Download Astrophysics for Physicists by Arnab Rai Choudhuri PDF

By Arnab Rai Choudhuri

ISBN-10: 0521815533

ISBN-13: 9780521815536

Designed for educating astrophysics to physics scholars at complicated undergraduate or starting graduate point, this textbook additionally offers an summary of astrophysics for astrophysics graduate scholars, ahead of they delve into extra really good volumes. Assuming history wisdom on the point of a physics significant, the textbook develops astrophysics from the fundamentals with out requiring any past learn in astronomy or astrophysics. actual thoughts, mathematical derivations and observational info are mixed in a balanced solution to offer a unified remedy. subject matters resembling normal relativity and plasma physics, which aren't frequently lined in physics classes yet used largely in astrophysics, are constructed from first ideas. whereas the emphasis is on constructing the basics completely, contemporary very important discoveries are highlighted at each degree.

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For example, radiation flux is simply the total energy of radiation coming from all directions at a point per unit area per unit time. 2) by dA dt and integrate over all solid angles. 3) Fν dν. 2). This energy passes through area dA in time dt in the direction n. radiation traverses a distance c dt in time dt, we expect this radiation dEν to fill ˆ The volume up a cylinder with base dA and axis of length c dt in the direction n. 2). To get the total energy density of radiation at a point associated with frequency ν, we have to integrate over radiation coming from different directions so that Uν = Iν d .

11) should be negative and proportional to Iν . 12) where αν is the absorption coefficient. This is the celebrated radiative transfer equation and provides the basis for our understanding of interaction between radiation and matter. In the early years of spectral research, many astronomers held the view that the Sun was surrounded by a cool layer of gas which only absorbed radiation at certain frequencies to produce the dark lines. Schuster (1905) recognized the importance of treating emission and absorption simultaneously by the same layer of gas.

Why is the radiation from a star not exactly blackbody radiation? Why do we see absorption lines? 23) by assuming the source to have constant properties. This is certainly not true for a star. As we go down from the star’s surface, temperature keeps increasing. 23) should be only approximately true. It is the temperature gradient near the star’s surface which gives rise to the absorption lines. 3. 25) that the source function should be equal to the blackbody function Bν (T ). In a realistic situation, we rarely have strict thermodynamic equilibrium.

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