Last edited by Mazuktilar
Sunday, April 26, 2020 | History

5 edition of Instabilities in Luminous Early Type Stars (Astrophysics and Space Science Library) found in the catalog.

Instabilities in Luminous Early Type Stars (Astrophysics and Space Science Library)

  • 141 Want to read
  • 2 Currently reading

Published by Springer .
Written in English

    Subjects:
  • Stars, interstellar matter,
  • Jager, C. de,
  • Astrophysics,
  • Science,
  • Wolf-Rayet stars,
  • Science/Mathematics,
  • Shell stars,
  • Astronomy - Star Guides,
  • Science / Astronomy,
  • Astronomy - General,
  • (Cornelis de),,
  • Congresses

  • Edition Notes

    ContributionsHenny J.G.L.M. Lamers (Editor), C. de Loore (Editor)
    The Physical Object
    FormatHardcover
    Number of Pages305
    ID Numbers
    Open LibraryOL9096707M
    ISBN 109027725225
    ISBN 109789027725226

    The Galactic O-Star Spectroscopic Survey (GOSSS). II. Bright Southern Stars Can the magnetic field in the Orion arm inhibit the growth of instabilities in the bow shock of Betelgeuse? A Rare Encounter with Very Massive Stars in NGC A1. Spectroscopic and physical parameters of Galactic O-type stars. II. Introduction This book is concerned with the physical processes related to the formation and evolution of galaxies. Simply put, a galaxy is a dynamically bound system that consists of many stars. A typical bright galaxy, such as our own Milky Way, contains a few times stars and has a. Introduction. This book presents a unified treatment of the chemistry of the elements. At present elements are known, though not all occur in nature: of the 92 elements from hydrogen to uranium all except technetium and promethium are found on earth and technetium has been detected in some stars.


Share this book
You might also like
technique of the revived Greek dance

technique of the revived Greek dance

Comparisons in art

Comparisons in art

Oversight hearing on traumatic brain injury (TBI)

Oversight hearing on traumatic brain injury (TBI)

Transformation in Metals

Transformation in Metals

William Robertson Smith

William Robertson Smith

Studies on diversion

Studies on diversion

Dickens and new historicism

Dickens and new historicism

In the cool shade of compassion

In the cool shade of compassion

The supermarketers

The supermarketers

A treatise on the law of contracts

A treatise on the law of contracts

Art of the October Revolution

Art of the October Revolution

Geology of the Squaw Lake - Sturgeon Lake area, district of Thunder Bay.

Geology of the Squaw Lake - Sturgeon Lake area, district of Thunder Bay.

part played by co-operative organisations in the international trade in wheat, dairy produce, and some other agricultural products

part played by co-operative organisations in the international trade in wheat, dairy produce, and some other agricultural products

House Committee on Foreign Affairs

House Committee on Foreign Affairs

Instabilities in Luminous Early Type Stars (Astrophysics and Space Science Library) Download PDF EPUB FB2

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, 21–24 April Editors: Lamers, Hermanus, de Loore, C.

(Eds.) Free Preview. 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, 21–24 April Title: Book-Review - Instabilities in Luminous Early Type Stars: Authors: Lamers, H.

M.; De Loore, C.; Garmany, C. Publication: Space Science Reviews, Vol. ADS Classic is now deprecated. It will be completely retired in October Please redirect your searches to the new ADS modern form or the classic info can be found on our blog.

Get this from a library. 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 [C de Jager; Henny J G L M Lamers; Camiel W H de Loore;].

adshelp[at] The ADS is operated by the Smithsonian Astrophysical Observatory under NASA Cooperative Agreement NNX16AC86A. Appenzeller I. () Theory of Vibrational Instabilities in Luminous Early Type Stars.

In: Lamers H.J.G.L.M., De Loore C.W.H. (eds) Instabilities in Luminous Early Type Stars. Astrophysics and Space Science Library (A Series of Books on the Recent Developments of Space Science and of General Geophysics and Astrophysics Published in Connection Cited by: 6. Get this from a library.

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 [Henny J G L M Lamers; Camiel W H Loore] -- On April 28 Cornelis de Jager reached the age of 65 years.

On April 30 he officially retired from the University of Utrecht. The winds of hot, luminous, massive stars are driven by line-scattering of stellar radiation, but such massive stars can also exhibit superwind episodes, either as Red Supergiants or Luminous Blue Author: Stan Owocki.

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.

