The atmosphere of the planet Venus is almost entirely composed of carbon dioxide (about 96.5% CO2). The carbon dioxide on Venus could be in equilibrium with carbonate ions in minerals on the planet's crust. Two possible equilibrium systems involve CaSiO3 and MgSiO3. CaSiO3(s) + CO2(g) ⇔⇔CaCO3(s) + SiO2(s). System 1 MgSiO3(s) + CaCO3(s) + SiO2(s) ⇔⇔ CaMgSi2O6(s) + CO2(g) System 2 The first graph that follows shows the expected pressures of carbon dioxide (in atm) at different temperatures for each of these equilibrium systems. (Note that the x-axes on this graph is logarithmic). The second graph is a phase diagram for carbon dioxide. Examine the graphs and answer the questions. Q#1: The partial pressure of carbon dioxide on the surface of Venus is 91 atm. What is the value of the equilibrium constant (Kp) if the Venusian carbon dioxide is in equilibrium according to system 1? According to system 2? Q#2: The approximate temperature on the surface of Venus is about 740K. What is the approximate carbon dioxide partial pressure for system 1 at this temperature? For system 2? (Use a point at approximately the middle of each colored band, which represents the rage of possible value to estimate the carbon dioxide partial pressure.) Q#3: Use the partial pressure of carbon dioxide on the surface of Venus given in part a to determine which of the two equilibrium systems is more likely to be responsible for the carbon dioxide on the surface of Venus. Q#4: From the carbon dioxide phase diagram, determine the minimum pressure required for supercritical carbon dioxide to form. If the partial pressure of carbon dioxide on the surface of Venus was higher in the distant past, could supercritical carbon dioxide have existed on the surface of Venus?
The atmosphere of the planet Venus is almost entirely composed of carbon dioxide (about 96.5% CO2). The carbon dioxide on Venus could be in equilibrium with carbonate ions in minerals on the planet's crust. Two possible equilibrium systems involve CaSiO3 and MgSiO3.
CaSiO3(s) + CO2(g) ⇔⇔CaCO3(s) + SiO2(s). System 1
MgSiO3(s) + CaCO3(s) + SiO2(s) ⇔⇔ CaMgSi2O6(s) + CO2(g) System 2
The first graph that follows shows the expected pressures of carbon dioxide (in atm) at different temperatures for each of these equilibrium systems. (Note that the x-axes on this graph is logarithmic). The second graph is a phase diagram for carbon dioxide. Examine the graphs and answer the questions.
Q#1: The partial pressure of carbon dioxide on the surface of Venus is 91 atm. What is the value of the equilibrium constant (Kp) if the Venusian carbon dioxide is in equilibrium according to system 1? According to system 2?
Q#2: The approximate temperature on the surface of Venus is about 740K. What is the approximate carbon dioxide partial pressure for system 1 at this temperature? For system 2? (Use a point at approximately the middle of each colored band, which represents the rage of possible value to estimate the carbon dioxide partial pressure.)
Q#3: Use the partial pressure of carbon dioxide on the surface of Venus given in part a to determine which of the two equilibrium systems is more likely to be responsible for the carbon dioxide on the surface of Venus.
Q#4: From the carbon dioxide phase diagram, determine the minimum pressure required for supercritical carbon dioxide to form. If the partial pressure of carbon dioxide on the surface of Venus was higher in the distant past, could supercritical carbon dioxide have existed on the surface of Venus?
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