Universe
11th Edition
ISBN: 9781319039448
Author: Robert Geller, Roger Freedman, William J. Kaufmann
Publisher: W. H. Freeman
expand_more
expand_more
format_list_bulleted
Videos
Question
Chapter 7, Problem 15Q
(a)
To determine
The escape speed from the surface of the Sun if the mass of the Sun is
(b)
To determine
The reason for very less escape of hydrogen gas from the Sun’s atmosphere if the mass of the Sun is
Expert Solution & Answer
Want to see the full answer?
Check out a sample textbook solution
Students have asked these similar questions
If Titan could be moved out to the orbit of Neptune would its atmosphere freeze into solid nitrogen? The formula to estimate the blackbody radiation temperature in Kelvin is:
where α is the albedo at 0.3, L the luminosity is 1.5 Watts/meter2, σ , the Stefan Boltzmann constant is 5.67 X10-8 W/m2/K. What would be the temperature and would the atmosphere freeze out if the freezing point of N2 gas 63 K?
answer choices
63 K, maybe
75 K, no
46 K, yes
103 K, no
Jupiter radiates more energy than it
receives from the Sun by 8.7 x10-10 LO.
Jupiter's radius
is 7.1 x109 cm and its mass is 1.9 x1030 g.
Compute its dynamical and thermal
timescales.
(b) Can we assume that Jupiter is in
hydrostatic equilibrium?
(c) Could gravitational contraction have
powered Jupiter's luminosity for its entire
4.5 Gyr lifetime?
(d) Use conservation of energy to estimate
the rate at which Jupiter's radius is
shrinking to power
this radiation. You may ignore the factor of
order unity that arises from Jupiter's
unknown density
distribution.
K
What is the wavelength (in nm) of the most intense radiation emitted from the surface of Mercury at high noon? (Hint: Use Wien's law, Amax
= 2.90 x 10° m: K
%3D
T (in K)
nm
In which band of the electromagnetic spectrum is that wavelength? (Hint: Examine the following figure.)
Visible light
Short wavelengths
Long wavelengths
4 x 107 5x 107 6x 107 7x 10meters
(400 nm) (500 nm) (600 nm) /(700 nm)
Wavelength (meters)
10 12
10 10
10
104
102
1
102
104
Gamma-
ray
Ultra-
violet
Micro-
Radio
X-ray
Infrared
wave
UHF VHF FM
AM
a
Opaque
Visual
window
Radio
window
Transparent
Short
Wavelength
Long
b
O gamma-ray
O X-ray
O ultraviolet
O visual
O infrared
O microwave
O radio
оооо о оо
Opacity of
Earth's atmosphere
Chapter 7 Solutions
Universe
Ch. 7 - Prob. 1CCCh. 7 - Prob. 2CCCh. 7 - Prob. 3CCCh. 7 - Prob. 4CCCh. 7 - Prob. 5CCCh. 7 - Prob. 6CCCh. 7 - Prob. 7CCCh. 7 - Prob. 8CCCh. 7 - Prob. 9CCCh. 7 - Prob. 10CC
Ch. 7 - Prob. 11CCCh. 7 - Prob. 12CCCh. 7 - Prob. 13CCCh. 7 - Prob. 1CLCCh. 7 - Prob. 2CLCCh. 7 - Prob. 3CLCCh. 7 - Prob. 4CLCCh. 7 - Prob. 1QCh. 7 - Prob. 2QCh. 7 - Prob. 3QCh. 7 - Prob. 4QCh. 7 - Prob. 5QCh. 7 - Prob. 6QCh. 7 - Prob. 7QCh. 7 - Prob. 8QCh. 7 - Prob. 9QCh. 7 - Prob. 10QCh. 7 - Prob. 11QCh. 7 - Prob. 12QCh. 7 - Prob. 13QCh. 7 - Prob. 14QCh. 7 - Prob. 15QCh. 7 - Prob. 16QCh. 7 - Prob. 17QCh. 7 - Prob. 18QCh. 7 - Prob. 19QCh. 7 - Prob. 20QCh. 7 - Prob. 21QCh. 7 - Prob. 22QCh. 7 - Prob. 23QCh. 7 - Prob. 24QCh. 7 - Prob. 25QCh. 7 - Prob. 26QCh. 7 - Prob. 27QCh. 7 - Prob. 28QCh. 7 - Prob. 29QCh. 7 - Prob. 30QCh. 7 - Prob. 31QCh. 7 - Prob. 32QCh. 7 - Prob. 33QCh. 7 - Prob. 34QCh. 7 - Prob. 35QCh. 7 - Prob. 36QCh. 7 - Prob. 37QCh. 7 - Prob. 38QCh. 7 - Prob. 39QCh. 7 - Prob. 40QCh. 7 - Prob. 41Q
Knowledge Booster
Learn more about
