By Attilio Ferrari, Robert Rosner (auth.), Luciana Bianchi, Roberto Gilmozzi (eds.)
The aim of this workshop was once to place jointly observational and theoretical works on outflows from other kinds of astrophysical gadgets, happening on varied scales and at a variety of evolutionary stages, and to debate the effect of observations from destiny area missions. For the celebs, we idea to stick to through the evolution the relevance (rates and dynamical rrodes) of the mass loss phenomenon, e. g. to give an explanation for how and while tremendous stars free so much in their ini tial mass to finish up with commonplace WD plenty. The observations of the sunlight wind have been incorporated for being a distinct case the place the starting place and propagation of the outflow could be resolved. We proposal that the comparability with related phenomena happening in galactic outflows will be fruitful, as tested via contemporary works on galactic winds and jets. The curiosity of getting this workshop in Torino got here simply because there are teams during this zone, on the Astronomical Observatory and on the Institute of Physics of the college, enthusiastic about the theoretical and observational stories of outflows from astrophysical items. The participants of the medical Organizing Conmi ttee have been: V. Castellani, C. Cesarski, P. Conti, A. Ferrari, A. Gabriel, M. Grewing, Y. Kondo, H. Lamers, V. Manno, M. Rees and R. Schilizzi. The neighborhood Organizing Conmi ttee used to be: L. Bianchi, G. Massone and E. Antonucci. throughout the workshop the subsequent subject matters have been handled: the sun wind, the mass loss from cool stars and from sizzling stars (m. s.
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Extra resources for Mass Outflows from Stars and Galactic Nuclei: Proceedings of the Second Torino Workshop, Held in Torino, Italy, May 4–8, 1987
Mass-loss rates for more stars and in particular more accurate values cannot be expected in the near future for normal giants. The situation is probably more favourable for highly evolved stars with molecular line emission. However, for most of these stars (like OH-IR stars) stellar parameters like mass are poorly known. I shall therefore briefly discuss the implications for stellar evolution. 10- 13 L/ g • R (1) proposed on dimensional arguments and calibrated with empirical mass-loss rates for a number of Pop I 36 giants and supergiants (Reimers, 1975).
2. 1 MASS LOSS STUDIES FROM UV LINES The Method of Line Fitting Mass loss rates can be determined from the analysis of the P Cygni profiles of UV resonance lines and lines from metastable levels. This analysis implies the comparison between the observed profiles and those calculated for spherical symmetric winds with an assumed velocity law. g. Castor and Lamers, 1979) because of its simplicity and accuracy for winds with large velocity gradients. Since the Sobolev approximation is not valid at low velocities, this linefitting does not give information about the conditions at the base of the wind.
5. EXTENDED CHROMOSPHERES AND WIND EXPANSION There is growing evidence that closely related to strong mass-loss in red giants is the existence of geometrically extended chromospheres. During a lunar occultatiQnof 119 Tau (M2Iab) it was observed that Ha light comes from a region having at least twice the diameter of that which produces the continuum. , 1986). It was also found that the extended Ha chromosphere has an elongated shape. Recall that during a solar eclipse bright red features (Ha ) are seen here and there around the obscured disk.