Foundations of Astronomy (MindTap Course List)
14th Edition
ISBN: 9781337399920
Author: Michael A. Seeds, Dana Backman
Publisher: Cengage Learning
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Question
Chapter 7, Problem 12P
To determine
The change in wavelength of the Balmer-beta line.
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An astronomer might observe in the Milky Way Galaxy have radial velocities as high as 500 km/s ( 5.00 × 102 km/s). What change in wavelength would this cause in the Balmer-beta line?
Why don’t we see hydrogen Balmer lines in the spectra of stars with temperatures of 45,000 K?
a.
There is no hydrogen in stars this hot.
b.
The stars are hot enough that most of the hydrogen is ionized and the atoms cannot absorb energy.
c.
These stars are so cool that nearly all of the electrons in the hydrogen atom are in the ground state.
d.
Stars of this temperature are too cool to produce an absorption spectrum.
e.
Stars of this temperature are too hot to produce an absorption spectrum.
One cubic meter of atomic hydrogen at 0°C at atmospheric pressure contains approximately 2.70 × 10 25 atoms. The first excited state of the hydrogen atom has an energy of 10.2 eV above that of the lowest state, called the ground slate. Use the Boltzmann factor to find the number of atoms in the first excited slate (a) at 0 ºC and at (b) (1.00 × 10 4 )°C.
Chapter 7 Solutions
Foundations of Astronomy (MindTap Course List)
Ch. 7 - Prob. 1RQCh. 7 - Prob. 2RQCh. 7 - Prob. 3RQCh. 7 - Prob. 4RQCh. 7 - Prob. 5RQCh. 7 - Prob. 6RQCh. 7 - Prob. 7RQCh. 7 - Prob. 8RQCh. 7 - Prob. 9RQCh. 7 - Prob. 10RQ
Ch. 7 - Prob. 11RQCh. 7 - Prob. 12RQCh. 7 - Prob. 13RQCh. 7 - Prob. 14RQCh. 7 - Prob. 15RQCh. 7 - Prob. 16RQCh. 7 - How is heat different from temperature?Ch. 7 - Prob. 18RQCh. 7 - Prob. 19RQCh. 7 - Prob. 20RQCh. 7 - Prob. 21RQCh. 7 - Prob. 22RQCh. 7 - Could an object be orbiting another object and we...Ch. 7 - Prob. 24RQCh. 7 - How Do We Know? How is the macroscopic world you...Ch. 7 - Prob. 1PCh. 7 - Answer these questions for celestial bodies at...Ch. 7 - Prob. 3PCh. 7 - Prob. 4PCh. 7 - Prob. 5PCh. 7 - Prob. 6PCh. 7 - Prob. 7PCh. 7 - Prob. 8PCh. 7 - Prob. 9PCh. 7 - Prob. 10PCh. 7 - Prob. 11PCh. 7 - Prob. 12PCh. 7 - Prob. 1SOPCh. 7 - Prob. 2SOPCh. 7 - Prob. 1LTLCh. 7 - Prob. 2LTLCh. 7 - Prob. 3LTLCh. 7 - Prob. 4LTLCh. 7 - Prob. 5LTLCh. 7 - Prob. 6LTLCh. 7 - Prob. 7LTL
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- Estimate the average thermal energy of a helium atom at (i) room temperature (27 °C), (ii) the temperature on the surface of the Sun (6000 K), (iii) the temperature of 10 million kelvin (the typical core temperature in the case of a star).arrow_forwardHydrogen accounts for about 75% by mass of the matter at the surfaces of most stars. However, the absorption lines of hydrogen are strongest (of highest intensity) in the spectra of stars with a surface temperature of about 9000 K. They are weaker in the sun spectrum and are essentially nonexistent in very hot (temperatures above 25,000 K) or rather cool (temperatures below 3500 K) stars. Speculate as to why surface temperature affects the hydrogen absorption lines that we observe.arrow_forwardThe temperature of the sun is approximately 5800 K and the temperature of the star Sirius A, the larger star of the Sirius via art, is approximately 10,000 K. The luminosity of Sirius A is about 33 times than Sun. The radiation law gives L=4(3.14) R^2 a T^4 By taking the ratio of the luminosities of Sirius A to the Sun, the relative values of luminosity and temperature can be used to determine the relative value of radius. What is the multiples of the Sun’s radius?arrow_forward
- In class I derived the ordinary nuclear density to be about 0.138 u/fm3. A neutron star is a collapsed star that contains neutrons in a highly compactified state, so its average density is higher. Assume a neutron star is spherical and has an average density which is about twice the ordinary nuclear density. If it is 50% heavier than the Sun, what would be its radius? (Given: mass of sun = 2*1030 kg, 1 u = 1.66*10-27 kg.) A) 14.6 km B) 11.6 km C) 10.1 km D) none of these.arrow_forwardIn hydrogen, the transition from level 2 to level 1 has a rest wavelength of 121.6 nm. Find the speed for a star in which this line appears at wavelength 120.5 mm. What about at 122.4 nm? Express your answer to three significant figures and include the appropriate units.arrow_forwardOur sun is a standard sequence yellow dwarf star with a temperature of about 6000 K and a radius of about 7 x 10^8 m, emitting about 3.8 x 10^26 W. There are yellow giant stars with the same blackbody color (temperature) but with a radius 10 times larger than our sun (7 x 10^9 m). Estimate the power (emitted radiation) from one of these yellow giant stars. (Hint: how much larger is the surface area of the yellow giant star, and pay careful attention to the power of 10 below.)arrow_forward
- Please answer this question asap.. (Fbd should be included)arrow_forwardAssuming that the Sun is a blackbody with a temperature of 6,000 K, at what wavelength does it radiate the most energy? [4.8 x 10‐7 m]arrow_forwardAt what rate does the Sun emit photons? For simplicity, assume that the Sun’s entire emission at the rate of 3.9 * 10^26 W is at the single wavelength of 550 nm.arrow_forward
- An astronomer measures the light from two objects, A and B, and she finds that they are both black bodies. If the peak in the observed emission of A is at wavelength 2000nm and the peak of B is at 400nm, then what is the ratio of their photospheric temperatures?arrow_forwardWhy don’t we see hydrogen Balmer lines in the spectra of stars with temperatures of 3,200 K? a. There is no hydrogen in stars this cool. b. The stars are hot enough that most of the hydrogen is ionized and the atoms cannot absorb energy. c. These stars are so cool that nearly all of the hydrogen atoms are in the ground state. d. Stars of this temperature are too cool to produce an absorption spectrum. e. Stars of this temperature are too hot to produce an absorption spectrum.arrow_forward
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