Download PDF by Roberta M. Humphreys (auth.), Henny J. G. L. M. Lamers,: Instabilities in Luminous Early Type Stars: Proceedings of a

By Roberta M. Humphreys (auth.), Henny J. G. L. M. Lamers, Camiel W. H. De Loore (eds.)

On April 28 1986 Cornelis de Jager reached the age of sixty five years. On April 30 he formally retired from the collage of Utrecht the place he has held a Chair for Stellar Astrophysics, later became house Physics, when you consider that 1958. Cees de Jager, as he prefers to be referred to as by way of his buddies, has had an energetic and profitable lifestyles in technological know-how. His curiosity in astronomy was once raised by way of his father less than the transparent skies of Celebes (Indonesia). He begun a examine in physics and astronomy as a scholar of the overdue M. Minnaert in Utrecht in the course of international battle II. whilst in 1943 the occupying forces recruited scholars who didn't wish to signal the announcement of loyalty for his or her war-efforts, Cees and 3 fellow scholars went into hiding on the Observatory in Utrecht. in this very "quiet" interval van de Hulst constructed the speculation of the 21 em radiation of impartial hydrogen and de Jager begun the observations of variable stars within the pitch darkish nights of a rustic at warfare. The research of Beta Cepheids speedy­ ly woke up his curiosity which was once saved during the years. In 1958 he equipped a world crusade to watch 12 Lac spectroscopically and photometrically, which was once a good success.

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Additional info for Instabilities in Luminous Early Type Stars: Proceedings of a Workshop in Honour of Professor Cees De Jager on the Occasion of his 65th Birthday held in Lunteren, The Netherlands, 21–24 April 1986

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300. -200. O. -100. 100. 200. VELOCITY IKM/SECl Apr. 1 I I V:· I ,l-' ~. ,. , ... • . • •• •• ' • • • . 4050 ~ 4100 • HJD Figure 5. Simultaneous monitoring of r lSco in UV spectroscopy (lUE satellite) and visual photometry (Geneva system) . Top: variation of the absorption components on the MgII line at 2795 A. Bottom: photometric variability at the same epoch. 32 G. BURKI ii) De Jager et al. (1984) proved that the motion field of the lower photosphere of Q Cyg (A2 la) can be described by a field of outward progressing sound waves which turn into shock waves in the photosphere.

A real treatment as a 'valve mechanism', i. e. an e>:treme mass loss on a very short time scale, is not possible by the kind of evolutionary codes we use for the 'overall' evolutionary pattern, (the evolutionary codes are made for the treatment of stable, spherical, equilibrium models, and are able to handle mass loss, when time is allowed for the model to restore equilibrium) and should require an hydrodynamical code. MAEDER: I want to emphasize the importance of surface chemistry as an observational test of stellar evolution, in addition to the HR diagram and number counts.

Quite recently we found this star surrounded by an AG Car-like nebula. The kinematic age of this nebula is about 20 000 years. DE JAGER: A rate of mass loss of 10- 4 MG/yr fits very well to the value observed near the instability limit. Hence we came to the interesting conclusion that just the 'average' rate of mass loss of hypergiants is sufficient to explain evolutionary the absence of stars beyond the HD limit, and that the addition of a significant contribution by episodical mass loss may not be needed.

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