Need a deep-dive on the concept behind this application? Look no further. Learn more about this topic, physics and related others by exploring similar questions and additional content below.Similar questions
- The gravitational collapse time for the Sun is a constraint on the timescale for the formation of the Solar System: Using the mass of the Sun and a 6.67 X10-11 in S.I. units (m, kg, sec) as the value for G, calculate the gravitational collapse time in millions of years for the mass of the Sun in a nebula with radius 4 light years. Recall that: tgravity = square root (R^3/ GM)arrow_forwardSaturn emits radiation at a rate of 1.98 x 1017 W and absorbs sunlight at a rate of 1.11 x 1017 W. a) Assuming that the radiation excess comes exclusively from Saturn's gravitational potential energy, at what rate dR/dt is Saturn shrinking? b) How long would it take for Saturn's radius to decrease by 1%?arrow_forwardThe gravitational collapse time for the Sun is a constraint on the timescale for the formation of the Solar System: Using the mass of the Sun and a 6.67 X10-11 in S.I. units (m, kg, sec) as the value for G, calculate the gravitational collapse time in millions of years for the mass of the Sun in a nebula with radius 4 light years. Recall that: tgravity=R3GM−−−√tgravity=R3GM Group of answer choices 20 28 10 80arrow_forward
- Consider the attached light curve for a transiting planet observed by the Kepler mission. If the host star is identical to the sun, what is the radius of this planet? Give your answer in terms of the radius of Jupiter. Brightness of Star Residual Flux 0.99 0.98 0.97 0.006 0.002 0.000 -8-881 -0.06 -0.04 -0.02 0.00 Time (days) → 0.02 0.04 0.06arrow_forwardWhat produced the helium now present in the Sun’s atmosphere? In Jupiter’s atmosphere? In the Sun’s core?arrow_forwardWhat is the escape velocity from the Sun? How much greater is it than the escape velocity from Earth?arrow_forward
- c) Derive the Schwarzschild criterion for the onset of convection in an ideal gas, namely d ln T d ln P 7-1 Y Explain all steps in your derivation, and justify any assumptions that you make. d) In a region of convective instability near the surface of a solar-type star of total mass M, the temperature and pressure are related approximately by the expression P KT5/2. Show that the temperature gradient for an ideal gas in hydrostatic = equilibrium in this convection zone is given by dT dr 2Gm(r)μ 5Rr² Further, assuming that the mass in the convection zone is small compared to M, show that at a depth h measured from the top of the convection zone, the temperature is approximately given by T = Ts + 2GMμ -h₂ 5RR² when his small compared to R, and Ts is the temperature at the top of the convection zone.arrow_forwarda. Calculate the surface temperature of Pluto and Charon at perihelion, assuming both bodies are rapid rotators and in equilibrium with the solar radiation field. b. Calculate the escape velocity from Pluto and Charon, and compare these numbers with the velocity of N2, CH4, and H2O molecules. c. Given your answers in (a) and (b), explain qualitatively the differences in surface ice coverage for Pluto and Charon.arrow_forwardProblem 2. Thermal Energy of the Gas Giants: Energy Radiated by Saturn (Palen, et. al., 1st Edition, Chapter 8, problems 40, 62) The equilibrium temperature (Links to an external site.) for Saturn should be 82 K but instead we find an average temperature of 95 K. How much more energy is Saturn radiating into space than it absorbs from the sun? Does this violate the law of conservation of energy? What is the source of this additional energy?arrow_forward
