In the following chapters we will present various chemical reaction mechanisms controlling the abundance of stratospheric ozone, the oxidizing power of the atmosphere, smog, and acid rain. We first review here some basic notions of chemical kinetics.
A bimolecular reaction involves the collision of two reactants A and B to yield two products C and D. The collision produces an activated complex AB* which decomposes rapidly either to the original reactants A and B or to the products C and D. The reaction is written
where k is the rate constant for the reaction. In this expression the concentrations [ ] are number densities so that the product [A][B] is proportional to the frequency of collisions. The rate of the reaction depends on the frequency of collisions and on the fate of the activated complex. Typically k is given in units of cm3 molecule-1s-1, in which case [A] and [B] must be in units of molecules cm-3.
The third body M is any inert molecule (in the atmosphere, generally N2 and O2) that can remove the excess energy from AB* and eventually dissipate it as heat. Common practice is to write the overall reaction as
The rate of a three-body reaction is defined as the formation rate of AB by reaction See :
The excited complex AB* has a very short lifetime and reacts as soon as it is produced. We may therefore assume that it is in steady state at all times (see section 3.1.2 for a discussion of this quasi steady state):
Rearranging and replacing into (9.3) :
where the equality between production of AB on the one hand, and losses of A and B on the other hand, follows from the steady state assumption for AB*. In the atmosphere, [M] is simply the number density of air na.
Equation (9.5) is the general rate expression for a three-body reaction (a more detailed analysis would include a small correction factor). There are two interesting limits. In the low-density limit [M] << k4/k5 (called the low-pressure limit), (9.5) simplifies to
so that the rate of the overall reaction depends linearly on [M]. One refers to ko = k3k5/k4 as the low-pressure limit rate constant. In the high-density limit [M] >> k4/k5 (called the high-pressure limit), (9.5) simplifies to
which means that the rate of AB production is limited by production of AB* and is independent of [M]; M is sufficiently abundant to ensure that all AB* complexes produced stabilize to AB. Since the rate of the overall reaction is then determined by the rate of See , one refers to See in the high-pressure limit as the rate-limiting step for production of AB, and k· = k3 as the high-pressure limit rate constant. Rewriting (9.5) in terms of ko and k· makes the two limits apparent:
The rate constant of a three-body reaction is sometimes given as one of the two limits; you can tell from the units of k (cm6 molecule-2 s -1 for the low-pressure limit, cm3 molecule-1 s-1 for the high-pressure limit) and you should then assume that the appropriate limit holds.
from which we define an equilibrium constant K10 for the two-way reaction See :
Consider an elemental slab of air of vertical thickness dz and unit horizontal area. The slab contains [X]dz molecules of X (where [X] is a number density). A photon incident on a molecule of X has a probability sX/A of being absorbed, where A is the cross-sectional area of the molecule and sX is the absorption cross-section (units of cm2 molecule-1) which defines the absorption characteristics of X. The molecules of X in the elemental slab absorb a fraction sX[X]dz of the incoming photons. We define the actinic flux I as the number of photons crossing the unit horizontal area per unit time from any direction (photons cm-2 s-1) and the quantum yield qX (units of molecules photon-1) as the probability that absorption of a photon will cause photolysis of the molecule X. The number of molecules of X photolyzed per unit time in the slab is qXsX[X]Idz. To obtain the photolysis rate constant k, we divide by the number [X]dz of molecules of X in the slab:
Absorption cross-sections and quantum yields vary with wavelength. For polychromatic radiation, as in the atmosphere, equation (9.12) must be integrated over the wavelength spectrum:
where Il is the actinic flux distribution function defined in the same way as the flux distribution function fl in chapter 7. The difference between the actinic flux Il and the radiation flux fl is that the former measures the number of photons crossing the unit horizontal surface surface from any direction, while the latter measures the photon energy flow perpendicular to the surface. Solar photons in the atmosphere originate from a multiplicity of directions due to scattering by air molecules, aerosols, and clouds; the relationship between fl and Il varies depending on the angular distribution of the photons.
Gases in the atmosphere are present at low concentrations - considerably lower than the concentrations generally used in laboratory experiments or in industrial processes. As a result, collisions between molecules are relatively infrequent. With few exceptions, the only reactions between molecules that proceed at appreciable rates in the atmosphere are those involving at least one radical species.
Radicals are defined as chemical species with an unpaired electron in the outer ( valence) shell. Because of this unpaired electron, radicals have high free energies and are much more reactive than nonradical species whose electrons are all paired up. You can figure out whether or not a species is a radical by counting its electrons; an odd number identifies a radical and an even number a nonradical. For example NO is a radical (7+8 = 15 electrons), while HNO3 is a nonradical (1+7+(3x)8 = 32 electrons). An important exception to this rule is atomic oxygen, which has 8 electrons but two unpaired valence shell electrons in its "triplet" O(3P) ground state (2s22px22py12pz1) and is therefore a radical (or more exactly a biradical). Atomic oxygen with all electrons paired (2s22px22py2) is in a higher-energy "singlet" O(1D) state and is actually even more reactive than O(3P).
Because radicals have high free energies, their formation from nonradical species is in general endothermic; an external source of energy is required. In the atmosphere, this source of energy is supplied by solar radiation:
Generation of radicals by reaction (R12) provides the initiation step for radical reaction chains which are propagated by subsequent reactions of radicals with nonradical species:
Note that reaction of a radical with a nonradical must always produce a radical in order to conserve the total odd number of electrons. The radical produced in (R13) goes on to react with another nonradical, propagating the chain, and in this manner a large number of nonradicals can be processed through the chain. During the propagation cycle, a nonradical species produced by a reaction of type (R13) may photolyze following (R12) to produce additional radicals; the photolysis is called a branching reaction as it accelerates (or "branches") the chain by augmenting the pool of radicals.
Termination reactions are generally slower than propagation reactions because radicals are present at low concentrations and collisions between radicals are therefore relatively infrequent. In subsequent chapters we will encounter many types of radical-assisted chains following the general schematic (R12) - (R15) . Due to the critical importance of solar radiation in initiating radical-assisted chain mechanisms in the atmosphere, these mechanisms are often referred to as photochemical.