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Download Investigating the Universe: Papers presented to Zdeněk Kopal by F. D. Kahn (auth.), F. D. Kahn (eds.) PDF

By F. D. Kahn (auth.), F. D. Kahn (eds.)

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Additional info for Investigating the Universe: Papers presented to Zdeněk Kopal on the occasion of his retirement, September 1981

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The optical remnant is dominated by two different kinds of filaments distinguishable both in their dynamics and spectra. These are unusual1y termed the 'quasi-stationary f1occu1i' (QSF) and the 'fast mov ing knots' (FMK). The QSF have spectra with strong hydrogen Balmer 1ines, [NIl] A6583 - 2-3 x Ha. The [OI] lines are fairly strong but the [0111] are weaker than HS. Lines of [NI], [SII] , [FeII] , [HeI] and [CaII] appear in similar strength to HS (Kirshner and Chevalier 1977). The QSF have a 10w ve10city dispersion (-200 km s-l) and Kamper and van den Bergh (1976) find an overa11 expansion rate, from proper motions of about 150 km s-l.

A strictly one-dimensional model can account for the existence of high-velocity clouds at high galactic latitudes, but not in directions close to the galactic plane, particularly so in the direction of the anti-centre. Further it is obviously idle to expect that a plane-parallel model will serve for extended regions of the Galaxy. The very existence of spiral structure shows that the rate of star formation varies considerably from place to place in the galactic disk, and there must be similar variations in the rate at which supernova explosions subsequently inject energy into the ICM.

Blair, Kirshner and Chevalier (1981) have found an almost identical relationship for M3l, using the post-shock pressure as given by the [SII] ratio to derive the driving pressure of the blast wave and hence the explosion energy. They also used Dopita, D'Odorico and Benvenuti's (1980) observations in M33 and galactic data from Daltabuit, D'Odorico and Sabbadin (1976) to show that these galaxies too follow essentially the same reIat ion (Fig. 2). Blair et al. prefer a model in which the [SII] emitting regions are dominated by magnetic pressure, either due to direct compression of the interstellar field (McKee and Hollenbach 1980), or by field amplification (Reynolds and Chevalier 1981).

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