Evolutionary and Physical Properties of Meteoroids: The Proceedings of the International Astronomical Union's Colloquium # 13, Held at the State University of New York, Albany, N.Y., on June 14-17, 1971
Scientific and Technical Information Office, National Aeronautics and Space Administration, 1973 - 378 من الصفحات
"The Fourteenth General Assembly of the International Astronomical Union was held in Brighton, England, in 1970. During the conference, arrangements were made to hold a colloquium on "The Evolutionary and Physical Problems of Meteoroids." An invitation was issued by the State University of New York at Albany (SUNYA) and the Dudley Observatory to host the meeting. C.L. Hemenway, P.M. Millman, and A.F. Cook were selected to organize the program. IAU Colloquium No. 13 was held June 14-17, 1971, at the State University of New York at Albany. Forty papers were presented and are included in this volume."--Preface.
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ablation analysis appears assumed asteroids Astrophys atmosphere atoms body bright charge chondrites collection collisions comets compared component composition computed craters curve density dependence derived detector determined direction distance distribution Dudley Observatory dust effect efficiency electron elements energy equation experiments field figure fireballs flux fragment function given grains height impact increase indicated initial intensity ionization ions iron km/s known light limit lower luminous lunar magnetic magnitude mass material mean measured meteor meteorites meteoroid micrometeorites multiplets Network objects observed obtained occurred orbits origin particles percent phase photographic physical position possible present pressure probability problem produced radar radiation radius range ratio recorded relative Research respect rock shower shown shows similar solar Space spectra spectrum station stream surface temperature tion trail values velocity volume
الصفحة 353 - This work has been supported in part by grants from the National Science Foundation and the National Aeronautics and Space Administration.
الصفحة 359 - cometesimals" of radius 100 m or larger at great solar distances. Correspondingly, the mean free path of the gas molecules is of the order of 1 m or more so that little error is made in applying Epstein's law up to perhaps s=10 m, while to about the same limit the diffusion slowing of the accretion rate by the second term of equation (13) can be neglected. Hence, by equation (15), the time...
الصفحة 239 - SHOEMAKER, EM, HAIT, MH, SWANN, GA, SCHLEICHER, DL, SCHABER, GG, SUTTON, RL, DAHLEM, DH, GODDARD, EN, AND WATERS, AC, 1970. Origin of the lunar regolith at Tranquility Base, Proc.
الصفحة 128 - ELTERMAN, L., 1964. Atmospheric attenuation model, 1964, in the ultraviolet, visible, and infrared regions for altitudes to 50 km, US Air Force Environ.
الصفحة 226 - Texas. , 1970. The Gegenschein and interplanetary dust outside the Earth's orbit, Icarus, 13, 184201.
الصفحة 141 - Perseid showers indicate a relationship between the frequency of occurrence of the oxygen line and solar activity. In 1969-70, near sunspot maximum, the strength of this so-called auroral green line is greatest near shower maximum, as though the nature of the meteoroids were a function of their distance from the core of the stream, or, alternatively, the strength of the green line were a function of the altitude of the radiant. SINCE 1948, A...
الصفحة 147 - Smithsonian Astrophysical Observatory Cambridge, Massachusetts AND CL HEMENWAY State University of New York at Albany and Dudley Observatory Albany, New York The spectra of 25 meteors, recorded with an image-orthicon technique in December 1969, are studied in relation to similar records made in August of the same year. Of 19 Geminid meteors in the absolute visual magnitude range 0 to +2, only one showed any evidence of the forbidden line of oxygen at 5577 A, while all Perseid meteors recorded in...
الصفحة 45 - Since the advent of low-light-level television (LLLTV) systems, it has been recognized that such devices offer the ability to observe meteors as faint as 10th magnitude which allows the extension of optical meteor data to masses as small as 10~4 gram. The Space Sciences Laboratory at Marshall Space Flight Center has been actively engaged in such observations using image orthicons and intensified SEC vidicons. The results of these observations are presented along with an interpretation in terms of...
الصفحة 220 - Icarus, 13, 215-225. , 1971. On the history of lunar impact cratering: the absolute time scale and the origin of planetesimals, Icarus, 14, 36-52. BERG, OE, AND GERLOFF, U., 1971. More than two years of micrometeorite data from two Pioneer satellites, Space Research XI, 225-235. BLOCH, MR, FECHTIG, H., GENTNER, W., NEUKUM, G., AND SCHNEIDER, E., 1971.
الصفحة 141 - ... features will be considered. The spectra from the 1961 shower were classified into four groups on the basis of the presence of certain spectral lines as follows: Group 1 — The H and K lines of ionized calcium Group 2 — The magnesium triplet at 5175 A, the auroral green line of neutral oxygen at 5577 A, the D line of sodium, and a calcium-iron blend near 6170 A Group 3 — Only the D line of sodium and the blend at 6170 A Group 4 — Only the D line of sodium In 1961 these four categories...