the Creative Commons Attribution 4.0 License.

the Creative Commons Attribution 4.0 License.

# The ion–ion recombination coefficient *α*: comparison of temperature- and pressure-dependent parameterisations for the troposphere and stratosphere

### Marcel Zauner-Wieczorek

### Joachim Curtius

### Andreas Kürten

Many different atmospheric, physical, and chemical
processes are affected by ions. An important sink for atmospheric ions is
the reaction and mutual neutralisation of a positive and negative ion, also
called ion–ion recombination. While the value for the ion–ion recombination coefficient *α* is well-known for standard conditions (namely 1.7 × 10^{−6} cm^{3} s^{−1}), it needs to be calculated for deviating temperature and pressure conditions, especially for applications at higher altitudes of the atmosphere. In this work, we review the history of theories and parameterisations of the ion–ion recombination coefficient, focussing on the temperature and pressure dependencies as well as the altitude range between 0 and 50 km. Commencing with theories based on J. J. Thomson's work, we describe important semi-empirical adjustments as well as
field, model, and laboratory data sets, followed by short reviews of binary
recombination theories, model simulations, and the application of
ion–aerosol theories to ion–ion recombination. We present a comparison
between theories, parameterisations, and field, model, and laboratory data sets to conclude favourable parameterisations. While many theories agree well with field data above an altitude of approximately 10 km, the nature of the recombination coefficient is still widely unknown between Earth's surface and an altitude of 10 km. According to the current state of knowledge, it appears reasonable to assume an almost constant value for the recombination coefficient for this region, while it is necessary to use values that are adjusted for pressure and temperature for altitudes above 10 km. Suitable parameterisations for different altitude ranges are presented and the need for future research, be it in the laboratory or by means of modelling, is identified.

*α*: comparison of temperature- and pressure-dependent parameterisations for the troposphere and stratosphere, Atmos. Chem. Phys., 22, 12443–12465, https://doi.org/10.5194/acp-22-12443-2022, 2022.

Earth's atmosphere is not only a neutral mixture of gases, but also contains
gas-phase ions that are crucial to the phenomena of atmospheric electricity.
They play a central role in meteorological processes in thunderstorms
(Sagalyn et al., 1985), maintaining the global atmospheric electrical
circuit (Harrison, 2004), the formation of aerosol particles with the
ion-induced nucleation mechanism (Hirsikko et al., 2011), and the
propagation of radio waves in the ionosphere (Basu et al., 1985), to name
but a few processes. It is thus important to understand the
production and loss of atmospheric ions. There are several sources of ions
in the atmosphere, of which ionisation by galactic cosmic rays (GCRs) is the
most important (Bazilevskaya et al., 2008). Close to the ground, ionisation
by the radioactive decay of radon as well as lightning are additional
sources of atmospheric ions (Viggiano and Arnold, 1995). Further, minor
sources of ionisation in the atmosphere include solar cosmic rays (also
called solar energetic particles, SEPs) and magnetospheric electrons
(Bazilevskaya et al., 2008). The two important sinks for atmospheric ions
are the reaction of a positive ion and negative ion, the so-called
recombination, as well as the condensation of ions onto aerosol particles
(Viggiano and Arnold, 1995). The ion–ion recombination coefficient *α*
describes the reaction rate of the recombination of a positive and negative
ion in the gas phase; its unit is cm^{3} s^{−1}, which is used
throughout this work unless noted otherwise. There are two important
recombination mechanisms: binary recombination, in which two ions of
opposite sign recombine upon collision, and ternary recombination, in which
one of the ions first collides with a neutral gas molecule, i.e. the third
body, to dissipate energy in order to recombine successfully with the second
ion. Hence, the latter process is also called three-body trapping. When
both the binary and ternary processes are included in a theory or
parameterisation, it is called total recombination. While ion–ion
recombination concerns the recombination of atomic or molecular ions or
small molecular ion clusters, ion–aerosol attachment regards the interaction
between an ion and a charged or neutral aerosol particle. Typically, aerosol
particles are defined to have a size of 1 nm or bigger. As the ion–aerosol
attachment coefficient depends on the size of the aerosol particle, the
ion–ion recombination coefficient can be viewed as a special case of the
former if the “aerosol particle” is considered to have ionic size and is
singly charged.

