Astrophysics for Physicists

Astrophysics for Physicists

Arnab Rai Choudhuri

Language: English

Pages: 490

ISBN: 0521815533

Format: PDF / Kindle (mobi) / ePub

Designed for teaching astrophysics to physics students at advanced undergraduate or beginning graduate level, this textbook also provides an overview of astrophysics for astrophysics graduate students, before they delve into more specialized volumes. Assuming background knowledge at the level of a physics major, the textbook develops astrophysics from the basics without requiring any previous study in astronomy or astrophysics. Physical concepts, mathematical derivations and observational data are combined in a balanced way to provide a unified treatment. Topics such as general relativity and plasma physics, which are not usually covered in physics courses but used extensively in astrophysics, are developed from first principles. While the emphasis is on developing the fundamentals thoroughly, recent important discoveries are highlighted at every stage.

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And they can be taken as typical representative samples in statistical studies of stars. 3.5.2 Important features of observational data Mass–luminosity relation If a star is both nearby and in a binary, then both its luminosity and mass can be determined. Plotting luminosities and masses of such stars, we get Figure 3.4. Our simple theoretical considerations led to (3.37), implying that luminosity should go as the cube of mass. The fact that a straight line fits the data reasonably well implies.

Data presented by Popper (1980). and the absolute visual magnitude MV , which are directly measured (rather than Teff and L which are inferred from these measurements). Stars lying on the right side of the diagram are reddish in colour, whereas stars lying on the left side are bluish in colour. HR diagrams with MV plotted against B − V are also called colour–magnitude diagrams. Most stars seem to lie on a diagonal strip in Figure 3.5 from the upper left corner to the lower right corner. This.

Our job is now to find the energy generation function ε for the whole chain of reactions. How can this be done? We note that the first reaction in (4.20) is mediated by the weak interaction (the emission of a neutrino is usually the signature of a reaction being mediated by the weak interaction) and is a slow reaction with a small cross-section. Even though some of the other reactions may be faster, they cannot proceed without the 2 H nuclei which are produced in 4.3 Nuclear reactions in.

The standing modes. Similarly, the eigenmodes of the Sun are caused by sound waves (we would call them ‘sound waves’ even though their frequencies are usually outside the audible range) which interfere constructively after passing through and around the Sun. Since different modes go up to different depths in the interior of the Sun, the analysis of many modes together 4.4 Detailed stellar models 105 Fig. 4.7 The difference between the density inferred from helioseismology and the density.

Considerations by assuming 153 154 Our Galaxy and its interstellar matter that the space around us is free of any absorbing material. Suppose we are surrounded by identical stars of absolute magnitude M distributed in space with a uniform density. We want to find the number N (m) of stars which appear brighter than apparent magnitude m. It should be clear from (1.8) that a star would have apparent magnitude m if it is located at a distance d = (10)1+0.2(m−M) pc. (6.1) All stars within a.

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