object near an albedo A, of 0.50. What is its surface temperature assuming that its singular source of heat is sunlight, and that the planet radiate as a black body. Suppose that th eplanet has the mass and radius of pluto. WOuld such a planet be expected to retain carbod Dioxide ( mass=44xmass of hydrogen)?
Answers:
The sun emit energy at a rate of P = 4x10^26 W. The amount of power density that reach the icy planey is then this
Pd = P/(4*pi*R^2)
where on earth R is the distance from the sun to the planet. This is the total flux of energy emit by the sun spread over the surface area of a sphere of radius R. The albedo (A) of a planet indicates how much of the incident vigour is reflected posterior into space. The absorbed power density is later
Pa = (1 - A)*Pd = (1 - A)*P/(4*pi*R^2).
The absorbed vigour heats the planet and also lead to radiation. The radiated power follows the Stefan-Boltzmann canon
Pr = e*s*T^4
where e is the emissivity, s is Stefan's constant, and T is the warmth of the radiating body. Stefan's constant is s = 5.67x10^-8 W/(m^2*K^4), and for a blackbody, the emissivity is one.
At equilibrium, the absorbed power and the radiate power are equal
(1 - A)*P/(4*pi*R^2) = s*T^4
which can be solved for T, the temperature of the planet.
The heat of the planet will impart kinetic energy to gas molecules within the air. The speed of the molecules will be distributed beside an rms spedd os
Vrms = sqrt(3*k*T/m) = sqrt(3*R*T/M)
where k is Boltzmann's constant, R is the wide-reaching gas constant, m is the mass of the molecule, and M is the molar mass.
For a planet the escape velocity for an object is given by
Vesc = sqrt(2*G*M/r)
where on earth G is the universal gravitation constant, M is the mass of the planet, and r is the planet's radius.
If the speed of the gas molecules is greater than the escape velocity of the planet, later that planet will not be able to retain that gas at the given heat.
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Answers:
The sun emit energy at a rate of P = 4x10^26 W. The amount of power density that reach the icy planey is then this
Pd = P/(4*pi*R^2)
where on earth R is the distance from the sun to the planet. This is the total flux of energy emit by the sun spread over the surface area of a sphere of radius R. The albedo (A) of a planet indicates how much of the incident vigour is reflected posterior into space. The absorbed power density is later
Pa = (1 - A)*Pd = (1 - A)*P/(4*pi*R^2).
The absorbed vigour heats the planet and also lead to radiation. The radiated power follows the Stefan-Boltzmann canon
Pr = e*s*T^4
where e is the emissivity, s is Stefan's constant, and T is the warmth of the radiating body. Stefan's constant is s = 5.67x10^-8 W/(m^2*K^4), and for a blackbody, the emissivity is one.
At equilibrium, the absorbed power and the radiate power are equal
(1 - A)*P/(4*pi*R^2) = s*T^4
which can be solved for T, the temperature of the planet.
The heat of the planet will impart kinetic energy to gas molecules within the air. The speed of the molecules will be distributed beside an rms spedd os
Vrms = sqrt(3*k*T/m) = sqrt(3*R*T/M)
where k is Boltzmann's constant, R is the wide-reaching gas constant, m is the mass of the molecule, and M is the molar mass.
For a planet the escape velocity for an object is given by
Vesc = sqrt(2*G*M/r)
where on earth G is the universal gravitation constant, M is the mass of the planet, and r is the planet's radius.
If the speed of the gas molecules is greater than the escape velocity of the planet, later that planet will not be able to retain that gas at the given heat.
Related Questions:
I own solar panel on my roof, is it middle-of-the-road for hose down to be pouring out into the gutter?
No. Depending on what kind of panels you have, a nouns valve could be hung open (if it got too hot), you could own a faulty panel, or the interconnecting piping could be compromised. Either way, the system should be looked...