In this work, we focus on ion–ion recombination and summarise the history
and fundamentals of the theory behind it in Sect. 2, followed by a
description of the theories of the binary ion–ion recombination process in
Sect. 3. In Sect. 4, we discuss the field and laboratory measurements and
subsequent semi-empirical parameterisations of ion–ion recombination. We
focus on the applicability of the theory to atmospheric conditions,
especially for the troposphere and stratosphere, i.e. in an altitude range
of 0–50 km. We describe the application of ion–aerosol
theories to the ion–ion recombination in Sect. 5, followed by an overview of numerical simulations in Sect. 6. Thereafter, we compare the available parameterisations and theories with field data, laboratory data, and a model simulation for the atmospheric altitude range of 0–50 km in Sect. 7. The determination of the three-body trapping sphere radius and the collision probability in the limiting sphere (a concept used in different theories) can be found in Sect. 8. Finally, we conclude the applicability of the discussed theories to atmospheric conditions and identify the demand for future research in Sect. 9. To improve the readability, we adhere to the conventionally used units of
hPa and atm for pressure, cm^{3} s^{−1} for the recombination rate and
related quantities, eV for the electron affinity, and km for the atmospheric
altitude; otherwise, we use the SI units.

The theoretical foundation of the recombination of gaseous ions was laid
down by J. J. Thomson and Ernest Rutherford. The theory based on their
approach is referred to as the Thomson theory in the literature. In their work
“On the Passage of Electricity of Gases exposed to Röntgen Rays”,
Thomson and Rutherford (1896) discuss, for the first time, the sources and
sinks of ions in the gas phase. In their experimental setup, the source of
ions are X-rays, while the sinks are the recombination of negative and
positive ions as well as losses to the electrodes. They describe the
temporal change of the number concentration of ions *n* according to Eq. (1):

where *t* is the time, *q* is the ion production rate, and *L* is the loss rate to the electrodes. This formula already includes the assumption that the number concentrations of negative and positive ions, *n*_{−} and *n*_{+}, are approximately equal and, therefore, the product ${n}_{-}{n}_{+}$ can be simplified to
*n*^{2}. They conclude that when the electrode current is small (*L* ≈ 0) and the system is in a steady state ($\mathrm{d}n/\mathrm{d}t=\mathrm{0}$), the number
concentration of gas-phase ions can be calculated in a simple way (Eq. 2):

As per today's convention, *q* is the production rate for ion pairs so that *n* in Eqs. (1) and (2) must be specified to be either *n*_{+} or *n*_{−}, not to be confused with *n*_{total} = ${n}_{+}+{n}_{-}$. Equation (2) can be
rearranged to determine *α* when the ion pair production rate and the
number concentration of positive or negative ions are known. A few years
later, in 1906, the Nobel Prize in Physics was awarded to J. J. Thomson for
his studies on the electrical conductivity of gases.