- Calculate the total amount of radiative energy per second intercepted by Mars from the Sun using the flux of radiation from the Sun at Mars' orbital radius. Flux of radiation from the Sun at Mars' orbital radius is 597 W m-2. The luminosity of the Sun Ls = 3.8×1026 W. Mars orbits at a distance of 2.25×1011 m (1.5 AU) from the Sun. Note: Consider carefully the cross-sectional area Mars presents to the outwards flow of radiative energy when answering this question.arrow_forwardCalculate the energy flux density at the average distance of Venus from the Sun rv (energy flux divided by surface area of sphere)Venus' distance from the Sun = rv = 1.082 x 1013 cmF = L /(4prv2) = ________________ ergs/sNext Calcuate the Amount of Solar Energy absorbed by Venus is the surface area of Venus which is facing the Sun (1/2 of Venus' surface area = 4pdv2 / 2 = 2pdv2 ) . Where dv = 6.052 x 106 cm is the radius of Venus. So Venus receives : E = F (2pdv2) = __________________ ergs/s from the Sun.The fraction of the energy flux received which is reflected into space is the albedo of Venus, av, which is about 0.76. The fraction of the energy flux which is absorbed is then (1-av) = 1. - 0.76 = 0.24. So the amount of energy actually absorbed by Venus in each second is Lv = (1-av)Ev.Lv = (1-av)Ev = ___________________ ergs/sarrow_forwardThe Sun is estimated to have about 5.00 billion years left in it’s “normal” (main sequence) lifetime. Assume the average “burn” rate that you computed in question #1, what % of the Sun’s current mass will have been converted at the end of it’s estimated 5.00 billion years of additional life? Actually, the Sun will lose more mass due to the solar wind, CMEs, the neutrio flux etc. the answer to number one was 3.683x10^14arrow_forward
arrow_back_ios
SEE MORE QUESTIONS
arrow_forward_ios
Recommended textbooks for you
Horizons: Exploring the Universe (MindTap Course ...PhysicsISBN:9781305960961Author:Michael A. Seeds, Dana BackmanPublisher:Cengage Learning
AstronomyPhysicsISBN:9781938168284Author:Andrew Fraknoi; David Morrison; Sidney C. WolffPublisher:OpenStax
Foundations of Astronomy (MindTap Course List)PhysicsISBN:9781337399920Author:Michael A. Seeds, Dana BackmanPublisher:Cengage Learning
Stars and Galaxies (MindTap Course List)PhysicsISBN:9781337399944Author:Michael A. SeedsPublisher:Cengage Learning
Horizons: Exploring the Universe (MindTap Course ...
Physics
ISBN:9781305960961
Author:Michael A. Seeds, Dana Backman
Publisher:Cengage Learning
Astronomy
Physics
ISBN:9781938168284
Author:Andrew Fraknoi; David Morrison; Sidney C. Wolff
Publisher:OpenStax
Foundations of Astronomy (MindTap Course List)
Physics
ISBN:9781337399920
Author:Michael A. Seeds, Dana Backman
Publisher:Cengage Learning
Stars and Galaxies (MindTap Course List)
Physics
ISBN:9781337399944
Author:Michael A. Seeds
Publisher:Cengage Learning
Kepler's Three Laws Explained; Author: PhysicsHigh;https://www.youtube.com/watch?v=kyR6EO_RMKE;License: Standard YouTube License, CC-BY