Results 11 to 20 of about 1,916 (218)
Dynamics of the Wind of LBV Stars [PDF]
Symposium - International Astronomical Union, 1995 Luminous Blue Variables are among the brightest objects and lie at the Humphreys-Davidson empirical limit of maximum luminosity (Lamers 1986b). A distinct feature of these stars is the higher rate of mass loss and the relatively lower terminal velocity than for other stars of the same spectral type.
G. L. Israelian +2 more
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Winds in hot, subluminous stars [PDF]
Symposium - International Astronomical Union, 1979 Recent observations with the International Ultraviolet Explorer (IUE) satellite show that two very different types of hot stars have stellar winds: not only do the young, massive OB stars (the subjects of our discussion in this symposium, so far) undergo high-velocity mass-loss, but so also do hot evolved, solar mass stars, among them the central star ...
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Wind Variability of LBV Stars [PDF]
International Astronomical Union Colloquium, 1993 AbstractGeneral properties of Luminous Blue Variables (LBV) have been reviewed by Lamers (1987). The LBV’s are all close to the Humphreys-Davidson luminosity upper limit. The semi periods of the photometric microvariations with ΔV ~ 0.1m are about twice as large as for normal supergiants of the same L and Teff, and 4-20 times larger than the ...
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AIP Conference Proceedings, 1996 Recent spectroscopic results from the far ultraviolet and X-ray region coupled with infrared observations demonstrate that winds from luminous stars can be warm (300000K) and fast (speeds of several hundred km s—1) linking the hot solar wind to the cool, massive winds of luminous M-type supergiant stars.
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Smooth winds and clumped winds for early-type stars [PDF]
Symposium - International Astronomical Union, 1994 The use of the IR and radio continuum as a clumping indicator for the stellar wind of early-type stars is investigated.
Blomme, Ronny, Runacres, Mark
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Blobs in the Winds of Wolf-Rayet Stars [PDF]
International Astronomical Union Colloquium, 1989 Abstract. Concentrations of material have been observed to propagate in the winds of many W-R stars. These are short-lived, stochastic features of unknown origin.
C. Robert, L. Drissen, A. F. J. Moffat
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Radiatively driven winds of OB stars [PDF]
Symposium - International Astronomical Union, 1994 We newly calculated the line radiative force with 520,000 atomic lines, which is twice as many as those of Abbott (1982), for OB supergiants. Our results are as follows. (1) The mass loss rates for O stars with Teff = 50,000K are seven times as large as Abbott's (1982) because of contribution from Fe iv lines.
Michihiro R. Shimada +3 more
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Winds of hot stars in the Magellanic Clouds [PDF]
Symposium - International Astronomical Union, 1991 The Magellanic Clouds provide a unique laboratory in which to study the metallicity dependence of stellar winds. If proved by observations, such a dependence would have important consequences for stellar evolution, nucleosynthesis, energy balance of the ISM, star formation and so on.
R. P. Kudritzki +3 more
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Stellar-winds and coronas in cool stars [PDF]
International Astronomical Union Colloquium, 1980 AbstractRecent observational and theoretical results are reviewed that pertain to the presence and characteristics of stellar coronae and winds in late-type stars. It is found that stars - principally dwarfs - exist with “hot” coronae similar to the Sun with thermally driven winds.
A.K. Dupree, L. Hartmann
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Pediatric Blood &Cancer, EarlyView.ABSTRACT Background and Aims Infant bone and soft tissue neoplasms present distinct clinical challenges and lack large‐scale data to inform treatment decisions. This study aims to characterize bone and soft tissue neoplasms in infants in Canada and to compare their outcomes with those of older pediatric patients.
Samuel Sassine +21 more
wiley +1 more source