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  • Open Daily: 10am - 10pm
    Alley-side Pickup: 10am - 7pm

    3038 Hennepin Ave Minneapolis, MN
    612-822-4611

Open Daily: 10am - 10pm | Alley-side Pickup: 10am - 7pm
3038 Hennepin Ave Minneapolis, MN
612-822-4611
Advances in Helio- And Asteroseismology: Proceedings of the 123th Symposium of the International Astronomical Union, Held in Aarhus, Denmark, July 7-1

Advances in Helio- And Asteroseismology: Proceedings of the 123th Symposium of the International Astronomical Union, Held in Aarhus, Denmark, July 7-1

Christensen-Dalsgaard, Jørgen
Frandsen, Søren

Paperback

Series: International Astronomical Union Symposia, Book 123

Astronomy & SpaceGeologyPhysics

ISBN10: 9027726159
ISBN13: 9789027726155
Publisher: Springer Nature
Published: Nov 30 1987
Pages: 628
Weight: 2.38
Height: 1.27 Width: 7.00 Depth: 10.00
Language: English
Helio- and asteroseismology study the interior of the Sun and other stars, by means of observations of oscillations on their surfaces. The last 10 years in the study of the solar interior, to a has witnessed a very rapid evolution point where we can now contemplate investigating the physical state of matter, or the details of rotation and other large-scale motion, in the Sun. The stellar studies are in some respects at the point of the solar studies 10 years ago, but appear poised to take off. Thus the time was deemed ripe for lAO Symposium No 123, to assess the present status of this work, and plan for its future development. Apart from the seismic data, few observations are available to provide information about stellar interiors. Detailed studies, by spectral analysis, can be made of stellar surface properties, including atmospheric temperature and chemical composition. However, the stellar radiative spectrum is almost entirely fixed by the mass, luminosity, radius and surface rotation of the star, and contains essentially no other information about the interior. An important test of stellar evolution theory is provided by observations of stel- lar clusters, whose members can reasonably be assumed to have the same age and chemical composition. The location of such stars in a HR diagram, where luminosity is plotted against the effective temperature, can roughly be understood in terms of stellar evolution calculations.

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