Jupiter II

Mike Superczynski, head of the Machinery Technology Branch of the Navy s David Taylor Research Center, is a big man with a booming laugh who knows all about Japanese EMT but is far more interested in what the navy calls S/C electric drive—superconducting electric drive—as it applies to ship propulsion, and specifically to a test craft called Jupiter II. He also knows a lot about superconductivity and likes to tell the story about the admiral who once introduced him to a scientific symposium with the words, Now the super is Mike s middle name, and the czynski is Polish for conductivity. ... 

The navy s approach to superconducting ships is far different from Saji s. While the ST-500 bootstraps itself along using seawater as the power fluid, the craft the navy has christened Jupiter II runs on a superconductive motor which drives a propeller. Moreover, the ST-500 is a model that has done its tricks only in a test tank. Jupiter II, with a 400-HP motor and generator (later upgraded to 3,000 HP), was the first vessel in history to be propelled at sea by a completely superconducting electric drive system. 

Jupiter II wasn t around during a visit to the navy s lab in Annapolis, but her engine was. Like Saji s model, it was up on blocks in a laboratory that looked, as do so many others where physicists and engineers work, like a machine shop full of jerry-built equipment stacked to the ceilings. 

Essential technology of the Navy s Superconductive Electric Propulsion system for the Jupiter II. (Courtesy of the U.S. Navy s David Taylor Research Center.)... 

DTNSRDC ELECTRIC DRIVE TEST CRAFT JUPITER II... 

Later Saturns and Titans used LP of higher Isp, eg Saturn-II and Saturn-IVB used LO/ liq Hydrogen Post 1959 Titans used N204/ Hydrazine derivatives Jupiter-C used LO/ Hydrazine derivatives and the French Diamant I space booster used nitric acid/turpentine (Ref 32). ... 

Figure 2.6 Carbon- and nitrogen-isotopic compositions of presolar SiC grains. Predictions from stellar models are shown for comparison. Solar metallicity AGB star models Nollett et al. (2003), Type II SN Rauscher et al. (2002), novae Jose et al. (2004). For data sources see Lodders Amari (2005) Zinner (2007). Note that for the solar 14N/15N ratio the value inferred for Jupiter s atmosphere is shown.

Figure 9 Comparison of silicate mass fractions. Two assumptions for interior strueture are shown (i) differentiated—rock core, ice mantle, and (ii) homogeneous—uniformly mixed ice and roek. Also shown are silicate mass fractions for the Jupiter and Saturn systems and expected values for two models of the early solar nebula carbon chemistry (see text) (after Johnson et aL, 1987) (reproduced by permission of Ameriean Geophysieal Union from /. Geophys. Res. Space Phys. 1987, 92, 14884-14894).

II n y a pas du tout d etain sur lui, massa Will, je vous le parie, interrompit Jupiter le scarabee est un scarabee d or, d or massif, d un bout a Fautre, dedans et partout, excepte les ailes. 

Tin Calx of tin (Libavius) Sel ou Vitriol de Jupiter (Beguin) (Tin(II) nitrate) Calx of tin (Libavius) (Tin(ll) acetate) Spiritus fumans Libavii (Libavius) ( Iln(IV) cblraide)... 

Aptaker, I. M. (1987). A Near Infrared Mapping Spectrometer (NIMS) for investigation of Jupiter and its satellites. In Imaging Spectroscopy II, ed. G. Vane. SPIE Proceedings, 834, 196, Bellingham, Washington. 

The term "Solar System ice" denotes in general a solidified volatile and/or mixtures of solidified volatiles. The Solar System ices are mostly water ice H2O, but also solidified CO2, CO, NH3, N2, SO2, CH4 and many other simple molecules as well as the organics. On the surfaces of many of the satellites of the giant planets (Jupiter, Saturn, Uranus, and Neptune) water ice is the dominant component. Therefore, in the following we will adopt the common assumption that a satellite is composed of water ice, and silicates. The radii and the masses of all satellites but the smallest ones are well known. Therefore their densities are known as well, see Table 1. Taking into account that the densities of water ice are about 940,1190, and 1360 kg m at phases I, II, and VI, respectively, and that the density of the silicates is (3400 400) kg m" the mass ratio C of silicates to total mass of the satellite can be estimated. This is rather simple for large satellites however, the estimate can fail for smaller satellites because of the possible bulk primordial porosity left fi-om an epoch of formation. 

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