Download Die Entstehung von Sternen durch Kondensation diffuser by G. R. Burbidge, F. D. Kahn, R. Ebert, S. v. Hoerner, St. PDF

By G. R. Burbidge, F. D. Kahn, R. Ebert, S. v. Hoerner, St. Temesváry (auth.)

Show description

Read or Download Die Entstehung von Sternen durch Kondensation diffuser Materie: 3 Preisschriften PDF

Similar german_5 books

Mehrdimensionale lineare Systeme: Fourier-Transformation und δ-Funktionen

Das Buch gibt einen Überblick über die mathematischen Methoden der mehrdimensionalen Systemtheorie. Ausgehend von der Faltungsoperation, dem Delta-Impuls und der Fourier-Transformation werden Gemeinsamkeiten und Unterschiede beim Übergang von einer auf mehrere Dimensionen aufgezeigt. Auf die Vielfalt der Delta-Funktionen und Abtastschemata im Mehrdimensionalen wird besonders ausführlich eingegangen.

Digitale Schnittstellen und Bussysteme: Einführung für das technische Studium

BuchhandelstextDie Praxis der Automatisierungstechnik verlangt von allen Beteiligten ein Grundwissen ? ber die verwendete Technologie. Hierzu z? hlen in besonderem Ma? e auch Kenntnisse ? ber die verwendeten Einrichtungen zur Datenkommunikation, wie digitale Schnittstellen oder Bussysteme. Mit diesem Buch wird eine einfache Darstellung zur ersten Einf?

Additional resources for Die Entstehung von Sternen durch Kondensation diffuser Materie: 3 Preisschriften

Example text

Stellar models with inhomogeneities in chemical composition 41 Following the work of SCHOENBERG and CHANDRASEKHAR, who did not take into account possible degeneracy in their models with isothermal cores, GAMOW and KELLER (83) considered isothermal cores with partial degeneracy and concluded that under certain conditions such models could give radii large enough to fit the red giants. The result was contested by HARRISON who computed a number of partially degenerate models that did not have large radii.

22 is not shown on this diagram, but it lay very far to the right of the other computed points, a result in agreement with the earlier work of SANDAGE and SCHWARZSCHILD (86). 19 to the approximations that have been made in this region. For example, since the star starts off on the pp-chain, the material is not sharply divided in composition at the core boundary; this does not occur until the CN-cycle dominates. Also, they have divided the outer envelope into two zones, the outer one in which the Kramers opacity alone is operating, and an inner one in which the electron scattering alone is at work.

Consequently this mode of evolution is of no practical significance. ({3) Rotational mixing. In the envelope of a non-rotating star in which radiative energy transport prevails, mixing is negligibly small since the diffusion effects are unimportant over timescales ~ 1010 years (69). However, in a rotating star currents will be set up in planes through the axis of rotation, the degree of mixing depending on the equatorial velocity. Investigations by SWEET and OPIK (70), (71), have shown that the estimate of the amount of mixing by EDDINGTON (72) was far too large.

Download PDF sample

Rated 4.42 of 5 – based on 14 votes