UNIVERSE LL W/SAPLINGPLUS MULTI SEMESTER
11th Edition
ISBN: 9781319278670
Author: Freedman
Publisher: MAC HIGHER
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Chapter 24, Problem 18Q
To determine
The reason for broad spectral lines in some AGN as suggested by the unified model.
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Chapter 24 Solutions
UNIVERSE LL W/SAPLINGPLUS MULTI SEMESTER
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- H II regions can exist only if there is a nearby star hot enough to ionize hydrogen. Hydrogen is ionized only by radiation with wavelengths shorter than 91.2 nm. What is the temperature of a star that emits its maximum energy at 91.2 nm? (Use Wien’s law from Radiation and Spectra.) Based on this result, what are the spectral types of those stars likely to provide enough energy to produce H II regions?arrow_forwardWhy is Hubble’s law considered one of the most important discoveries in the history of astronomy?arrow_forwardWhy would we not expect to detect X-rays from a disk of matter about an ordinary star?arrow_forward
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- 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 = ? pcarrow_forwardWhat is the ratio of the percent of metals in extreme Population I stars (3%) to that in extreme Population II stars (0.05%)? NpopI NpopII =arrow_forwardA star with mass m, period Ti = 30 days, and radius ri = 1E4 km collapses into a neutron star (Links to an external site.) with a radius of rf = 3 km. Our goal will be to determine the period Tf of the neutron star. Useful formulae: Li=Lf; L=Iω; ω=2πf=2π/T; Isphere=2/5mr^2.arrow_forward
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