Soon after Thomson and Rutherford's publication, several experiments to
determine the ion–ion recombination coefficient were pursued by different
scientists. It was shown that *α* is dependent on the chemical
composition of the surrounding gas, as well as on the temperature and
pressure. Here, we focus on experiments in air. Many of these first
approaches have been reviewed by Lenz (1932), who himself had developed a
sophisticated experimental setup in order to control losses due to diffusion
and deposition on walls. It is remarkable that even during this time, the
determined values of *α* are similar to the one used today and have
not changed significantly since then. For standard conditions, i.e. 273.15 K
and 1013 hPa, Thirkill (1913) determined a value of 1.7 × 10^{−6} cm^{3} s^{−1}, while Thomson (1924) determined a value of 2.0 × 10^{−6} cm^{3} s^{−1}. Lenz (1932) reported (1.7 ± 0.1) × 10^{−6} cm^{3} s^{−1} for the
conditions of 291.15 K and 1013 hPa. The value for *α* used nowadays
is 1.6 × 10^{−6} cm^{3} s^{−1} (e.g. Franchin et al., 2015)
and is taken from Israël (1971) (which is the English translation of the
first edition in German: Israël, 1957). In addition, Gardner (1938)
reported the value of 2.1 × 10^{−6} cm^{3} s^{−1} for pure
oxygen, 1013 hPa, and 298.15 K. Sayers (1938) reported a value of
2.3 × 10^{−6} cm^{3} s^{−1}, while Nolan (1943), who has
also reviewed previous works, concluded 1.4 × 10^{−6} cm^{3} s^{−1}. Within a particular uncertainty range, these
values do agree quite well and no further ado appears to be necessary to
discuss this value. However, the values for *α* differ tremendously
when temperatures are lower than 273.15 K and pressures are lower than
1013 hPa, as Lenz (1932) has already shown. Loeb (1960) pointed out that before the 1950s, measurement techniques were not sophisticated enough and gases not pure enough to be able to determine the ion–ion
recombination accurately. In any case, a correct value for *α* is crucial for the analysis of field data and the calculations of atmospheric models at higher altitudes in the atmosphere where the temperatures and pressures are different from those at ground level. This calls for a good understanding of the mechanisms involved in ion–ion recombination and a solid parameterisation of *α*.

In a later work, Thomson (1924) explains his theory in more detail and
provides a kinetic derivation of the recombination coefficient. In his
approach, recombination occurs when the two oppositely charged ions each
collide with a neutral molecule of the surrounding gas within a certain
sphere *d*_{T} around the respective ions. It is defined as the sphere in which the ions of opposite signs experience Coulomb attraction (Loeb, 1960); thus, it can be derived from equalising the Coulomb potential energy,
*e*^{2}(4*π**ε*_{0}*d*_{T})^{−1}, and the thermal energy
of motion from the surrounding molecules and ions in the absence of an
electrical field, 1.5 *k*_{B}*T* (Loeb, 1960), as shown in Eq. (3):

where *e* is the elementary charge, *ε*_{0} is the vacuum
permittivity, *k*_{B} is the Boltzmann constant, and *T* is the temperature.
Loeb (1960) stresses that the pre-factor value of 1.5 for the thermal energy
is debated, ranging from 1 (Tamadate et al., 2020b), 1.5 (Thomson, 1924),
and 2.4 (Natanson, 1959a) to 6 (Loeb and Marshall, 1929), amongst others.
Loeb and Marshall (1929) approximate the radius *d*_{T} to be in the order of 10 nm when the value of 6 *k*_{B}*T* is used for the thermal energy. Thus, a rough estimate of 10–60 nm for *d*_{T} can be derived from different Thomsonian theories.

Thomson deduced that *α* is dependent on the average speeds of the
positive and negative ion, *v*_{+} and *v*_{−}, respectively, according to Eq. (4) for low pressures and Eq. (5) for high pressures:

where the pressure is low, i.e. ${d}_{\mathrm{T}}{\mathit{\lambda}}_{\mathrm{ion}}^{-\mathrm{1}}$ is small, *λ*_{+} and *λ*_{−} are the mean free paths of the
positive and negative ions, respectively, and *λ*_{ion} is the mean free path of one ion.

where the pressure is high, i.e. ${d}_{\mathrm{T}}{\mathit{\lambda}}_{\mathrm{ion}}^{-\mathrm{1}}$ is large. From these equations, Thomson (1924) deduced that the recombination
coefficient is proportional to the pressure for low pressures (because of
the sum of the reciprocal mean free paths of the ions), whereas it is
independent of the pressure for high pressures. This was supported by the
measurements of Thirkill (1913) who found *α* to be proportional to
the pressure throughout the measurement range of approximately 200–1000 hPa. Thus, the pressure regime of 1013 hPa and below is included in the low-pressure scenario. The transition pressure from the low-pressure to the high-pressure regime is clearly above 1013 hPa, and thus beyond the concern of atmospheric application. The temperature dependence is given as *α* ∼ *T*^{−2.5} for low pressures and *α* ∼ *T*^{−1.5} for high pressures because
*d* ∼ *T*^{−1} and
${v}_{+,-}$ ∼ *T*^{0.5} (Thomson, 1924). Hence, the recombination
coefficient decreases with rising temperature for pressures below 1013 hPa.
For the troposphere, this leads to a somewhat counterbalancing effect on
*α* for increasing altitudes when both the temperature and pressure drop simultaneously.

