An Introduction to Thermal Physics
1st Edition
ISBN: 9780201380279
Author: Daniel V. Schroeder
Publisher: Addison Wesley
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Question
Chapter 7.4, Problem 56P
(a)
To determine
The solar constant for Venus and the average temperature of the surface of Venus.
(b)
To determine
The temperature of Venus considering the reflectivity of the clouds.
(c)
To determine
The temperature of Venus.
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Students have asked these similar questions
A. The planet Venus is different from the earth in several respects: (a) it is
only 70 % as far from the sun, so the solar constant is 2800 W/m²; (b) its
thick clouds reflect 77% of all incident sunlight and (c) its atmosphere is
much more opaque to infrared light.
B.
(i) Estimate what the average surface temperature of Venus would be if it
had no atmosphere and did not reflect any sunlight.
(ii) Taking into account the reflectivity of the clouds, estimate the surface
temperature.
Use the theory of Earth's energy balance to discuss the greenhouse effect.
Our Sun shines bright with a luminosity of 3.828 x 1026 Watt. Her energy is responsible for many processes and the habitable temperatures on the Earth that make our life possible.
Calculate the amount of energy arriving on the Earth in a single day.
To how many litres of heating oil (energy density: 37.3 x 106 J/litre) is this equivalent?
The Earth reflects 30% of this energy: Determine the temperature on Earth’s surface.
What other factors should be considered to get an even more precise temperature estimate?
Note: The Earth’s radius is 6370 km; the Sun’s radius is 696 x 103 km; 1 AU is 1.495 x 108 km.
In contrast to Venus, the coldest temperature yet measured on the surface of
any body in the solar system is -235°C. This temperature was detected by
Voyager 2 as it passed by Neptune's largest moon, Triton. What is Triton's
surface temperature in degrees Fahrenheit and in kelvins?
The warmest temperature in Antarctica was recorded at the Vanda Station on
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Answer must be given as calculated
and then to the side given in
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Chapter 7 Solutions
An Introduction to Thermal Physics
Ch. 7.1 - Prob. 1PCh. 7.1 - Prob. 3PCh. 7.1 - Prob. 4PCh. 7.1 - Show that when a system is in thermal and...Ch. 7.1 - Prob. 7PCh. 7.2 - Prob. 8PCh. 7.2 - Prob. 9PCh. 7.2 - Prob. 11PCh. 7.2 - Prob. 12PCh. 7.2 - Prob. 13P
Ch. 7.2 - Prob. 14PCh. 7.2 - Prob. 15PCh. 7.2 - Prob. 16PCh. 7.2 - Prob. 17PCh. 7.2 - Prob. 18PCh. 7.3 - Prob. 19PCh. 7.3 - Prob. 20PCh. 7.3 - Prob. 21PCh. 7.3 - Prob. 22PCh. 7.3 - Prob. 24PCh. 7.3 - Prob. 25PCh. 7.3 - Prob. 26PCh. 7.3 - Prob. 29PCh. 7.3 - Prob. 32PCh. 7.3 - Prob. 33PCh. 7.3 - Prob. 34PCh. 7.4 - Prob. 37PCh. 7.4 - Prob. 38PCh. 7.4 - Prob. 39PCh. 7.4 - Prob. 40PCh. 7.4 - Prob. 41PCh. 7.4 - Prob. 42PCh. 7.4 - Prob. 43PCh. 7.4 - Prob. 44PCh. 7.4 - Prob. 45PCh. 7.4 - Prob. 46PCh. 7.4 - Prob. 47PCh. 7.4 - Prob. 48PCh. 7.4 - Prob. 49PCh. 7.4 - Prob. 50PCh. 7.4 - Prob. 51PCh. 7.4 - Prob. 52PCh. 7.4 - Prob. 53PCh. 7.4 - Prob. 54PCh. 7.4 - Prob. 55PCh. 7.4 - Prob. 56PCh. 7.5 - Prob. 57PCh. 7.5 - Prob. 58PCh. 7.5 - Prob. 59PCh. 7.5 - Prob. 60PCh. 7.5 - The heat capacity of liquid 4He below 0.6 K is...Ch. 7.5 - Prob. 62PCh. 7.5 - Prob. 63PCh. 7.5 - Prob. 64PCh. 7.6 - Prob. 65PCh. 7.6 - Prob. 66PCh. 7.6 - Prob. 67PCh. 7.6 - Prob. 68PCh. 7.6 - If you have a computer system that can do...Ch. 7.6 - Prob. 70PCh. 7.6 - Prob. 71PCh. 7.6 - Prob. 72PCh. 7.6 - Prob. 73PCh. 7.6 - Prob. 75P
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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 radiant flux at Earth is 1365 W/m2. Say we move towards the sun to a radius that is 1/3 the radius of the Earth's orbit. By what factor would the radiant flux increase or decrease?arrow_forwardHow is the distance from the sun for planets in our solar system related to the mean temperature of each planet? To find out, a scatterplot that relates the natural log of the distance of each planet (including Pluto) from the sun in millions of miles and the natural log of the mean planetary temperature in Kelvin was created. In(Temperature) vs. In(Distance) 6.8 6.6 6.4 6.2 6 5.8 5.6 5.4 5.2 4.8 4.6 4.4 4.2 4 4 6 7 8. In(Distance) Predictor Coef 7.9009 SE Coef P Conatant 0.4381 18.03 0.000 In Distance -0.4536 0.0706 -6.42 0.004 s = 0.3446 R-Sq = 85.5 R-8q (adj) = 