Search Results for mass-loss-and-evolution-of-o-type-stars

EVOLUTION OF O STARS AND THE WR CONNECTION Peter S. Conti” Joint Institute for Laboratory Astrophysics, ... CO 80309 ABSTRACT The stellar wind mass loss rates of at least some single Of type stars appear to be sufficient to remove much ...

Author: P.S. Conti

Publisher: Springer Science & Business Media

ISBN: 9789400994522

Category: Science

Page: 520

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The organization of this Symposium had its beginnings at the International Astronomical Union General Assembly in Grenoble in 1976. The initial "rounding up" of the Scienti fic Organizing Committee was begun by Drs. Snow and Swings; most of us who became the eventual organizing committee met a few times during the Assembly and formulated the essential outlines of the meeting. Extensive correspondence with all the committee subsequently established the program. The idea was to bring together both observers and theoreticians to discuss the stellar winds and mass loss rates and their effects on evolutions of O-type stars. On the observational side, there are now spectroscopic data from the far UV to the near IR regions concerning the stellar winds. There is also information about the free-free emission in the wind from the IR and radio portions of the spectrum. Fortunately, these different detection methods give more or less the same mass loss rate for the one star, s Pup" which has been observed at all wavelengths. One of the intents of the first three sessions of this Symposium is to outline the eXisting data on mass loss rates as it per tains to the O-type stars.
2012-12-06 By P.S. Conti

Symposium No. 83 held at Vancouver Island, Canada, June 5-9, 1978

Author: International Astronomical Union. Symposium

Publisher: Springer

ISBN: UVA:X001320289

Category: Science

Page: 501

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Symposium No. 83 held at Vancouver Island, Canada, June 5-9, 1978

PANAGIA: In Our sample the Of stars do not exhibit any larger mass loss rate than "normal" O-type stars with equal spectral type and luminosity class. In particular, for main sequence stars with not Of characteristic we find log M/L ...

Author: C. Chiosi

Publisher: Springer Science & Business Media

ISBN: 9789400985001

Category: Science

Page: 570

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The IAU Colloquium No. 59, "The effects of mass loss on Stellar Evolution" was held on September 15-19, 1980 at the International Centre for Theoretical Physics, Miramare, Trieste (Italy), under the auspices of the IAU Executive Co~ mittee and the Italian National Council of Research. The planning of this conference began two years ago du ring the IAU Symposium No. 83 "Mass loss and evolution of 0 type stars" (Qualicum Beach, Victoria, Canada) when we felt that mass loss and its effects on the evolution of stars was too broad a subject for being confined to 0 type stars only. Therefore we thought that a conference dealing with the general problem of mass loss across the whole HR diagram would have been of interest to all people working in the field. The main idea was that bringing together Astronomers and Astrophysicists of the widest range of interests and e~ pertize - all in some way related to the problem of mass loss from stars - would have spurred thorough discussions on the many aspects and implications of this topic. We hope this goal has been achieved. Furthermore, the most recent observational and theoreti cal developments on the problem of mass loss from early ty pe stars avoided this meeting to be a simple updating of the Qualicum Beach Symposium as far as this issue is concerned.
2012-12-06 By C. Chiosi

Mass Loss and Evolution of O-type Stars', IAU Symp. 83,291. Niemelä, V. S. and Mendez, R. H.: 1974, Astrophys. J. Letters 187, L25. Niemelä, V. S. and Sahade, J.: 1979, in P. S. Conti and C. W. H. de Loore (eds.), “Mass Loss and ...

Author: C. de Jager

Publisher: Springer Science & Business Media

ISBN: 9789400990302

Category: Science

Page: 470

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No part of the Hertzsprung-Russell diagram shows a more pronounced diversity of stellar types than the upper part, which contains the most luminous stars. Can one visualize a larger difference than between a luminous, young and extremely hot Of star, and a cool, evolved pulsating giant of the Mira type, or an S-type supergiant, or - again at the other side of the diagram - the compact nucleus of a planetary nebula? But there is order and unity in this apparent disorder! Virtually all types of bright stars are evolutionally related, in one way or the other. Evolution links bright stars. In many cases the evolution is speeded up by, or at least intimately related to various signs of stellar instability. Bright stars lose mass, either continuously or in dramatic sudden events, they vibrate or pulsate - and with these tenuous, gigantic objects this often happens in a most bizarre fashion. Sometimes the evolution goes so fast that fundamental changes are observable in the time span of a human's life - several of such cases have now been identified.
2012-12-06 By C. de Jager

The influence of SW: we have to separate SW mass loss in O type stars from the SW mass loss in LBV's. a. The Mdot in O type stars: when current semi-empirical Mdot relations are used in evolutionary codes we conclude that SW mass loss ...

