By K. B. Macgregor (auth.), Lex Kaper, Alexander W. Fullerton (eds.)
It is celebrated that stellar winds are variable. fresh investigations express that the saw fluctuations are frequently cyclical in nature. This estate looks shared via the winds of cool and sizzling stars, even supposing the actual mechanisms using those winds are essentially diverse. The time was once ripe for astrophysicists learning sorts of stars, yet making use of very comparable types, to give the state-of-the-art in a concise shape. The complaints will supply an invaluable, updated evaluate of the observations, interpretation, and modelling of the time-dependent mass outflows from a large choice of stars, together with younger, pre-main-sequence gadgets, solar-type stars, purple supergiants, and scorching, substantial stars.
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Extra info for Cyclical Variability in Stellar Winds: Proceedings of the ESO Workshop Held at Garching, Germany, 14 – 17 October 1997
With realistic path lengths between scatterings, a vastly greater number of scatterings is required. I found Monte Carlo simulations with synthetic line lists instructive in understanding the relation between photon trapping, energy degradation and momentum transfer. You could carry out the same exercise or consult the paper of V. Springmann (1994, A&A, 289, 505). A Thermo-Radiatively Driven, Analytical 2-D Model for Stellar Outflows Alexander Kakouris 1 ,2 1 2 Section of AA&M, University of Athens, Athens, Greece Hellenic Air Force Academy, Dekelia, Attiki, Greece Analytical, steady-state, 2-D solutions for thermally driven stellar winds were found by Kakouris & Moussas (1996).
Lucy loss. The basic point of departure from LS was to replace their accurate but cumbersome calculations of gR by an approximate but rapid calculation based on an analytical expression for each line's contribution given by Sobolev theory (Lucy 1971; Castor 1974). 2) dV) - 9 + -2a 2 -1 -dv = gR (. p, v, V d1' d1' l' As written, this equation reflects the fact that, when evaluated in the Sobolev approximation, gR is a function only of local variables including, in particular, the velocity gradient dv/d1', which therefore, remarkably, appears twice in the equation of motion.
2. Radial and azimuthal velocity proilles for thermally driven winds in the presence of rotation. Curve (a) applies to the case of an outflow from a non-rotating star, while curves (b) - (d) depict the effects of increasingly rapid rotation, as discussed in the text. 08 TO, for parameter values appropriate to the results of Figure 2] and Te are, respectively, the locations ofthe sonic critical point corresponding to E = 0 and E =j: O. 08 TO as E is increased. 88, a second, noncritical zero exists in the numerator of the equation of motion (6), with a location (9) = that increases from Tc2 TO for increasing E within the indicated range.