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 college of Utrecht the place he has held a Chair for Stellar Astrophysics, later became house Physics, because 1958. Cees de Jager, as he prefers to be known as by way of his buddies, has had an lively and winning lifestyles in technological know-how. His curiosity in astronomy used to be raised by means of his father less than the transparent skies of Celebes (Indonesia). He began a examine in physics and astronomy as a pupil of the past due M. Minnaert in Utrecht in the course of international conflict II. whilst in 1943 the occupying forces recruited scholars who didn't wish to signal the assertion 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 idea of the 21 em radiation of impartial hydrogen and de Jager all started the observations of variable stars within the pitch darkish nights of a rustic at conflict. The learn of Beta Cepheids quick ly aroused from sleep his curiosity which was once stored during the years. In 1958 he geared up a global crusade to watch 12 Lac spectroscopically and photometrically, which used to be an excellent success.
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Extra resources 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
However, as shown by Percy (1980), in no case is a radial mode known to be absent. In addition, according to the calculations by Lesh and Aizenman (1974), the value of the pulsation quantity Q is generally in favour of the 1st overtone for these radial modes. 2. Line Profile Variations The variation the mode spectrometers by Petrie theoretically of the photospheric line profiles became very useful for identification when photoelectric high-resolution came into use. The pioneer work was done observationally (1954) on the extreme P Cephei star BW Vul and by Osaki (1971) who calculated the line profile OBSERVATIONS AND INTERPRETATIONS OF STELLAR PULSATIONS 25 variations for various cases of non-radial pulsations.
Astrophys. Supp1. , 1985, Astron. Astrophys. , 1986, Astron. Astrophys. , 1976, Astron. Astrophys. P. , 1981, Intrinsic Variability in B stars, in Workshop on Pulsating B stars, Eds. N. and C. Sterken, Observatoire de Nice, p. , 1967, Oscillation Theories of Magnetic variable stars, in The magnetic and related stars, Ed. C. Cameron, Mono Book Corporation, Baltimore, p. , 1984, Astron. Astrophys. , 1978, Acta Astron. , 1967, Z. f. , 1981, Mode identification in pulsating B stars, in Workshop on pUlsating B stars, Eds.
23 H. 1. G. L. M. Lamers and C. W. H. ), Instabilities in Luminous Early Type Stars, 23-38. © 1987 by D. Reidel Publishing Company. 24 G. 1. Classical cepheids. In the case of the classical cepheids with period shorter than 10 days the agreement is fairly good between the observational log R - log P relation, based on the results of the Baade-Wesselink method (Burki, 1985), and the theoretical relation based on cepheid models (Fernie, 1984). 1 (3) The log R - log P diagram can be used to select the overtone pulsators: at a given log R value these stars have a lower log P value with respect to the standard relation.
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 by Roberta M. Humphreys (auth.), Henny J. G. L. M. Lamers, Camiel W. H. De Loore (eds.)