83.2% Based on the scatterplot and computer output, a reasonable estimate of mean temperature in Kelvin for Saturn, which is 886.7 million miles away from the sun is: O 4.822 degrees Kelvin because ý = -0.4536(In 886.7) + 7.9009 = 4.822. O 124.2 degrees Kelvin because in y = -0,4536(in 886,7) + 7.9009 =4,822 and e4.822 = 124.2. O 709.0 degrees Kelvin because In y = - 0.4536(log 886.7) + 7.9009 =6.564 and e6.564 = 709.0. O…arrow_forwardThe next four questions use this description. Our Sun has a peak emission wavelength of about 500 nm and a radius of about 700,000 km. Your dark-adapted eye has a pupil diameter of about 7 mm and can detect light intensity down to about 1.5 x 10-11 W/m2. Assume the emissivity of the Sun is equal to 1. First, given these numbers, what is the surface temperature of the Sun in Kelvin to 3 significant digits? What is the power output of the Sun in moles of watts? (in other words, take the number of watts and divide it by Avogadro's number) Assuming that all of the Sun's power is given off as 500 nm photons*, how many photons are given off by the Sun every second? Report your answer to the nearest power of 10 (e.g. if you got 7 x 1024, give your answer as 25).arrow_forward
- The Stefan-Boltzmann Law says that the light radiated from a perfect radiator ("blackbody") is proportional to the temperature raised to the fourth power: where σ is the Stefan-Boltzmann constrant (σ = 5.67 x 10-8 in MKS units) In equilibrium, F coming in equals F going out. At Mars' distance from the Sun, F coming in is 153 in MKS units. What is the blackbody temperature for Mars at a distance of 1.524 AU from the Sun?arrow_forwardThe following heat transfer formula quantifies the radiation emitted from the Sun: P = eoA(T4 – T?) Equation 5 where: P= radiated power (Watts) e = emissivity (=1 for ideal radiator; unitless) o = Stefan-Boltzmann constant = 5.67x10-8 W/m2-K+ A = radiating area (m²) T= temperature of radiator (Kelvin) Tc = temperature of surroundings (Kelvin) Q3 Using the following values, together with equation 5, calculate the power emitted by the Sun. sun's surface temperature = 5780 K temperature of the environment that the Sun is located in = 4 K emissivity of the Sun = 1 radius of the Sun = 695,700,000 m Stephen-Boltzmann constant o = 5.67 x 10-8 W/m2-K4 Show your work below-you may use the equation editor or insert a picture of your handwritten work.arrow_forwardUse the value of the solar energy flux on Earth to determine the radius of the Sun. Assuming that the Sun's temperature is 5780 K and that its emissivity is 1, find its radius in kilometers. Neglect the temperature of the environment.arrow_forward
- The planet Venus is different from the earth in several respects. First, it is only 70% as far from the sun. Second, its thick clouds reflect 77% of all incident sunlight. Finally, its atmosphere is much more opaque to infrared light. Estimate the surface temperature again, taking the reflectivity of the clouds into account.arrow_forwardThe average temperature of the atmosphere has increased by 0.4°C over the last thirty years. Estimate how much energy has gone into warming up the planet in this way. Keep in mind that the atmosphere has a mass of 5 × 1018kg, and the specific heat capacity of air is about 1 Jg−1K−1. How do we get to this answer (2×1021J)arrow_forwarda) Calculate the escape velocity for hydrogen atoms from the surface (the photosphere) of our Sun. The Sun has a mass of 1.99×1030 kg and a radius of 6.96×108 m. b) If the velocity in (a) were the root-mean-squared of the hydrogen atoms in the Sun, what would the temperature of the photosphere have to be?arrow_forward
- Proxima Centauri, the nearest star to our Sun, has a surface temperature of 2,768.85 °C. What is its total intensity emitted? O 4.3 MW per square meter. O 4.9 MW per square meter. O 5.2 MW per square meter. O 5.7 MW per square meter. O 6.4 MW per square meter.arrow_forwardThe amount of radiant energy emitted by a surface is given by q = ɛ0 AT+ where q represents the rate of thermal energy (per unit time) emitted by the surface in watts; e = the emissivity of the surface 0<ɛ<1 and is unitless o = Stefan-Boltzman constant (o = 5.67×10% ) A represents the area of the surface in m² Ty = surface temperature of the object expressed in kelvin What are the appropriate units for o if the equation is to be homogeneous in 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
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