Author: D. Vanbeveren

Publisher: Springer Science & Business Media

ISBN: 9789401110808

Category: Science

Page: 490

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Massive stars occupy an exceptional place in general astrophysics. They trigger many if not all of the important processes in galactic evolution whereas due to their intrinsic brightness, they offer the (only until now) possibility to study the stellar content and stellar behaviour in distant galaxies. The last, say, 25 years, massive stars have been the subject of numerous meetings discussing the influence of massive stars on population synthesis, the number distribution of different types of massive stars, the LBV phenomenon, WR stars, X-ray binaries, stellar winds in massive stars, chemical pecularities in massive stars, supernova explosions of massive stars and the important SN1987A event, the influence of massive stars and chemical evolution of galaxies. It is clear that without a theory of stellar evolution, the study of these topics loses a lot of its significance. Massive star evolution therefore got a chance in these meetings, but rarely as a prime subject. The state of the art, the physical processes and the uncertainties in stellar evolution were barely touched. Even more, the influence of close binaries in all these massive star meetings slowly disappeared the last, say, 13 years without any scientific justification, although a significant fraction of stars occurs in close binaries with periods small enough so that both components will interact during their evolution. Denying the binaries or not discussing their influence on results and conclusions, makes the latter very uncertain or even completely unreliable.
2012-12-06 By D. Vanbeveren

Massive O-type stars stars are characterized by dense, highly-supersonic mass outflows. These stellar winds have a ... Mass-loss rates are therefore a crucial parameter of stellar evolution models. Aside from their effect on the ...

Author: Wolf-Rainer Hamann

Publisher: Universitätsverlag Potsdam

ISBN: 9783940793331

Category:

Page: 254

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From IAU colloquium 59 on effects of mass - loss of stellar evolution ; Trieste , Italy ( 15 Sep 1980 ) . The mechanisms by which early type ( O and B ) stars lose mass is investigated . The phenomena occurring close to the photosphere ...

Author:

Publisher:

ISBN: UOM:39015026171861

Category: Power resources

Page:

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hydrogen burning, so that shell hydrogen burning does not occur; a huge stellar mass loss rate has a comparable effect. ... types: for WolfRayet stars and the hottest O-stars they are of the order of 4000 km s−1; for lower mass stars ...

Author: C. de Loore

Publisher: Springer Science & Business Media

ISBN: 9789401125024

Category: Science

Page: 458

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Classical stellar evolution theories have undergone some drastic changes in recent decades. New insights into the development of stellar interiors were obtained from studying stars in various stages of their lives, as well as with the help of fast computers, which gave a boost to the branch of numerical modelling of stellular structure and evolution. This book is divided into two parts. The first part deals with the general aspects of stellular structure and evolution including a chapter on numerical modelling. The second part deals with specific evolutionary aspects of single and binary stars with a variety of masses. The last chapter gives several models of stars with specific masses. The book is intended as an introduction for students, as well as a reference for researchers.
2012-12-06 By C. de Loore

Macroclumping as solution of the discrepancy between Hα and P v mass loss diagnostics ... The WR and O-type star population predicted by massive star evolutionary synthesis. New Astronomy, 3,443– 492.

Author: Giacomo Beccari

Publisher: Cambridge University Press

ISBN: 9781108428583

Category: Science

Page: 358

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An advanced review of how binary stars affect stellar evolution, presenting results from state-of-the art models and recent observations.
2019-04-30 By Giacomo Beccari

83 on "Mass Loss and Evolution of O-type Stars" held at Qualicum Beach, Vancouver Island, Canada - WR stars generally figure prominently in O-star meetings and vice versa! Following general approval by the IAU Executive Committee the ...

Author: C. de Loore

Publisher: Springer Science & Business Media

ISBN: 9789400979109

Category: Science

Page: 636

View: 469

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The formative ideas for this symposium originated in 1978 at the IAU Symposium No. 83 on "Mass Loss and Evolution of O-type Stars" held at Qualicum Beach, Vancouver Island, Canada - WR stars generally figure prominently in O-star meetings and vice versa! Following general appro val by the IAU Executive Committee the initial ideas were cemented at a subsequent meeting, IAU Colloquium No. 59 on "The Effects of Mass Loss on Stellar Evolution", held at Miramare, Trieste, Italy in 1980, which was attended by the ma,jority of the present Scientific Organising Committee and at which meeting the outline programme for this symposium was formulated. 1981 was considered an appropriate year in which to hold a meeting on WR stars, since the last IAU Symposium devoted to this stellar class had been held a decade earlier, in Buenos Aires (IAU Sym posium No. 49), and during this intervening period a wealth of new observational material had been obtained for WR stars together with significant advances on the theoretical front. The venue for this sym posium was chosen from the requirement, which can be inferred from the above, that a meeting on 'hot' stars take place in an appropriate, sunny climate and followed upon the excellent suggestion of Dr. C. Firmani to hold the symposium in Mexico.
2012-12-06 By C. de Loore