Several decades of observations of the most massive and most luminous stars have revealed a complex upper HR Diagram, shaped by mass loss, and inhabited by a variety of evolved stars exhibiting the consequences of their mass loss histories. This introductory review presents a brief historical overview of the HR Diagram for massive stars, highlighting some of the primary discoveries and results Author: Roberta M.

Humphreys. A hypergiant (luminosity class 0 or Ia +) is a very rare kind of star that has an extremely high luminosity and mass loss by stellar term hypergiant is defined as luminosity class 0 (zero) in the MKK r, 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.

6 The early-type stars Introduction Main-sequence models Axial rotation along the upper main sequence Circulation, rotation, and diffusion Rotation of evolved stars Bibliographical notes 7 The late-type stars. The Atmospheres of Early-Type Stars Proceedings of a Workshop Organized Jointly by the UK SERC’s Collaborative Computational Project No.

7 and the Institut für Theoretische Physik und Sternwarte, University of Kiel Held at the University of Kiel, Germany, 18–20 September A nebula (Latin for 'cloud' or 'fog'; pl. nebulae, nebulæ or nebulas) is an interstellar cloud of dust, hydrogen, helium and other ionized ally, the term was used to describe any diffused astronomical object, including galaxies beyond the Milky Andromeda Galaxy, for instance, was once referred to as the Andromeda Nebula (and spiral galaxies in general as "spiral nebulae.

Variable stars are generally analysed using photometry, spectrophotometry and ements of their changes in brightness can be plotted to produce light regular variables, the period of variation and its amplitude can be very well established; for many variable stars, though, these quantities may vary slowly over time, or even from one period to the : Robert A.

Heinlein & Spider Robinson. originate from stellar envelopes or outer stellar atmospheres in early-type stars. A catalog of early-type emission-line stars from LAMOST DR2 has been published and a preliminary analysis is made on this sample (Hou et al., ).

Another generation mechanism for emission lines is stellar activities, often star flares due to magnetic behaviors. (a) Traditional hallmarks of luminous blue variables.

The diverse collection of objects known collectively as LBVs was first proposed by Conti [], and the standard interpretation of these stars and their role in evolution was established through the s and s (e.g. []).The central idea that emerged is that LBVs are massive single stars in a transitional phase between the main sequence Cited by: 7.

VARIABLE STAR TYPE DESIGNATIONS IN VSX By the VSX Team (Sebastián Otero, Christopher Watson and Patrick Wils) For an alphabetical list of variable star types used in VSX, click here. Based on the General Catalog of Variable Stars (GCVS) document of variable star type designations (Samus et al., ) with expansions, clarifications, corrections, and additions from the literature and surveys.

Structure and Evolution of the Universe Physics at the earliest moments of our universe, when it was unimaginably hot and dense, is intimately related to physics at the highest energies.

The universe then, a fraction of a second after the Big Bang, was a hot quantum soup of the fundamental particles being revealed in today's particle accelerators. A type of giant/supergiant star which pulsates regularly with a period in the range from about a day to about days.

The changes in radius, temperature, and hence luminosity, arise from instabilities in the envelopes of such evolved giant or supergiant stars.

Planetary nebulae present a fascinating range of shapes and morphologies. They are ideal laboratories for the study of different astrophysical processes: atomic physics, radiative transfer, stellar winds, shocks, wind-wind interaction, and the interaction between stellar winds and the interstellar medium.

In addition, planetary nebulae provide information about the late stages of stellar. Instabilities in Luminous Early Type Stars von - Englische Bücher zum Genre Physik & Astronomie günstig & portofrei bestellen im Online Shop von Ex Libris.

Type II Supernova (SNII) - Explosive death of a >4 M sun star. Type II supernovae (SNII) were recognized as a distinct type of supernova in the early s.

They are distinguished by H emission lines in their spectra, and light curve shapes significantly different than those of Type I supernovae. The Genesis tradition mentions only three classes of body in the solar system: the Sun, the Moon and the ‘stars’, i.e.

other luminous bodies, once referred to as “wandering stars”. Accordingly, creation theory predicts that the origin of the Earth’s moon will not yield to a satisfactory natural explanation. Deuterium is not made in stars (it can actually be destroyed in stars) but during the Big Bang.

