5 edition of Pulsation, Rotation and Mass Loss in Early-Type Stars (International Astronomical Union Symposia) found in the catalog.
August 31, 1994
Written in English
|Contributions||Luis A. Balona (Editor), Huib F. Henrichs (Editor), Jean Michel Le Contel (Editor)|
|The Physical Object|
|Number of Pages||572|
CiteSeerX - Document Details (Isaac Councill, Lee Giles, Pradeep Teregowda): Abstract. The detection of possible nonradial pulsation modes among some λ Bootis stars offers the prospect of using asteroseismology to determine their masses and ages, thereby testing competing theories for the origin of their chemical peculiarities. As a step toward this goal, we conducted multi-site photometric. All β Cephei stars for which long-term behavior of their pulsation periods could be derived from observations are listed in Table s 1 and 2 are self-explanatory. The third column gives the number of pulsation modes. Column 4 contains the pulsation periods; for stars in which more than one mode is seen, the period of the mode with the largest photometric amplitude is listed.
New York, Mass Market Paperback. Condition: Very Good. A Del Rey Books Mass Market Original. + pp. Clean, crisp pages. Slight wear to edges of cover. Solid binding. Pulsation, Rotation and Mass Loss in Early-Type Stars (International Astronomical Union Symposia) Mass-Losing Pulsating Stars and Their Curcumstellar Matter. tions for rotating early-type stars, but in many cases our The e ect of rotation on the velocity eld of pulsation is included in Sect. In Sect we derive an expression for the ratio of the horizontal to the vertical pulsational amplitude, k,which P and are the mass density, the pressure.
The book is suitable for researchers and graduate students interested in the astrophysics of cool stars and the sun, including abundances, magnetohydrodynamics, circumstellar disks, stellar rotation, pulsation and mass loss. Theoretical Predictions for Mass Loss Rates: Rotation & Pulsation S. R. Cranmer, Massive star winds: radiative driving • The Castor, Abbott, & Klein (CAK) theory gives a prediction for mass loss rates: • Metallicity dependence (largely) verified by observations in SMC and LMC, but it flattens out for lower Z (Vink ).
Census of population of Ireland, 1956
Summary of aerological observations obtained by means of kites, airplanes and sounding balloons in the United States
Memoirs and correspondence of Viscount Castlereagh...
A study of history
Agreement as to hours and holidays
list of source materials for teachers of college hygiene
Human rights litigation promoting international law in U.S. courts
French politics and public policy
Maths at work
Aspects of extradition law
Topics in quantum field theory
Pulsation, Rotation and Mass Loss in Early-Type Stars Proceedings of the nd Symposium of the International Astronomical Union, Held in Antibes-Juan-Les-Pins, France, October 5–8, Pulsation, Rotation and Mass Loss in Early-Type Stars Proceedings of Pulsation nd Symposium of the International Astronomical Union, Held in Antibes-Juan-Les-Pins, France, October 5–8, Editors: Balona, Luis A., Henrichs, Huib F., Le Contel, Jean Michel (Eds.) Free Preview.
PDF | On Jan 1,Luis A. Balona and others published Pulsation, rotation and mass loss in early-type stars | Find, read and cite all the research you need on ResearchGate. Symposium - International Astronomical Union, Volume (Pulsation, Rotation and Mass Loss in Early-Type Stars)pp.
; This volume was published under a Cited by: 2. Books-Received - Pulsation Rotation and Mass Loss in Early Type StarsAuthor: L.
Balona, H. Henrichs, J. Le Contel. PULSATION, ROTATION AND MASS LOSS IN EARLY-TYPE STARS: Editors: LA Balona, HF Henrichs, JM LeContel: Place of Publication: DORDRECHT: Publisher: Kluwer Academic Publishers: Pages: Number of pages: 2: ISBN (Print) Publication status: Published.
Pulsation, Rotation and Mass Loss in Early-Type Stars. Pulsation, Periodic Variations and Mass Loss in Be Stars. In: Balona L.A., Henrichs H.F., Le Contel J.M.
