Synthesis Imaging in Radio Astronomy by Nrao, N. M.) Nmimt Synthesis Imaging Summer School 1998

By Nrao, N. M.) Nmimt Synthesis Imaging Summer School 1998 (Socorro

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In addition of course, the abundance of heavy elements (where the term `heavy' denotes atoms heavier than He) increased as more and more hydrogen and then helium was fused in stars. Subsequent stars typically had lower mass and longer lives and shed their atmospheres more gently into the ISM when they died. The 15 N/ 14 N ratio of the material in the ISM is a good indicator of how much the material has evolved, since 15 N comes mainly from early primary production in stars ending in Type II supernovae, while 14 N comes mainly from second-generation lower-mass, longer-lived stars.

Courtesy of Mark McCaughrean and the Astronomical Journal. , 1998). As can be seen, the circumstellar disc is of the order of 1,000 AU across. This formation scenario requires a mechanism for disc dispersal on timescales of 1 million to 10 million years. Solar mass stars cannot easily blow away dense circumstellar discs and thus accretion onto the star seems more likely. However in order for this accretion to proceed, some way is needed of losing or redistributing the angular momentum. By conservation of angular momentum, one would expect the nebula to rotate fastest towards the centre and thus the protoSun should initially have been rotating very rapidly.

2d which lists the larger Neptunian satellites with a radius greater than 100 km. Voyager 2 observed Triton to have an extremely thin N2 atmosphere. 3 SATELLITES OF THE OUTER PLANETS The satellites of the giant planets are believed to have formed in two ways: (1) formation in a circumplanetary accretion disc (accretion discs are discussed in Chapter 2) at the same time as the planet; and (2) later capture of remaining planetesimals in the solar system. Satellites formed by the ®rst mechanism are expected to lie in the equatorial plane of the planet and to have near-circular orbits.

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