2 edition of Instabilities in evolved super- and hypergiants found in the catalog.
Instabilities in evolved super- and hypergiants
|Statement||C. de Jager and H. Nieuwenhuijzen, editors.|
|Series||Verhandelingen, Afd. Natuurkunde, Eerste reeks ;, d. 36, Verhandelingen der Koninklijke Nederlandse Akademie van Wetenschappen, Afd. Natuurkunde., d. 36.|
|Contributions||Jager, C. de 1921-, Nieuwenhuijzen, H.|
|LC Classifications||Q57 .A532 d. 36, QB843.S9 .A532 d. 36|
|The Physical Object|
|Pagination||199 p. :|
|Number of Pages||199|
|LC Control Number||93110770|
A hypergiant (luminosity class 0 or Ia +) is among the very rare kinds of stars that typically show tremendous luminosities and very high rates of mass loss by stellar winds. The term hypergiant is defined as luminosity class 0 (zero) in the MKK system.
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ISBN: OCLC Number: Notes: "Proceedings of the international colloquium, Amsterdam, 26 February-1 March "--Preliminary page. Instabilities in evolved super- and hypergiants. Amsterdam ; Oxford: North-Holland, (OCoLC) Material Type: Conference publication, Government publication, National government publication: Document Type: Book: All Authors / Contributors: C de Jager; H Nieuwenhuijzen; Koninklijke Nederlandse Akademie van Wetenschappen.
Afdeling. Super- and hypergiant masers and related phenomena in extreme red objects; the relationship between masers, dust and atmospheric or envelope instabilities. Humphreys R. M.:in G. De Jager and H.
Nieuwenhuijzen (eds.), Instabilities in evolved super-and hypergiants, 13 Google ScholarCited by: 2. Can classical model atmospheres be of any use for the study of hypergiants Gustafsson, B. Plez, B. Abstract. Not Available. Publication: Instabilities in Evolved Super- and Hypergiants. Pub Date: Bibcode: 86G full text sources.
ADS |Author: B. Gustafsson, B. Plez. Observations of A through M-type super- and hypergiants and related groups of stars; interpretation of the data. instabilities in evolved super- and hypergiants. At the conference he presented the idea that stellar microturbulence is strongly related to the physics of at-mospheric shock waves.
Through numerical integrations of the hydrodynamics equations an observable microturbulent velocity is computed, assuming that the. Abstract. The paper gives a summary of the situation mid of theory and observations regarding massive stars. I describe: stellar mass loss and its implications, pre-main-sequence evolution, the main sequence, problems of atmospheric instability, Luminous Blue Supergiants, Yellow Hyper-giants, Wolf—Rayet stars and by: 1.
The term hypergiant is defined as luminosity class 0 (zero) in the MKK system. However, this is rarely seen in the literature or in published spectral classifications, except for specific well-defined groups such as the yellow hypergiants, RSG (red supergiants), or blue B (e) supergiants with emission spectra.
adshelp[at] The ADS is operated by the Smithsonian Astrophysical Observatory under NASA Cooperative Agreement NNX16AC86A. Maeder, A.in: C. de Jager & H. Nieuwenhuijzen (eds.), Instabilities in Evolved Super-and Hypergiants (Amsterdam: North Holland), p.
Google ScholarAuthor: D. Schaerer, A. De Koter, W. Schmutz. F and G Supergiants with Large Infrared Excesses. Instabilities in Evolved Super- and HypergiantsInstabilities in Evolved Super- and Hypergiants. Cite this publication. Origin and definition . Inthe astronomers Feast and Thackeray used the term super-supergiant (later changed into hypergiant) for stars with an absolute magnitude brighter than M V = −7 (M Bol will be larger for very cool and very hot stars, for example at least − for a B0 hypergiant).
InKeenan suggested that the term would be used only for supergiants showing at least. New models of massive stars have been calculated as a part of a project aimed at the construction of an extended grid Bertelli G., Bressan A.: a, In Instabilities in Evolved Super and Hyper giants, ed.
de Jager, H. Nieuwenhuijzen. Amsterdam In Instabilities in Evolved Super and Hypergiants,ed. de Jager, H Cited by: 2. A greatly improved census of the likely progenitor class, including the most luminous evolved stars, the luminous blue variables (LBVs), and the warm and cool hypergiants is now needed for a.
Infrared astronomical satellite (IRAS) catalogs and atlases (v ; v ) Instabilities in Evolved Super and Hypergiants () The Instabilities in evolved super- and hypergiants book of variable stars with their environment.
IAPPP International Amateur-Professional Photoelectric Photometry Communications (v 7/; v) IAUC. A 'read' is counted each time someone views a publication summary (such as the title, abstract, and list of authors), clicks on a figure, or views or downloads the full-text.
the instabilities that constrain and deﬁne stellar evoluti on in the upper reaches of the HR diagram. Relating to this, the lack of secu- lar evolution amongst the cool hypergiants and the presence of both high-luminosity yellow hypergiants and red supergiants within. Supergiants are evolved high-mass stars, larger and more luminous than main-sequence stars.
O class and early B class stars with initial masses around 10– M ☉ evolve away from the main sequence in just a few million years as their hydrogen is consumed and heavy elements start to appear near the surface of the star.
These stars usually become blue supergiants, although it is possible. SAO/NASA Astrophysics Data System (ADS) Title: Waves and instabilities; static and dynamic models of the atmospheres and envelopes of evolved super- and hypergiants.
Journal: Koninklijke Nederlandse Akademie van Wetenschappen. Verhandlingen, Afd. Natuurkunde. Eerste Reeks, Proceedings of the International Colloquium, Amsterdam, 26 February - 1 MarchAmsterdam:. most luminous objects in their spectral class. The yellow hypergiants and their characteristics have been reviewed recently by de Jager ().
