Physical Studies of Minor PlanetsScientific and Technical Information Office, National Aeronautics and Space Administration, 1972 - 687 Seiten " ... Some papers and discussions included in this book even though they were not presented at the meeting. In some respects, therefore, the book is independent of the colloquium. Several papers had been invited long beforehand with the request to publish them as review papers. The lack of a modern textbook on minor planets is keenly felt, and the proceedings of this meeting, with these additions, should provide a good reference book."--Page viii. |
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Seite 145
... variation due to the odd - order terms , which may be associated with either a spotted surface or Lambert law reflectivity . However , it appears likely that if 39 Laetitia is observed closer to its equatorial plane , the size of these ...
... variation due to the odd - order terms , which may be associated with either a spotted surface or Lambert law reflectivity . However , it appears likely that if 39 Laetitia is observed closer to its equatorial plane , the size of these ...
Seite 146
... variation is due to shape rather than spots . Is it possible to make the model yield shape information as well as ... variation was primarily due to shape . Variation in surface reflectivity could contribute something , but when the ...
... variation is due to shape rather than spots . Is it possible to make the model yield shape information as well as ... variation was primarily due to shape . Variation in surface reflectivity could contribute something , but when the ...
Seite 257
... variation in brightness ( after corrections for distance and phase effects have been made ) must correspond to a variation in the projected surface area . There will be no change in the brightness variation over one orbital period if ...
... variation in brightness ( after corrections for distance and phase effects have been made ) must correspond to a variation in the projected surface area . There will be no change in the brightness variation over one orbital period if ...
Inhalt
ASTROMETRIC OBSERVATIONS | 3 |
THE WORK AT THE MINOR PLANET CENTER | 9 |
DIAMETER MEASUREMENTS OF ASTEROIDS | 25 |
Urheberrecht | |
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accretion albedo Alfvén Anders Apollo Apollo 12 Apollo asteroids asteroid belt asteroid families Astron Astrophys axis brightness Brouwer Ceres chondrites collisional collisions cometary comets counterglow craters curve density determined diameter discussed distance Dohnanyi Dollfus Earth ecliptic effect Ephemeris equation Eros families Figure flyby fragments function Gehrels Geophys gravity heliocentric Houten Icarus impact interplanetary dust iron meteorites jetstream Jupiter km/s Kuiper launch libration lightcurve longitude lunar magnitude Mars Mars-crossing asteroids mass distribution material measurements meteor meteoroid minor planets mission Moon NASA number of asteroids numbered asteroids objects Observatory observed obtained orbital elements Pallas parent bodies particles percent perihelion perturbations phase angle phase coefficient photometric planetary planetoids polarization pole propulsion radius range relative rotation sample satellites scattering semimajor axis solar nebula solar system space spacecraft stream surface target telescope trajectory Trojans velocity Vesta wavelength Whipple Zodiacal Light