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Monday, May 18, 2020 | History

6 edition of Variable and Non-Spherical Stellar Winds in Luminous Hot Stars found in the catalog.

Variable and Non-Spherical Stellar Winds in Luminous Hot Stars

Proceedings of the Iau Colloquium No. 169 Held in Heidelberg, Germany, 15-19 June, 1998 (Lecture Notes in Physics)

  • 64 Want to read
  • 24 Currently reading

Published by Springer-Verlag Telos .
Written in English

    Subjects:
  • Astrophysics,
  • Stars, interstellar matter,
  • Theoretical & mathematical astronomy,
  • Early stars,
  • Stars,
  • Science,
  • Stellar winds,
  • Science/Mathematics,
  • Astronomy - Star Guides,
  • Astrophysics & Space Science,
  • Cosmology,
  • Congresses

  • Edition Notes

    ContributionsB. Wolf (Editor), O. Stahl (Editor), Alex W. Fullerton (Editor)
    The Physical Object
    FormatHardcover
    Number of Pages424
    ID Numbers
    Open LibraryOL9062931M
    ISBN 103540657029
    ISBN 109783540657026

    Luminous blue variable stars can undergo "giant outbursts" with dramatically increased mass loss and luminosity. Eta Carinae is the prototypical example, with P Cygni showing one or more similar outbursts – years ago, but dozens have now been catalogued in external galaxies. Many of these were initially classified as supernovae but re-examined because of unusual features. The term “Luminous Blue Variable” is unfortunate in three respects: Many unrelated luminous blue stars are also variable, LBV’s are often not very blue or not strongly variable, and it has caused extraneous objects to be included in lists of LBVs, often without observed outbursts [12,13]. Thus we should regard the trigram “LBV” as an.

    Mass loss by stellar winds. In addition to radiating energy into space, stars also lose mass. In hot stars, radiation pressure must be taken into account, so the expression for the pressure becomes. For example, for an Eta-Carinae-like luminous blue variable star, one might say. to model the remarkably high mass-loss rate of that star. NGC also known as the Fireworks Galaxy is a face-on intermediate spiral galaxy with a small bright nucleus, whose location in the sky straddles the boundary between the northern constellations of Cepheus and Cygnus. Its distance from Earth is about million light-years or megaparsecs, similar to the distance of M in the constellation Ursa Major.

    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. Supernova discoveries are reported to the International Astronomical Union's Central Bureau for Astronomical Telegrams, which sends out a circular with the name it assigns to that name is the marker SN followed by the year of discovery, suffixed with a one or two-letter designation. The first 26 supernovae of the year are designated with a capital letter from A to Z.


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Variable and Non-Spherical Stellar Winds in Luminous Hot Stars Download PDF EPUB FB2

Variable and Non-spherical Stellar Winds in Luminous Hot Stars Proceedings of the IAU Colloquium No. Held in Heidelberg, Germany, 15–19 June Editors: Wolf, Bernhard, Stahl, Otmar, Fullerton, Alex W.

(Eds.) Free Preview. Get this from a library. Variable and non-spherical stellar winds in luminous hot stars: proceedings of the IAU Colloquium no. held in Heidelberg, Germany, 15. Variable and Non-spherical Stellar Winds in Luminous Hot Stars: Proceedings of the IAU Colloquium No.

Held in Heidelberg, Germany, June in Physics) (Lecture Notes in Physics ()) Softcover reprint of the original 1st ed.

EditionFormat: Paperback. Variable and non-spherical stellar winds in luminous hot stars proceedings of the IAU Colloquium no. held in Heidelberg, Germany, June by IAU Colloquium (th Heidelberg, G Published by Springer in Berlin, New : Langer N. () The evolution of non-spherical and non-stationary winds of massive stars.

In: Wolf B., Stahl O., Fullerton A.W. (eds) Variable and Non-spherical Stellar Winds in Luminous Hot Stars. Lecture Notes in Physics, vol Author: Norbert Langer. Non-spherical radiation-driven wind models. Variable and Non-spherical Stellar Winds in Luminous Hot Stars, pp Nebulae around luminous blue variable (LBV) stars are often.

Disk winds of B[e] supergiants. Variable and Non-spherical Stellar Winds in Luminous Hot Stars, pp This is the bistability of stellar winds for stars with Teff ≃ 21, K. Luminous blue variable stars can undergo "giant outbursts" with dramatically increased mass loss and luminosity.

η Carinae is the prototypical example, with P Cygni showing one or more similar outbursts – years ago, but dozens have now been catalogued in external galaxies. Many of these were initially classified as supernovae but re-examined because of unusual features.

Variable and Non-spherical Stellar Winds in Luminous Hot Stars av Bernhard Wolf, Otmar Stahl, Alex W Fullerton Inbunden, Engelska, Precise Stellar Radial Velocities Victoria, Canada, JuneEds.

J.B. Hearnshaw & C.D. Scarfe ASP Conference Series ISBN 1 Jan Electronic version: IAUC Variable and Non-Spherical Stellar Winds in Luminous Hot Stars Lecture notes in physics Vol Heidelberg, Germany, JuneEds.

Wolf, O. Stahl & A. Discover Book Depository's huge selection of Alexander Fullerton books online. Free delivery worldwide on over 20 million titles. We use cookies to give you the best possible experience.

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They are supergiant stars of spectral types B or A. Variations in brightness on the order of magnitudes are associated with the pulsations, which often seem irregular, due to beating of multiple pulsation periods. @article{osti_, title = {Luminous and Variable Stars in M31 and M IV. Luminous Blue Variables, Candidate LBVs, B[e] Supergiants, and the Warm Hypergiants: How to Tell Them Apart}, author = {Humphreys, Roberta M.

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