Planetary Atmospheres. (a) Calculate the density of the atmosphere at the surface of Mars (where the pressure is 650 Pa and the temperature is typically 253 K, with a CO 2 atmosphere), Venus (with an average temperature of 730 K and pressure of 92 atm, with a CO 2 atmosphere), and Saturn’s moon Titan (where the pressure is 1.5 atm and the temperature is −178°C, with a N 2 atmosphere). (b) Compare each of these densities with that of the earth’s atmosphere, which is 1.20 kg/m 3 . Consult Appendix D to determine molar masses.
Planetary Atmospheres. (a) Calculate the density of the atmosphere at the surface of Mars (where the pressure is 650 Pa and the temperature is typically 253 K, with a CO 2 atmosphere), Venus (with an average temperature of 730 K and pressure of 92 atm, with a CO 2 atmosphere), and Saturn’s moon Titan (where the pressure is 1.5 atm and the temperature is −178°C, with a N 2 atmosphere). (b) Compare each of these densities with that of the earth’s atmosphere, which is 1.20 kg/m 3 . Consult Appendix D to determine molar masses.
Planetary Atmospheres. (a) Calculate the density of the atmosphere at the surface of Mars (where the pressure is 650 Pa and the temperature is typically 253 K, with a CO2 atmosphere), Venus (with an average temperature of 730 K and pressure of 92 atm, with a CO2 atmosphere), and Saturn’s moon Titan (where the pressure is 1.5 atm and the temperature is −178°C, with a N2 atmosphere). (b) Compare each of these densities with that of the earth’s atmosphere, which is 1.20 kg/m3. Consult Appendix D to determine molar masses.
Soon after Earth was formed, heat released by the decay of radioactive elements raised the average internal temperature from 300 to 3000 K, at about which value it remains today. Assuming an average coefficient of volume expansion of 3.0 * 10-5 K-1, by how much has the radius of Earth increased since the planet was formed?
Here we would like to figure out why we do not seem to have any molecular hydrogen in the Martian atmosphere. Although this can get very complicated quickly IRL, we can simplify things by asking a couple of questions, one at a time. We will examine just molecular hydrogen as a diatomic ideal gas. The molar mass of molecular hydrogen is about 2 x 10-3 kg/mol. The mass of Mars is about 6.4 x 1023 kg, and the mean radius of Mars is about 3.39 x 106 m.a) First, we would like to see if Martian gravity has what it takes to hold molecular hydrogen. Calculate the mean escape velocity at the surface of Mars.
b) Then, we would like to see if Mars is too hot to hold molecular hydrogen. Calculate the rms speed of molecular hydrogen at an average Martian atmospheric temperature of 210 K. Is molecular hydrogen expected to escape at this speed
c) Perhaps if we wanted to be really sure we did not miss anything, we can examine another scenario. The Martian upper atmosphere (thermosphere and up) is…
Space probes to Mars have shown that its atmosphere consists mostly of carbon dioxide. The average temperature on the surface of Mars is –55°C with a pressure of 0.00570 atm. Compare the density of on Mars’s surface with that on the Earth’s surface at 17°C and one atmosphere.
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.