Another approach to explain the recombination of ions was introduced by
Langevin (1903a, b) whose ansatz is based on the speeds of ions in an
electrical field, as opposed to the later thermodynamic approach of Thomson.
To account for the effectiveness of collisions of a negative and positive
ion with regard to recombination, Langevin introduced the ratio of
successful recombinations per collision, *ε*_{L}, which is
included in the formula that he proposed to determine *α* (Eq. 6);
this probability is of empirical nature and was not further defined by a
formula:

where *μ*_{+} and *μ*_{−} are the ion mobilities of the positive
and negative ions, respectively, defined by Eq. (7a) and (7b):

where *E* is the external electrical field and *e*(4*π**ε*_{0}*r*^{2})^{−1} is the electrical field produced by the ions. Here,
*r* is the distance between the two ions of opposite charge (Langevin, 1903a).
The consideration of the recombination efficiency leads to an adapted term
for the recombination sink (Langevin, 1903a) shown in Eq. (8):

Langevin (1903b) further determined the pressure (*p*) dependence of
*ε*_{L} (and thus of *α*). For 1013 hPa, *ε*_{L} = 0.27 and *ε*_{L} ∼ *p*^{2} (and thus *α* ∼ *p*^{2}) for pressures below 1013 hPa. However, this is in contrast to Thomson (1924) who stated that *α* ∼ *p* for low pressures. Loeb and his colleagues later argued
that the assumptions made by Langevin to calculate *ε*_{L} are based on incorrect, sometimes even antithetical assumptions. They even
stated that this correction factor was only introduced to make the
experimental results fit the theoretical ones. The application of the Langevin theory is only considered valid for very high pressures (above approximately 10 atm) (Loeb and Marshall, 1929; Gardner, 1938; Loeb, 1960) and is therefore not within the focus of this work.

Loeb and Marshall (1929) further advanced and refined the Thomson theory; they introduced a probability term, similar to Langevin, for collisions leading to recombination, extending Eq. (5) to a more refined Eq. (9):

In subsequent works, the ratio of the doubled collision sphere radius and
the mean free path of the ion, 2${d}_{\mathrm{T}}\cdot {\mathit{\lambda}}_{\mathrm{ion}}^{-\mathrm{1}}$, is often denoted as *x*. With a number of assumptions and simplifications, and together
with validation from experimental work, Gardner (1938) summarised the
previous findings and advanced them to a set of equations (Eqs. 10–13)
that contain macroscopic quantities that are more accessible for direct
observation:

where

and

where *T*_{0} is the temperature at standard conditions (i.e. 273.15 K),
*m*_{ion} is the ion mass in Da, *ε*_{T} is the recombination
probability upon collision, *p*_{0} is the pressure at standard conditions
(i.e. 1013.25 hPa), *λ*_{air} is the mean free path of the
surrounding air, and the ratio ${\mathit{\lambda}}_{\mathrm{air}}\cdot {\mathit{\lambda}}_{\mathrm{ion}}^{-\mathrm{1}}$ = 5. Here, *x* is no longer defined by the ratio of *d*_{T} and *λ*_{ion}, but as a function of *T*, *p*, and the ratio ${\mathit{\lambda}}_{\mathrm{air}}\cdot {\mathit{\lambda}}_{\mathrm{ion}}^{-\mathrm{1}}$, and hence denoted as *x*^{′}. Importantly, Loeb and Marshall (1929) also discuss the
limitations of their approach. Firstly, the exact masses of the ions are
unknown since clustered ions and ions from impurities in the sample gas can
also occur. This has a non-negligible effect on the value of the
recombination coefficient. They argue that this circumstance could be the
reason for the variation of results among different authors. Apart from
the difference in ion mass, the property of free electron pairs in the
surrounding gas may also influence the recombination (Loeb and Marshall,
1929). Secondly, based on the observation that the measured *α* value is much smaller than the calculated one at low temperatures, they
discuss whether the presumed power of −1.5 for the *T* dependence might be
inaccurate.

