By J. B. Hutchings (auth.), P. S. Conti, C. W. H. De Loore (eds.)
ISBN-10: 9027709890
ISBN-13: 9789027709899
ISBN-10: 9400994524
ISBN-13: 9789400994522
The association of this Symposium had its beginnings on the overseas Astronomical Union normal meeting in Grenoble in 1976. The preliminary "rounding up" of the Scienti fic Organizing Committee was once started by way of Drs. Snow and Swings; so much people who grew to become the eventual organizing committee met a couple of times in the course of the meeting and formulated the basic outlines of the assembly. huge correspondence with the entire committee therefore confirmed this system. the assumption was once to collect either observers and theoreticians to debate the stellar winds and mass loss premiums and their results on evolutions of O-type stars. at the observational aspect, there at the moment are spectroscopic information from the some distance UV to the close to IR areas in regards to the stellar winds. there's additionally information regarding the free-free emission within the wind from the IR and radio parts of the spectrum. thankfully, those various detection equipment provide roughly an identical mass loss price for the only celebrity, s domestic dog" which has been saw in any respect wavelengths. one of many intents of the 1st 3 classes of this Symposium is to stipulate the present information on mass loss premiums because it in step with tains to the O-type stars.
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Extra resources for Mass Loss and Evolution of O-Type Stars
Sample text
Unfortunately, the high rotation 1eads to weak 1 ines and difficul ties in measuring velocities, so that high quality data would be required. I would like to emphasise a pet point here. In the extreme cases a stratified expanding envelope will underestimate V sin i measured from absorption 1 ines. Thi s leads directly to a controversy over HD 153919 whose absorption 1 ine V sin i is much slower than synchronous. My recent light curve analysis l"Hutchings 1978) suggests that rotation must be synchronous (as do circularisation arguments, and V sin 1 estimates from emission lines).
We probably have here a real runaway object! Hutchings: HD l48937? Can you estimate the size and age of the nebula around Pismis: In my paper on NGC 6164-5 I have given an estimate of the size of the nebula as 3 pc and an age of 4-5 x 10 3 yrs. These are however very rough estimates since the distance of the nebula, and star, is only approximate. Niemela: Are there studies of any of the central stars to determine if they are binaries? If they are binaries the mass loss could be through the two external equilibrium points.
4. Ml-67 This object is so far considered to be a planetary nebula and is the only one to have a central WR star of the nitrogen sequence (WN 8). The structure of this nebula, dominated by blobs, shows again bi-symmetry. / as in the former two H II 1regions. But clearly, the outer filaments are moving away from the central star while the regions closer to the star show expansion (Pi§mi§ and Recillas-Cruz, 1971). Thus, here again, E we have a nebula formed probably by mass ejected from the central star.
Mass Loss and Evolution of O-Type Stars by J. B. Hutchings (auth.), P. S. Conti, C. W. H. De Loore (eds.)
by Mark
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