Titlebook: Cyclical Variability in Stellar Winds; Proceedings of the E Lex Kaper,Alexander W. Fullerton Conference proceedings 1998 Springer-Verlag Be

Carcinoma

Infelicity

Variable Dust Emission Observed in Mirasins when T < 1200 K in the shell. During their pulsational cycle Miras vary in luminosity, forcing the dust that has formed in the circumstellar shells alternately to evaporate and re-condense in the inner parts of their shells. Hence, emission from the dust will vary during the pulsational cycle. T

dithiolethione

Systematic Variability in OB-Star Winds. I summarize evidence for cyclic wind variability and rotational modulation, based on extended time-series UV data sets (including the ‘. MEGA Campaigns’). The constraints provided by these data indicate that the modulating ‘clocks’ apparent in some hot star winds must ultimately have an origin at

恫嚇

MEAN

encyclopedia

Jaydip Singh,Srishti Nagu,Jyotsna Singhnclude the differential rotation of the fluid and the influence of the radiative force in an optically thin stellar atmosphere (Kakouris & Moussas 1997). The solutions use a new thermo-radiative mechanism in order to describe self-consistently outflows from early-type supergiants, for which the radi

cunning

CEDE

https://doi.org/10.1007/978-3-642-16809-3nuum emission. Our test cases include the stars . TrA (K4 II), . Vel (K4 Ib-II), and . Aur (K4 Ib + B5 V). Of particular interest is the sensitivity of the line profiles to the wind parameters ., .., .., β, and ... We are finding that while accurate and reliable values of . are difficult to obtain,

Proclaim

Example 1 Audio FPGA Passthroughicki (1992). They are repeated here to compare with the unpublished spectrum from 1978 (thick lines). Although not cyclical, the variability in the wind is apparent. Non-LTE analysis (see Gesicki 1992) results in a mass-loss rate of about 5 × 10. M. yr. in 1978, which is higher than in 1970. These r

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