Hence the observed abundance is a lower limit to that produced in the early stages of the Big Bang. The open Universe model predicts a production of one deuterium atom per 10 5 atoms, whilst a closed Universe should have one deuterium atom per 10 Only luminous early spectral type stars show such extreme environments, and Filliatre and Chaty () concluded that IGR J was an unusual HMXB hosting a sgB[e] with characteristic luminosity 10 6 L ⊙, mass 30 M ⊙, radius 20 R ⊙ and temperature T = K, located at a distance between 1 and 6 kpc (see also Chaty and Filliatre Cited by: High-Resolution Spectroscopy of Early-Type Halo Stars Together with N.C.

Hambly, W.R.J. Rolleston, F.P. Keenan, and P.L. Dufton (Queen's U. Belfast), Saffer analyzed high-resolution spectroscopic observations of early-type stars drawn from a complete sample of targets identified by low-resolution spectroscopy in the Palomar-Green Survey by. @article{ref:Abazajian_, author = {{Abazajian}, K.~N.

and others}, title = {{The Seventh Data Release of the Sloan Digital Sky Survey}}, journal. The cores of luminous B- and A-type (BA) supergiant stars are the seeds of later core-collapse supernovae.

Thus, constraining the near-core conditions in this class of stars can place tighter constraints on the size, mass, and chemical composition of supernova remnants.

Asteroseismology of these. Zodiacal clouds like the Sun's can be imaged by SIRTF around the nearest solar-type stars, while planetary debris disks like those found by IRAS can be studied around stars more distant than lkpc.

For the more prominent systems, SIRTF's images will show the orientation, structural features, and detailed morphology of the disks, including the. This is the first GMC catalog of an early-type galaxy. We find that the GMC population in NGC is gravitationally bound, with a virial parameter α ∼ 1.

The mass distribution, dN/dM ∝ M{sup −±}, is steeper than that for GMCs in the inner Milky Way, but comparable to that found in.

cascade of triaxial instabilities and leads to the formation of a quasi-star: a growing black hole, initially of typical stellar-mass, embedded in a hydrostatic giant-like envelope. Quasi-stars are the main object of study in this dissertation.

Their envelopes satisfy the equations of stellar structure so the Cambridge STARS code is modified toFile Size: 5MB. Massive stars easily rank as the most luminous in the cosmos — the brightest outshine the Sun by a million times.

And these are the only stars bright enough for us to see in distant galaxies. @article{ref:Humphreys_, author = {{Humphreys}, R.~M. and {Davidson}, K.}, title = {{The most luminous stars}}, journal = {Science}, keywords.

early twentieth century (e.g. Jeans, ), lies at the heart of modern theories of star and planet formation. Originally inferred from the infrared excesses of young stellar objects (e.g. Lada and Wilking, ), PP disks were directly imaged rst in the sub-mm (Sargent and Beckwith, ; Koerner et al., ), and then spectacularly in the op-File Size: 3MB.

Very massive stars occasionally expel material in colossal eruptions, driven by continuum radiation pressure rather than blast waves. Some of them rival supernovae in total radiative output, and the mass loss is crucial for subsequent evolution.

Some are supernova impostors, including SN precursor outbursts, while others are true SN events shrouded by material that was ejected earlier. The type of star in question are FU Orionis stars (FU Ori). FU Orionis is both a type of star, and also a specific star in the constellation Orion.

The type is named after the specific star, which. The growth of instabilities is controlled by magnetic diffusion which ultimately determines the equilibrium strength of the field." "For stars more massive than around 15M ⊙ the Kelvin–Helmholtz turbulence dominates over the magnetic turbulence and a stable field cannot be sustained by the dynamo." Differential rotations.

The best stars to try this on are the closest and brightest—Rigel, Betelgeuse (see Figure ), the red supergiant R Sculptoris, and both stars in the Spica binary system (see Table ).

Note that, even for these stars, the direct stellar evolution codes may be unable to converge to a solution, in which case they will simply break. A planetary nebula, abbreviated as PN or plural PNe, is a type of emission nebula consisting of an expanding, glowing shell of ionized gas ejected from red giant stars late in their lives.

The term "planetary nebula" is a misnomer because they are unrelated to planets or term originates from the planet-like round shape of these nebulae observed by astronomers through early.As recognised early on by Oort () and Baade (), our own Milky Way is composed of various populations of stars, each featuring different dynamics, chemical properties, and formation epochs.

Thus, from a stellar content viewpoint, galaxies can be broken .if faster: stars would be too luminous if slower: stars would not be luminous enough Age of the Universe if older: no solar-type stars in a stable burning phase in the right part of the galaxy if younger: solar-type stars in a stable burning phase would not yet have formed.