Universe: Stars And Galaxies
Universe: Stars And Galaxies
6th Edition
ISBN: 9781319115098
Author: Roger Freedman, Robert Geller, William J. Kaufmann
Publisher: W. H. Freeman
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Chapter 24, Problem 18Q
To determine

The reason for some AGN to have broad spectral lines while some do not.

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The difference in absolute magnitude between two objects is related to their fluxes by the flux-magnitude relation: FA / FB = 2.51(MB - MA)  A distant galaxy contains a supernova with an absolute magnitude of -19.  If this supernova were placed next to our Sun (M = +4.8) and you observed both of them from the same distance, how much more flux would the supernova emit than the Sun? Fsupernova / FSun = ?
1) There is a one earth mass planet orbiting an M5 star of 0.2 Mo and luminosity 1x10-2 Lo- A) How close does the planet need to be to the star in order to receive the same amount of energy as the Earth receives from the sun? B) What is the orbital period of the planet at this distance? C) What is the magnitude of the radial velocity perturbation of the star? D) If the system is edge on to us, would we be likely to detect this planet using the radial velocity method?
A planetary nebula expanded in radius 0.3 arc seconds in 30 years.  Doppler measurements show the nebula is expanding at a rate of 35 km/s.  How far away is the nebula in parsecs? First, determine what distance the nebular expanded in parsecs during the time mentioned.  Δd = vpc/sTs So we first need to convert the rate into pc/s and the time into seconds: vpc/s = vkm/s (1 pc / 3.09 x 1013km) vpc/s = ? Ts = (Tyr)(365 days/yr)(24 hrs/day)(3600 s/hr) Ts = ? s Δd= vpc/sTs Therefore, Δd = ? pc
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