1:4 Calculate the work performed by 0.01 kg of oxygen (M oxygen = 31.999)
expanding isothermally* at 20 °C from 1 to 0.3 atm of pressure.
0.917 kJ
1:5 Everything we experience is at disequilibrium (the universe is expanding and
we’re on a warm planet in cold space but exposed to the sun’s hot rays). How
come, or why, we develop a physics based on equilibrium states?
*All these processes are internally reversible and quasi-static (see Chap. 6).
References
1. Henderson LJ (1917) The Order of Nature. Harvard University Press, Cambridge
2. Schumacher EF (1973) Small is Beautiful. Harper and Row, New York (p. 47)
3. Planck M (1969) Treatise on Thermodynamics, 3rd edition. Dover, New York
4. Callen HB (1
st edition, 1960; 2nd edition, 1985) Thermodynamics and an Introduction to
Thermostatistics. Wiley, New York
5. Kondepudi D, Prigogine I (1998) Modern Thermodynamics: From Heat Engines to Dissipative
Structures. Wiley, New York
6. Zemansky MK (1943) Heat and Thermodynamics, 2
nd edition. McGraw-Hill, New York
1.10 Quantity of Heat
23
expanding isothermally* at 20 °C from 1 to 0.3 atm of pressure.
0.917 kJ
1:5 Everything we experience is at disequilibrium (the universe is expanding and
we’re on a warm planet in cold space but exposed to the sun’s hot rays). How
come, or why, we develop a physics based on equilibrium states?
*All these processes are internally reversible and quasi-static (see Chap. 6).
References
1. Henderson LJ (1917) The Order of Nature. Harvard University Press, Cambridge
2. Schumacher EF (1973) Small is Beautiful. Harper and Row, New York (p. 47)
3. Planck M (1969) Treatise on Thermodynamics, 3rd edition. Dover, New York
4. Callen HB (1
st edition, 1960; 2nd edition, 1985) Thermodynamics and an Introduction to
Thermostatistics. Wiley, New York
5. Kondepudi D, Prigogine I (1998) Modern Thermodynamics: From Heat Engines to Dissipative
Structures. Wiley, New York
6. Zemansky MK (1943) Heat and Thermodynamics, 2
nd edition. McGraw-Hill, New York
1.10 Quantity of Heat
23