# 1.3: The variables of state, pressure units, and the ideal gas law

Temperature is only one of the key ways that we can describe the properties of a gas. Counting up the number of molecules - or, more reasonably, the number of moles - is another.

These are two of the four conventional variables of state (or state variable) for a gas. The variables of state are considered the ways of describing the entire condition of an ideal gas.

 State variable Symbol SI Unit (mks) Abbreviation Base SI units Temperature T Kelvin K K Count of substance n moles mol mol Volume V cubic meters m3 m3 Pressure P Pascals Pa kg m-1 s-2 (or N m-2)

Volume units are very straightforward; they’re length units in three dimensions, in keeping with a volume being proportional to any length dimension of an object cubed. Of course, the base SI units for volume, cubic meters, are very large indeed; nobody would actually want to lift a cube of anything that was a meter of length on each side. This is why most small-scale exercises will set units of volume to cubic centimeters, or the size of a cube 1 centimeter on each side; this is much more manageable.

Many modern physical chemistry textbooks will make mention of a cubic decimeter, the size of a cube 1 decimeter (or 10 centimeters) on each side. 1 dm3 is just another way to describe one liter, which is the common metric unit of volume. Because of the cubing of 10, there are 1000 liters in a cubic meter; there are 1000 cubic centimeters in a liter, which is why the cubic centimeter and the milliliter are frequently equated with one another.

$1 upper L equals 1 dm cubed equals 1000 cm cubed equals 1000 mL 1 m cubed equals 1000 dm cubed equals 1000 upper L$

Pressure units are much more plentiful, and much more convoluted. Pressure is defined simply as a force per unit area. The base SI unit of pressure is the Pascal, which is equivalent to SI measure of force (the Newton) divided by the SI measure of surface area (the square meter). This is a very small unit of pressure, approximately one-one hundred thousandth normal atmospheric pressure.

Historically standard atmospheric pressure has been defined by the height of a column of mercury that is supported by that pressure, in the nature of an experiment designed by one of Galileo Galiei’s apprentices, Evangelista Torricelli. In his honor, a height of 1 millimeter of mercury in a barometric column is called a torr; standard atmospheric pressure, also known as one atmosphere, is equivalent to a height of 760 mm of mercury in this kind of column; this turns out to be about 101,300 Pascals (or 101.3 kiloPascals).

Most chemists use the atmosphere as their reference atmospheric pressure, but some prefer a truly metric unit, the bar, which is set to exactly 100,000 Pascals (exactly 100 kPa). Meterological pressure is frequently communicated in millibars.

$1 atm equals 760 torr equals 1.013 bar equals 101 300 Pa 1 bar equals 750.2 torr equals 0.9872 atm equals 100 000 Pa$

For reasons that are purely historic, we will prefer the atmosphere as our units of pressure - but there will be times when any of the four will be preferable. Vapor pressures are far more frequently communicated in torr (which, again, is the same thing as mm Hg). When we do computations in base-SI units, we will need Pascals; and again, bars are metric derivations from the Pascal. Atmospheres are simply most frequently used and most easily explained - a multiple of normal atmospheric pressure.

If we take the kinetic theory’s two conditions of ideality of gases - the essentially zero volume of the gas molecules, and the lack of attraction or repulsion between gas molecules - as valid, we find that the ratio of pressure times volume of an ideal gas to number of moles times temperature is a constant:

$upper R equals StartFraction upper P upper V Over n upper T EndFraction upper R equals 0.082058 upper L atm mol Superscript negative 1 Baseline upper K Superscript negative 1 Baseline equals 8.31447 upper J mol Superscript negative 1 Baseline upper K Superscript negative 1$

This is the equation more commonly written as PV = nRT, the ideal gas law. R, like the value of kB, is a constant that will turn up every now and again in our computations. Like the definition of temperature, we can derive this law from first physical principles; however, this is a familiar enough statement to us that we will simply take it as something we know, as a straightforward starting point.

There's one additional thing to note about these two constants we've worked with, the value of kB and the value of R. You see a hint of that thing in the exponent on the value of kB, the exponent of 10-23. Divide the value of R by the value of kB and make a note of what comes out:

$StartFraction upper R Over k Subscript upper B Baseline EndFraction equals StartFraction 8.31447 upper J mol Superscript negative 1 Baseline upper K Superscript negative 1 Baseline Over 1.38065 times 10 Superscript negative 23 Baseline upper J upper K Superscript negative 1 Baseline EndFraction equals 6.0221 times 10 Superscript 23 Baseline mol Superscript negative 1 Baseline right-arrow StartFraction upper R Over k Subscript upper B Baseline EndFraction equals upper N Subscript upper A Baseline$

R and kB are, in many ways, the exact same constant. R, on the one hand, deals with an energy per mole per Kelvin; kB deals with an energy per molecule per Kelvin. The ratio of R to kB is the familiar value of Avogadro's number; this connection can prove useful for us as we move forward.