EBK PHYSICS FOR SCIENTISTS & ENGINEERS
5th Edition
ISBN: 9780134296074
Author: GIANCOLI
Publisher: VST
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Chapter 44, Problem 18P
To determine
The ratio of diameter.
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The figure above shows the light-curve obtained from continuous monitoring of the flux received from a star. Assuming that the dips arise because a planet orbiting the star passes between it and the observer once per orbit, estimate the orbital period (in days), the orbital semi-major axis (in Astronomical Units), and the physical radius of the planet (in units of the Earth’s radius). The star has a mass of 1.47 M⊙ and a radius of 1.84 R⊙.
(Astronomy)
PSR1913+16 Problem III.
As the shape of the graph shown is not skewed, the orbit can be assumed circular. Also assume the system is viewed edge-on (that is, the orbital system is not inclined to the observer). Using these assumptions, the maximum radial velocities, and the orbital period T = 7.75 hours, find the orbital radii of the stars from the center of mass. (Hints: The figures below may be helpful. Use v = 2πr/P, where v is velocity, P is period, and r is radius. Note: redshifts have positive radial velocities values in the upper figure, whereas blueshifts have negative radial velocity values.)
Problem 3:
Two stars, M and N, from the same galaxy (at the same distance from
earth) are observed to have the same luminosity (that is, they emit the
same amount of energy per unit time). Star M is red, its spectrum peaks
2.4 × 1015s-1 while star N is white, its spectrum peaks at w =
3.6 x 1015s-1. Assuming that both stars radiate as black body, what is the
at w =
ratio of their radii?
Chapter 44 Solutions
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- a) b) Electron degeneracy pressure in a white dwarf star, of uniform density p, in the nonrela- tivistic case is given by Pwd ħ² 3memp 25/305/3 where symbols have their usual meanings. Using the result that the central pressure in a star, of radius R and uniform density, under gravitational attraction is given by Pc = Gp² R², derive an expression for the radius Rwd of a white dwarf in terms of its mass M, in the case of nonrelativistic electron degeneracy. Using your result, briefly discuss the limitations of your expression for the radius, in the context of white dwarfs of increasing mass. Consider a white dwarf, mass M, radius Rwd and temperature T, consisting entirely of helium nuclei and electrons. Show that the internal thermal energy of the ions alone is given by 3 M Eth= -kT, 8 mp where mp is the proton mass. White dwarfs initially have a very high temperature when they form, and then cool by radi- ation. Derive a differential equation for the rate of change of the temperature…arrow_forward(c) Consider a star of radius r and temperature T. By modelling the star as a spherical black body, show that at a distance d away from the star the flux radiation is F= rT* ()". where a is the Stefan-Boltzmann constant.arrow_forward1. a) Using the virial mass for a spherical distribution of stars of radius R and mass M, find how R depends on o and Lassuming some constant M/L. b) Now, assume that all ellipticals have some constant surface brightness to show that L < 04arrow_forward
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