Astronomy
1st Edition
ISBN: 9781938168284
Author: Andrew Fraknoi; David Morrison; Sidney C. Wolff
Publisher: OpenStax
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Textbook Question
Chapter 24, Problem 13E
Why would we not expect to detect X-rays from a disk of matter about an ordinary star?
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Chapter 24 Solutions
Astronomy
Ch. 24 - How does the equivalence principle lead us to...Ch. 24 - If general relativity offers the best description...Ch. 24 - Einstein’s general theory of relativity made or...Ch. 24 - If a black hole itself emits no radiation, what...Ch. 24 - What characteristics must a binary star have to be...Ch. 24 - A student becomes so excited by the whole idea of...Ch. 24 - What is an event horizon? Does our Sun have an...Ch. 24 - What is a gravitational wave and why was it so...Ch. 24 - What are some strong sources of gravitational...Ch. 24 - Suppose the amount of mass in a black hole...
Ch. 24 - Imagine that you have built a large room around...Ch. 24 - A monkey hanging from a tree branch sees a hunter...Ch. 24 - Why would we not expect to detect X-rays from a...Ch. 24 - Look elsewhere in this book for necessary data,...Ch. 24 - Which is likely to be more common in our Galaxy:...Ch. 24 - If the Sun could suddenly collapse to a black...Ch. 24 - Suppose the people in Figure 24.4 are in an...Ch. 24 - You arrange to meet a friend at 5:00 p.m. on...Ch. 24 - You are standing on a scale in an elevator when...Ch. 24 - Look up G, c, and the mass of the Sun in Appendix...Ch. 24 - Suppose you wanted to know the size of black holes...Ch. 24 - Use the result from Exercise 24.21 to calculate...Ch. 24 - Since the force of gravity a significant distance...
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- Would you expect to be able to detect an H II region in X-ray emission? Why or why not? (Hint: You might apply Wien’s law)arrow_forwardWhat is the maximum energy, maximum frequency and minimum wavelength associated with an 6MV beam?arrow_forwardGo to Question 8 60 Msun I luminosity (solar units) 106 105 104 103 102 10 0.1 10-2 10-3 10-4 10-5 30 Msun 10 Solar Radii Lifetime 10 yrs 1 Solar Radius 0.1 Solar Radius 10-2 Solar Radius 10-3 Solar Radius 30,000 increasing temperature 102 Solar Radi B Centauri Spica 10 Msun Bellatrix MAIN Sirius B Lifetime 108 yrs B Rigel Deneb 6 Msun Achernar SEQUENCE Lifetime 10⁹ yrs WHITE SUPERGIANTS Msun Vega DWARFS Procyon B 103 Solar Radi Sirius Lifetime 1010 yrs A 10,000 Altair Canopus Procyon Sun Arcturus Polaris Lifetime 10¹1 yrs T Ceti 6,000 surface temperature (Kelvin) GIANTS x Centauri A Pollux x Centauri B Eridani F G K Aldebaran Barnard's Star Betelgeuse 61 Cygni A 61 Cygni B Lacaille 9352 0.3 Msun Antares M (It may help you to know that 1 Lsun is 3.8 x 1026 Watts. Use 3.1415 for Pi.) Wolf 359 Proxima Centauri DX Cancri Gliese 725 A Gliese 725 B 0.1 Msun Ross 128 3,000 decreasing temperature The physics of thermally radiating gases relates the luminosity (L), temperature (T) and radius…arrow_forward
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- The luminosity density of an accretion disk, which extends from riso to rmax, is given by the blackbody Planck's formula Ιναν Tmax 12 Sam r ehv/kBT(r) BT(r) – 1 dr, rlso where is the radiation frequency, T (r) is the temperature in the disc at radius r, h is the Planck's constant and kB is the Boltzmann's constant. Show that, in the limit hv <1, L, is proportional to 12. KBTarrow_forwardlambdamax = 600nm (5000K/T) L ∝ R2 T 4 1. What is the peak wavelength of an O star of temperature 50,000 K? What range of the spectrum is this?arrow_forward3 E As a star becomes a giant, its outer layers are expanding and the pressure consequently drops in the outer atmosphere. Where does the energy for expanding these layers come from? O from a magnetic dynamo effect in the star's outer layers, caused by a much stronger magnetic field inside the star O from the fusion of hydrogen into helium in a shell around the core O from an explosion in the core O from the fusion of helium into carbon in the core. O from the long-term fusion of hydrogen into helium in the core C F3 44 $ R 49 F F4 ww V DII FS % Q Search 5 T G * A 6 B F6 H F7 & 7 U N PrtScn F8 8 Home 3 9 K End F10 PgUp FI O Larrow_forward
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