There are indications (relatively small mass; overabundance of Na and N with respect to the Sun) that yellow hypergiants are evolved stars, evolving from the red supergiant phase to the blue phase. de Jager's research works with 1, citations and 1, reads, including: Pulsations, eruptions, and evolution of four yellow hypergiants.
The title supergiant, as applied to a star, does not have a single concrete definition. The term giant star was first coined by Hertzsprung when it became apparent that the majority of stars fell into two distinct regions of the Hertzsprung–Russell diagram.
We have determined the location of the line-opacity modified Eddington limit for stars in the LMC using the most recent atmosphere models combined with a precise mapping to the H-R diagram through up-to-date stellar evolution calculations. Contributed talk, Int. Conf. on Instabilities in Evolved Super- and Hypergiants, Amsterdam, The Netherlands, Feb ( Mb pdf) The Instability Parameters of Stellar Atmospheres.
Contributed talk, Int. Conf. on Instabilities in Evolved Super- and Hypergiants, Amsterdam, The. Nieuwenhuijzen's 63 research works with citations and reads, including: Pulsations, eruptions, and evolution of four yellow hypergiants.
Pijpers: On the propagation of sound waves in a stellar wind traversed by periodic strong shocks 11 Landau, L. D., Lifshitz, E. M.,Course of TheoreticalFile Size: KB. New models of massive stars have been calculated as a part of a project animed at the construction of an extended grid of stellar tracks for several metallicities, covering all the main evolutionary phases of low, intermediate and massive stars, with updated physics.
After a brief description of the input physics, we discuss the properties of the stellar content of young clusters as a Cited by: 2. hypergiants are the absolute largest stars in the universe in relation to there tremendous mass and luminosity, super giants are one step down from hypergiants, hypergiant to luminosity.
supergiant to luminosity. giant.0 to -4 luminosity. This query page only provides access to articles that have been scanned by the ADS. If you want to access every article from a particular journal, please use the Journal/Volume/Page Query Page.
All articles are copyrighted by the publisher of the article. Hypergiants are born through the same process as other stars and shine the same way, but beyond that, they are very, very different from their tinier siblings.
Learning about Hypergiants Hypergiant stars were first identified separately from other supergiants because they are significantly brighter; that is, they have a larger luminosity than. Instabilities in evolved super- and hypergiants Instabilities in luminous early type stars: proceedings of a workshop in honour of professor Cees De Jager on the occasion of his 65th birthday held in Lunteren, The Netherlands, April Post-RedSupergiants 3 LBVs have evolved oﬀ the RSG (e.g.
Lamers et al. The situation proves even less settled for the B[e] supergiants, it is possible that they constitute a rapidly rotating sub-sample of the objects that evolve through the LBV phase. In this paper, we focus on the evolutionary phase that immediately follows.
Astron. Astrophys.() References. SIMBAD Objects; Abt H. A.,A NASA ADS; Altamore A., Giangrande A., Viotti R.,A&AS 49, census of the likely progenitor class, including the most luminous evolved stars, the Luminous Blue Varaibles (LBVs), and the warm and cool hypergiants is now needed for a complete picture of the ﬁnal pre-SN stages of very massive stars.
We have begun a survey of the evolved and unstable luminous star populations in several nearby resolved. and the warm and cool hypergiants is now needed for a complete picture of the ﬁnal pre-supernova stages of very massive stars. We have begun a survey of the evolved and unstable luminous star populations in several nearby resolved galaxies.
In this second paper on M31 and M33, we review the spectral characteristics, spectral energy. Other warm or yellow hypergiants include the Galactic stars HR and HR A [41,42,43].
These hypergiants are visually bright and relatively nearby, which has made them important laboratories for study of late-stage evolution. Interestingly, de Jager suggests that all of the yellow hypergiants are post-red supergiants.
During blueward Author: Michael S. Gordon, Roberta M. Humphreys. Luminous Stars. Introduction to the Program Luminous Blue Variables, Hypergiants, and Supernova Impostors In quiescence an LBV or S Doradus variable is a moderately evolved hot star, with a B-type supergiant or Of-type/late-WN classification.
subphotospheric gravity-mode instabilities, and super-Eddington winds (see Humphreys and. A yellow supergiant star is a star, generally of spectral type F or G, having a supergiant luminosity class (e.g.
Ia or Ib). They are stars that have evolved away from the main sequence, expanding and becoming more luminous. Yellow supergiants are smaller than red supergiants; naked eye examples include Canopus and of them are variable stars, mostly pulsating Cepheids such as δ.
A yellow hypergiant is a massive star with an extended atmosphere, a spectral class from A to K, and, starting with an initial mass of about 20–60 solar masses, has lost as much as half that mass.
They are amongst the most visually luminous stars, with absolute magnitude (MV) around −9, but also one of the rarest with just 15 known in the Milky Way and six of those in just a single cluster. Nieuwenhuijzen, editors, Instabilities in Evolved Super- and Hypergiants, pages 98 –Proceedings of the Royal Dutch Academy of Sciences, Sect.
Two Decades of Hypergiant Research DELSY: A Dutch accelerator and storage ring used for nuclear physics is being moved to Dubna, to add to Russia’s Synchrotron capability.REFERENCES.
Abbott, D.C. Ap. J. ; Abbott, D.C., Bieging, J.H., Churchwell, E., Torrees, A.V. Ap. J. Abbott, D.C., Conti, P.S. A yellow hypergiant is a massive star with an extended atmosphere, a spectral class from A to K, and, starting with an initial mass of about 20–60 solar masses, has lost as much as half that are amongst the most visually luminous stars, with absolute magnitude (M V) around −9, but also one of the rarest with just 15 known in the Milky Way and six of those in just a single cluster.