A detailed overview of the different theories and their experimental
validations can be found in Loeb (1960) (second edition of Loeb, 1955)
where he discusses ion–electron and ion–ion recombination. For the latter,
cases of *α*, particle- or X-ray-induced ion production that feature a non-uniform spatial ion distribution are also described. Until the
beginning of the 1980s, it was hypothesised that, in general, ions are not
uniformly distributed in the atmosphere because the ions are produced along
the GCR paths and diffusion may not be sufficiently fast. Bates (1982)
showed that ions are mixed fast enough in the atmosphere so that the assumption of a uniform ion concentration of the “volume recombination” theories, described in the following discussion, is valid. Table 1 provides a selection of recombination theories discussed in detail by Loeb (1960).
Above atmospheric pressure, the Langevin theory is applied. Loeb subclassifies it, firstly, to the range of 20–100 atm, where there is no diffusional approach of the ions towards each other because they are already within the Coulomb attractive radius *d*_{T} and, secondly, to the range of 2–20 atm (called the Langevin–Harper theory), where the initial distance of the ions *r*_{0} is greater than *d*_{T}; hence they first have to diffuse towards each other. The subsequent collision inside *d*_{T} is almost certain because of
the high pressure. For the pressure range of 0.01–1013 hPa, i.e. for the
lower and middle atmosphere, the Thomson theory is applicable. Here, the initial distance of the ions is greater than *d*_{T} and the mean free path *λ*_{ion}; therefore, a random diffusive approach is necessary. Within *d*_{T}, the collision probability *ε*_{T} is less than
1. Below 0.01 hPa, i.e. in the ionosphere, the collision probability becomes
almost 0, and thus the collision is governed by the collision cross
section. For super-atmospheric pressures (i.e. in the Langevin regime),
*α* is dependent on *p*^{−1} and proportional to *T*. In the regime where the Thomson theory should be applicable (i.e. from 0.01 to 1013 hPa),
*α* is dependent on *T*^{−1.5}. The pressure dependence of *α* is
different in various Thomsonian theories; while Thomson (1924) stated a
proportional dependence (see Eq. 4), it varies in the parameterisations of
Gardner (1938), Israël (1957), and Loeb (1960) (see Eqs. 10, 14,
15, respectively, with Eqs. 11–13): for approximately 500–1000 hPa, *α* is dependent on *p*^{0.5} and below 500 hPa, it
approaches *p*^{1}. In the cross-section regime (i.e. < 0.01 hPa),
*α* is independent of the pressure and dependent on *T*^{−0.5}.

A detailed derivation of all theories and the above-mentioned equations is
given in Loeb (1960). In his work, the only variation in the Thomson
parameterisation for *α* from the one presented by Gardner (1938) is
the first factor in the formula for the recombination coefficient, as shown
in Eq. (14):

Israël (1957) further altered this parameterisation by including the
few experimental data available at that time into his parameterisation. In
the derivation of the formula, he used the value of 1.6 × 10^{−6} cm^{3} s^{−1} for *α* for “normal conditions”. However, he neither included a reference for this nor specified the normal conditions. These were probably 273.15 K and 1013.25 hPa. Furthermore, he stated that the recombination of small negative and small positive ions are accompanied by the recombination of small and big ions as well as small ions with neutrals, so that a whole equation system of recombination rates would result. He proposed the slightly altered parameterisation of the small-ion recombination that no longer includes the ion mass according to Eq. (15):

Contrary to previous authors, Israël used the value ${\mathit{\lambda}}_{\mathrm{air}}\cdot {\mathit{\lambda}}_{\mathrm{ion}}^{-\mathrm{1}}$ ≈ 3 for air; Gardner (1938)
and Loeb (1960) used the value of 5. Note that in Israël's work, there
is a typing error in the formula of *ε*_{T}: instead of
${\mathit{\epsilon}}_{\mathrm{T}}=\mathrm{1}-\frac{\mathrm{4}}{{{x}^{\prime}}^{\mathrm{4}}}\cdot [\mathrm{1}-{e}^{-{x}^{\prime}}\cdot ({x}^{\prime}+\mathrm{1}){]}^{\mathrm{2}}$, the fraction in front of
the brackets was erroneously given as $\frac{\mathrm{4}}{{{x}^{\prime}}^{\mathrm{2}}}$.

