By B. N. Swanenburg (auth.), Bengt E. Westerlund (eds.)
The 4th eu nearby assembly in Astronomy, entitled "Stars and big name Systems", used to be held in Uppsala, Sweden, on August 7 -12, 1978. It used to be attended through 228 individuals from 24 nations. Over a hundred papers have been provided; this required parallel periods through the assembly. monetary aid used to be given by means of the IAU, the Swedish division of schooling, the Swedish average technology learn Council, the Swedish Institute and the college of Uppsala. The participants of the clinical and native Organizing Committees are indexed less than, and that i thank them all for his or her contributions to the assembly. The assembly used to be divided into six sections, in line with the scien tific subject matters: Galaxies (A) - together with galactic constitution and superstar for mation; High-Energy Astrophysics (B); Stars (C); Interstellar approaches (D); Astronomical Instrumentation (E) and schooling in Astronomy (F). In each one part a couple of Invited Papers have been awarded in addition to lots of contributed papers. additionally, every day a common Lecture used to be given via an Invited Speaker. the current quantity comprises the entire basic Lectures and the entire Invited Papers offered in the course of the assembly. In 3 situations, despite the fact that, and for numerous purposes, in simple terms short summaries were on hand. Abstracts of the contributed papers can be present in Uppsala Astronomical Observatory, document No. 12.
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Extra info for Stars and Star Systems: Proceedings of the Fourth European Regional Meeting in Astronomy Held in Uppsala, Sweden, 7–12 August, 1978
223, 788. HIGH-ENERGY PHENOMENA ON THE SOLAR SURFACE Claudio Chiuderi Istituto di Astronomia, Universita di Firenze, Italy 1. INTRODUCTION I shall start this review of the high-energy phenomena on the solar surface by briefly discussing the meaning of the title. By solar surface it is meant the whole of the solar atmosphere, from, say, T5000 = 1 up. By high-energ~ phenomena I mean the complex of the observed events that lnvolve the presence of suprathermal particles and the emission of radiation whose brightness temperature exceeds the kinetic temperature.
9·2 9-0 o GALAXY x M33. M101 • SMC. £ 8·4 + 8·2 N ~ 8·0 0·0 Fig. ) ] corresponding to equation (1). The relat~on predicted by the simple model is a straight line of unit slope. 003. The straight line in Fig. 3 represents the predictions of the simple model, now using a logarithmic scale. We can see that it fits both Magellanic Clouds and some of the H II regions in the outer parts of our own Galaxy and M33 and MlOl (the ones on the left side of the diagram). This result is of some interest, because it suggests that the progress of element formation in the Magellanic Clouds has not been very different from what it has been in the outer parts of the three spiral galaxies, so that modifications to the simple model, with inflows, outflows or changes in the IMF have had only minor effects.
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