This page contains a Flash digital edition of a book.
Scientists were surprised that Eros appears to have little or no magnetic field. Most meteorites, including chondrites, tend to be more magnetized than Eros. Perhaps its low levels of iron and the fact that it never has been heated to melting play a role in this differentiation. The spectral homogeneity of Eros combined with


Exploring Gas Giants


The goal of the Cassini mission is to explore Saturn, its many known moons and those yet to be discovered. Managed by NASA’s Jet Propulsion Laboratory (JPL) in Pasadena, California, USA, Cassini is a joint endeavor of NASA, the European Space Agency (ESA) and the Italian


gravity-field measurements,


structural characteristics and indications of structural coherence suggests that Eros is a collisional fragment of a larger parent body. The NEAR mission, a mission of many firsts in


NASA’s Discovery Program, substantially increased our knowledge of primitive bodies in our solar system. Although the data returned by NEAR have revealed many secrets of asteroids, many questions remain unanswered, and more will be learned from future missions.


4 0. NASA/ J et Propulsion Lab oratory – Cassini Mission to Saturn: http: / / w w w . j pl. nasa. gov/ new s/ fact_ sheets/ cassini. pdf ( accessed April 13 , 2006) .


H DAC


space agency, Agenzia Spaziale Italiana (ASI). It is one of the most ambitious efforts in planetary space exploration.4 0


Because of the low level of sunlight reaching Saturn, solar arrays are not feasible as a power source. Engineers employed a set of radioisotope- thermoelectric generators similar to those used


> Im aging Saturn’ s rings. The Ultraviolet Im aging Spectrograph ( UVIS) is a set of telescopes used to m easure ultraviolet light from the Saturn sy stem ’ s atm ospheres, rings and surfaces. The UVIS has tw o spectrographic channels or instrum ents: the ex trem e ultraviolet channel and the far ultraviolet ( FUV) channel. Each instrum ent is housed in alum inum cases, and each contains a re ecting telescope, a concave grating spectrom eter and an im aging, pulse- counting detector. The UVIS also includes a high-speed photom eter ( HSP) channel, a hy drogen-deuterium ab sorption cell ( HDAC) channel and an electronic and control sub assem b ly . ( Im age courtesy of NASA/ Lab oratory for Atm ospheric and Space Phy sics. )


4 -m high-gain antenna


11-m m agnetom eter b oom


Radar b ay


Radio/ plasm a w ave sub sy stem antenna ( 1 of 3 )


Rem ote sensing instrum ents


Radioisotope therm oelectric generator ( 1 of 3 )


4 4 5 N engine ( 1 of 2)


> Preparing Cassini for  ight. Technicians reposition and level the Cassini orb iter in the Pay load Hazardous Servicing Facility at the K ennedy Space Center in J uly 19 9 7 , after stack ing the craft’ s upper eq uipm ent section on the propulsion m odule ( left) . The orb iter’ s prim ary sy stem s are show n ( right) . ( Im ages courtesy of NASA/ J PL. )


5 6 Oilfield Review Low -gain antenna ( 1 of 2)


Huy gens Titan prob e


FU V spectrograph


H SP


Page 1  |  Page 2  |  Page 3  |  Page 4  |  Page 5  |  Page 6  |  Page 7  |  Page 8  |  Page 9  |  Page 10  |  Page 11  |  Page 12  |  Page 13  |  Page 14  |  Page 15  |  Page 16  |  Page 17  |  Page 18  |  Page 19  |  Page 20  |  Page 21  |  Page 22  |  Page 23  |  Page 24  |  Page 25  |  Page 26  |  Page 27  |  Page 28  |  Page 29  |  Page 30  |  Page 31  |  Page 32  |  Page 33  |  Page 34  |  Page 35  |  Page 36  |  Page 37  |  Page 38  |  Page 39  |  Page 40  |  Page 41  |  Page 42  |  Page 43  |  Page 44  |  Page 45  |  Page 46  |  Page 47  |  Page 48  |  Page 49  |  Page 50  |  Page 51  |  Page 52  |  Page 53  |  Page 54  |  Page 55  |  Page 56  |  Page 57  |  Page 58  |  Page 59  |  Page 60  |  Page 61  |  Page 62  |  Page 63  |  Page 64  |  Page 65  |  Page 66  |  Page 67  |  Page 68