Natanson (1959a) (English translation of the original in Russian: Natanson, 1959b) developed a theory to unify Thomson's (low pressure) and Langevin's (high pressure) approaches; this formula is given in Eq. (16), assuming two ions of identical mass:

with

and

where *d*_{N} is the ion–ion trapping distance, *v*_{rel} is the mean relative thermal speed of the ions, *ε*_{N} is the probability that one ion collides with a gas molecule while the other ion is at a distance < *d*_{N} (also named “absorption coefficient”), *D* is the diffusion coefficient, and *m*_{red} is the reduced mass in kg. Note that the use of *x*_{N} depends on Natanson's *d*_{N} in Eq. (20), which is otherwise
identical to Eq. (12); *D* is the sum of *D*_{+} and *D*_{−}, the diffusion
coefficients of the positive and negative ion, respectively. Tamadate et al. (2020b) suggested exchanging ${v}_{\mathrm{rel}}\cdot {D}^{-\mathrm{1}}$ with the reciprocal of the ion–ion mean free path, *λ*^{−1}, in the first fraction of the denominator in Eq. (16), based on the definition of *λ* in Eq. (22):

where *D*_{+} and *D*_{−} are calculated according to Eq. (23a) and (23b),
respectively:

and

with

where ${D}_{+,\mathrm{0}}$ and ${D}_{-,\mathrm{0}}$ are the reference diffusivities calculated from
the reference ion mobility at standard pressure (*p*_{0} = 1013.25 hPa) and standard temperature (*T*_{0} = 273.15 K), *μ*_{0}, given by
López-Yglesias and Flagan (2013) as *μ*_{0} = 1.35 × 10^{−4} m^{2} V^{−1} s^{−1}
for the ion mass of 90 Da. The temperature dependence of 1.75 for
${D}_{+,-}$ is taken from Tang et al. (2014). Note that López-Yglesias and
Flagan (2013) use *T*^{2} and the Chapman–Enskog theory predicts *T*^{1.5}
(Chapman and Cowling, 1960).

In the course of time, additional sinks for atmospheric ions, other than the
ion–ion recombination process, have been discussed. Lenz (1932) explained
the strong deviations observed between several experimentally derived values
for *α* by the authors' negligence of losses due to their experimental
setups, for example, by wall losses. In addition, the attachment of ions to
aerosol particles suspended in the surrounding gas has been found to cause
problems in the quantification of *α*, especially in field studies
performed in the atmosphere (Rosen and Hofmann, 1981; Morita, 1983), while
Franchin et al. (2015), who conducted chamber experiments, included the
aerosol sink and wall losses to their calculations. Furthermore, one has to
bear in mind that the capabilities of the instruments and the purity of the
gases were less advanced before the 1950s (Loeb, 1960). Therefore, results
obtained before that time need to be considered with caution. Nevertheless,
the theory of ion–ion recombination experienced more advances in the
following decades as discussed in the next sections.

In the previous section, the theories and parameterisations that concern the
total ion–ion recombination, i.e. the combination of binary and ternary
processes, were discussed. Commencing in the late 1970s, several groups
examined the binary and ternary processes, respectively, in more detail.
Hickman (1979) developed an approach to determine the binary recombination
coefficient, *α*_{2}. Based on a complex potential model, the
neutralisation of two ions of opposite sign is determined by an electron
transfer from the negative to the positive ion. While the two ions approach
one other, the electron transfer can occur when the potential curve of the
initial state crosses at least one of the potential curves of the final
states. In the semi-empirical Eq. (25), *α*_{2} depends on the
temperature *T*, the reduced mass *m*_{red}, and the electron affinity EA of the negative ion, i.e. its electron detachment energy:

