 81–86. Agrell S. O., Scoon J. H., Muir I. D., Long J. V. P., McConnell J. D. C., and Peckett A. (1970b) Observations on the 655 656 Lunar Sourcebook Alvarez R. (1973a) Lunar fines 74241,2, low frequency Andre C. G., Bielefeld M. J., Eliason E., Soderblom L. A., dielectric variations with density and temperature. Eos Adler I., and Philpotts J. A. (1977) Lunar surface chemistry: Trans. AGU, 54, 1129. A new imaging technique. Science, 197, 986–989. Alvarez R. (1973b) Lunar powder simulator under lunarlike Annell C. S. and Helz A. W. (1970) Emission spectrographic conditions, dielectric properties. J. Geophys. Res., 78, determination of trace elements in lunar samples from 6833–6844. Apollo 11. Proc. Apollo 11 Lunar Sci. Conf., pp. 991–994. Alvarez R. (1974a) Dielectric comparison of lunar and Apollo 15 Preliminary Examination Team (1972) Preliminary terrestrial fines at lunar conditions. J. Geophys. Res., 79, examination of lunar samples. In Apollo 15 Preliminary 5453–5457. Science Report, pp. 6–1 to 6–25. NASA SP-289. Alvarez R. (1974b) Electrical properties of sample 70215 in Apollo Soil Survey (1971) Apollo 14: Nature and origin of rock the lunar temperature range of 100° to 373°K (abstract). types in soil from Fra Mauro Formation. Earth Planet. Sci. In Lunar Science V, pp. 15–17. The Lunar Science Lett., 12, 49–54. Institute, Houston. Appleman D. E., Nissen H.-U., Stewart D. B., Clark J. R., Alvarez R. (1974c) Electrical properties of sample 70215; low Dowty E., and Huebner J. S. (1971) Studies of lunar frequency corrections. Proc. Lunar Sci. Conf.5th, pp. 2663– plagioclases, tridymite, and cristobalite. Proc. Lunar Sci. 2671. Conf. 2nd, pp. 117–133. Alvarez R. (1974d) Lunar magnetization and surface charge Arkani-Hamed J. (1973) On the thermal history of the Moon. variations (abstract). In Lunar Interactions (D. R. Criswell Proc. Lunar Sci. Conf. 4th, pp. 2673–2684. and J. W. Freeman, eds.), pp. 61–63. The Lunar Science Arkani-Hamed J. (1974) Lunar mascons as consequences of Institute, Houston. giant impacts. The Moon, 10, 307–322. Alvarez R. (1975) Lunar and terrestrial sample Armstrong N., Collins M., and Aldrin E. E. (1970) First on the photoconductivity. Proc. Lunar Sci. Conf. 6th, pp. 3187– Moon. Little, Brown and Co., Boston. 511 pp. 3197. Armstrong T. W. and Alsmiller R. G. Jr. (1971) Calculation of Alvarez R. (1977a) On charge transport in the terminator's cosmogenic radionuclides in the Moon and comparison vicinity (abstract). In Lunar Science VIII, pp. 28–30. The with Apollo measurements. Proc. Lunar Sci. Conf. 2nd, pp. Lunar Science Institute, Houston. 1729–1745. Alvarez R. (1977b) Photoconductive effects on lunar and Arndt J. and von Engelhardt W. (1987) Formation of Apollo terrestrial fines. Proc. Lunar Sci. Conf. 8th, pp. 1277–1290. 17 orange and black glass beads. Proc. Lunar Planet. Sci. Anders E. (1968) Chemical processes in the early solar Conf. 17th, in J. Geophys. Res., 92, E372–E376. system, as inferred from meteorites. Acc. Chem. Res., 1, Arndt J., Flad K., and Feth M. (1979) Radiative cooling 289–298. experiments on lunar glass analogues. Proc. Lunar Planet. Anders E. (1978) Procrustean science: Indigenous Sci. Conf. 10th, pp. 355–373. siderophiles in the lunar highlands, according to Delano Arndt J., Hummel W., and Gonzalez-Chabeza I. (1982) and Ringwood. Proc. Lunar Planet. Sci. Conf. 9th, pp. 161– Diaplectic labradorite glass from the Manicouagan impact 184. crater. Phys. Chem. Minerals, 8, 230–239. Anders E. and Ebihara M. (1982) Solar-system abundances of Arndt J., von Engelhardt W., Gonzales-Cabeza I., and Meier the elements. Geochim. Cosmochim. Acta, 46, 2363–2380. B. (1984) Formation of Apollo 15 green glass beads. Proc. Anders E., Ganapathy R., Keays R. R., Laul J. C., and Morgan Lunar Planet. Sci. Conf. 15th, in J. Geophys. Res, 89, C225– J. W. (1971) Volatile and siderophile elements in lunar C232.
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