(eds) Pulsation, Rotation and Mass Loss in Early-Type Stars. International Astronomical Union / Union Astronomique Internationale, vol Buy this book on publisher's site. Title: Book Review: Pulsation, rotation and mass loss in early-type stars (IAU symposium ) / Kluwer, Journal: Space science reviews, vol.
76, no.p. () Bibliographic Code: SSRv B. Complete bibliographic record Other article options Print this article. Pulsation, Rotation and Mass Loss in Early-Type Stars: Proceedings of the nd Symposium of the International Astronomical Union, Held in Antibes-Juan-Les-Pins, France, October 5–8, ; Biopharmaceuticals in Plants: Toward the Next Century of Medicine.
For the hotter stars, recent work suggests a strong link between the type of pulsation behavior, the mass loss rates, and the rotation velocity. How Effective is Rotation in Enhancing the Rate of Mass Loss in Early Type Stars.
Mass Loss and Rotation in Central Stars of Planetary Nebulae. adshelp[at] The ADS is operated by the Smithsonian Astrophysical Observatory under NASA Cooperative Agreement NNX16AC86A. DANS is an institute of KNAW and NWO.
Driven by data. Go to page top Go back to contents Go back to site navigation. SAO/NASA Astrophysics Data System (ADS) Title: Optical Resolution of Be Star Envelopes Authors: Vakili, F., Mourard, D., & Stee, P. Journal: Pulsation; rotation; and mass loss in early-type stars: proceedings of the nd symposium of the International Astronomical Union held in Antibes; Juan-les-Pins; France; October ; Edited by Luis A.
Balona, Huib F. Henrichs, and Jean Michel Le. Get this from a library. Pulsation, rotation, and mass loss in early-type stars: proceedings of the nd symposium of the International Astronomical Union held in Antibes, Juan-les-Pins, France, October[Luis A Balona; Huib F Henrichs; Jean Michel Le Contel; International Astronomical Union.
Symposium]. The structure of the circumstellar material in Be stars Published in Pulsation, rotation and mass loss in early type stars, proceedings of IAU symposium- Pulsation, Rotation and Mass Loss in Early-Type Stars de Luis A. Balona, Huib F. Henrichs( Academic Publishers) Isbn: € In this Symposium, researchers specializing in pulsation, rotation, magnetic fields and stellar winds are brought together for the first time in order to broaden our understanding of O and B stars.
Book-Review - Rotation in the Solar System. such as probably are the W Serpentis stars, larger and more important disks can be anticipated.
Pulsation Rotation and Mass Loss in Early Type. Star - Star - Pulsating stars: An impressive body of evidence indicates that stellar pulsations can account for the variability of Cepheids, long-period variables, semiregular variables, Beta Canis Majoris stars, and even the irregular red variables.
Of this group, the Cepheid variables have been studied in greatest detail, both theoretically and observationally. The American Astronomical Society (AAS), established in and based in Washington, DC, is the major organization of professional astronomers in North America.
Its membership of. Get this from a library. Pulsation, Rotation and Mass Loss in Early-Type Stars: Proceedings of the nd Symposium of the International Astronomical Union, Held in Antibes-Juan-Les-Pins, France, October[Luis A Balona; Huib F Henrichs; Jean Michel Contel] -- In this Symposium, researchers specializing in pulsation, rotation, magnetic fields and stellar winds are.
The theory of radiation-driven wind including stellar rotation is reexamined. After a suitable change of variables, a new equation for the mass-loss rate is derived analytically.
The solution of this equation remains within 1% confidence when compared with numerical solutions.Understanding Stellar Evolution is based on a series of graduate-level courses taught at the University of Washington since It describes the structure and evolution of stars, with emphasis on the basic physical principles and the interplay between the different processes inside stars.
Based on these principles, the evolution of low- and high-mass stars is explained from their formation.future models of stellar evolution. There may be a need, for instance, to include processes such as rotation, mass loss, and magnetic fields. There may also be non-evolutionary processes which are contributing to the period changes.
known constant period P. When (O–C) is plotted against time.