where *m*_{red} is in Da and EA is in eV. Due to the mass and electron affinity dependencies, the recombination coefficient can vary by 1 order of
magnitude or more, e.g. from (49 ± 20) × 10^{−8} cm^{3} s^{−1} for NO^{+} + O^{−} to (4.1 ± 0.4) × 10^{−8} cm^{3} s^{−1} for CClF${}_{\mathrm{2}}^{+}$ + Cl^{−} (Hickman, 1979). The temperature dependence is *T*^{−0.5}; the mass dependence of ${m}_{\mathrm{red}}^{-\mathrm{0.5}}$ is in accordance to Gardner (1938) and Loeb (1960). The dependence on the electron affinity is unique compared to the other approaches.

Several experiments were performed to test this deduction. A recent approach
was reported by Miller et al. (2012), who used the variable electron and
neutral density attachment mass spectrometry (VENDAMS) method, utilising a
flowing afterglow/Langmuir probe (FALP) apparatus. This method is limited to
atomic cations from noble gases. Miller et al. (2012) determined the rate
coefficients of neutralisation reactions of several anions, among them
SF${}_{\mathrm{4}\text{\u2013}\mathrm{6}}^{-}$, NO${}_{\mathrm{3}}^{-}$, and Br${}_{\mathrm{2}}^{-}$, with Ar^{+} and
Kr^{+} at conditions of 300–550 K and a helium buffer gas number
concentration of typically 3.2 × 10^{16} cm^{−3} (i.e. 1.3 hPa at 300 K). They also summarised previous works. The resulting binary ion–ion recombination coefficients were found to be in the range of 2.5–5.6 × 10^{−8} cm^{3} s^{−1} at 300 K, showing decreasing values for higher temperatures, with a typical uncertainty of
5 × 10^{−9} cm^{3} s^{−1} (Miller et al., 2012). Shuman et al. (2014b) later pointed out that the rate coefficients involving Ar^{+} should be increased uniformly by 4 × 10^{−9} cm^{3} s^{−1}. Miller et al. (2012) fitted the data to the parameterisation developed by Hickman (1979), resulting in adapted exponents for *T*, *m*_{red}, and EA, as shown in Eqs. (26) and (27):

for diatomic anions and

for polyatomic anions.

Later, the mutual neutralisation reactions of di- and polyatomic cations
with the halide anions Cl^{−}, I^{−}, and Br^{−} were also studied
(Shuman et al., 2014a). The cations were produced by transferring the charge
from Ar^{+} to neutral species such as O_{2}, NO, or CF_{4}. It was
found that the binary ion–ion recombination coefficients are primarily
governed by the chemical nature of the system (i.e. the locations of the
curve crossings) for systems with the recombination of two monoatomic ions, while the physical nature of the system (e.g. the relative velocity of the ions) becomes dominant for systems with more than four or five atoms. For the latter, a good description of the rate constants is given by
2.7 × 10${}^{-\mathrm{7}}{m}_{\mathrm{red}}^{-\mathrm{0.5}}(T/\mathrm{300}{)}^{-\mathrm{0.9}}$ (Shuman et al., 2014a),
thus agreeing with the previous findings given in Eq. (27). In addition,
experiments with heavier molecular ions such as C_{10}H${}_{\mathrm{8}}^{+}$,
WF${}_{\mathrm{5}}^{+}$, and C_{6}F${}_{\mathrm{11}}^{+}$ support these findings (Wiens et
al., 2015).

While most research in the field has been carried out on the recombination
process itself, some works have also been devoted to study the product
formation. For instance, Shuman et al. (2010) investigated the different
product channels of the recombination of SF${}_{\mathrm{4}\text{\u2013}\mathrm{6}}^{-}$ with Ar^{+}. Besides simple electron transfer reactions, the elimination of F atoms was also observed.

Subsequently, further parameterisations of the total ion–ion recombination coefficient based on laboratory experiments and field measurements in the troposphere and stratosphere were developed, as will be discussed in the next section.

In the late 1970s, Smith and Church (1977) investigated the different
influences of binary and ternary collisions on the recombination
coefficient. They determined the recombination rates of NO^{+} and
NO${}_{\mathrm{2}}^{-}$ in an experimental setup for different temperatures and
pressures typical for the atmosphere and inferred the binary (*α*_{2}) and ternary (*α*_{3}) recombination rates for different
altitudes using helium as the carrier gas. They found that above 30 km,
where air is less dense, the binary recombination is dominant, while below
30 km, where air is denser and three-body collisions are more likely, the
ternary recombination is more important. For ground level, they determined a
rather high value of *α*_{3} = 3 × 10^{−6} cm^{3} s^{−1}. Interestingly, the total ion–ion recombination rate is almost constant throughout the whole troposphere according to their work. The value only decreases above 10 km, until an altitude of about 50 km. With regard to the temperature, they determined a dependency of *T*^{−0.4} from their data for the binary recombination. For the ternary recombination, they expected a dependency of *T*^{−2.5} to *T*^{−3}, while Fisk et al. (1967) even determined *T*^{−4.1} in a recombination experiment with Tl_{2}I^{+} and TlI${}_{\mathrm{2}}^{-}$. Smith and Church (1977) have inferred an equation for the binary recombination from further experiments (Eq. 28), which was later adapted by Bates (1982) (Eq. 29):

and

Furthermore, Smith and Adams (1982) presented a parameterisation valid for the altitude range of 10–60 km based on the laboratory measurements of binary recombination with the FALP technique. The resulting parameterisation is simple because it only depends on the altitude and contains two terms that represent the ternary and binary recombination, respectively, as Eq. (30) shows:

where *h* is the altitude in km. Johnsen et al. (1994) later disputed their results because they found that the ion-collecting probes, as used by Smith and Adams, are not suitable to obtain data on ion–ion recombination
coefficients in flowing-afterglow studies.

Bates (1982) criticised that the binary and ternary recombination rates had
been erroneously considered to be additive in previous works, stating that both processes are not independent of each other. Instead of the binary
recombination rate *α*_{2}, he defined the enhancement due to the
binary channel, Δ*α*_{2}, and calculated *α*_{3},
Δ*α*_{2}, and the resulting total recombination coefficient,
*α*, in a Monte Carlo (MC) simulation for altitudes between 0 and 40 km.
Interestingly, Smith, Church, Adams, and Bates have never cited the works of
Israël (1957) or Lenz (1932). It seems that the two latter authors have
been overlooked, probably because they published their works in German
(however, Israël's textbook was translated into English in 1971). This
is especially remarkable since Bates (1982) determined *α* to be
1.67 × 10^{−6} cm^{3} s^{−1} at ground level, which is in
striking agreement with Israël (1957) (1.6 × 10^{−6} cm^{3} s^{−1}) and Lenz (1932) ((1.7 ± 0.1) × 10^{−6} cm^{3} s^{−1}). Instead, Bates referred to Sayers (1938)
(2.3 × 10^{−6} cm^{3} s^{−1}) and Nolan (1943)
(1.4 × 10^{−6} cm^{3} s^{−1}), whom he regarded as the
first experimenters to quantitatively and accurately determine *α*.

At the start of the 1980s, science was in urgent need of correct and altitude-resolved values for the recombination coefficient. Arnold and Fabian (1980) presented a method to calculate the concentration of gaseous sulfuric acid from measured concentration ratios of the ambient HSO${}_{\mathrm{4}}^{-}$ and NO${}_{\mathrm{3}}^{-}$ ions. The recombination coefficient, which describes the sink for ions, forms part of the formula (see Arnold and Qiu, 1984, for a more detailed derivation). Until the early 1980s, this method was the only way to determine the concentration of trace gases, such as sulfuric or nitric acid, in the different layers of the atmosphere.

The need for an experimental investigation in the atmosphere was answered by
Gringel et al. (1978), Rosen and Hofmann (1981), and Morita (1983). Gringel
et al. (1978) conducted balloon-borne measurements of the air conductivity
between 4 and 25 km over northern Germany in August and October 1976. From
the measured air conductivity, *σ*, the calculated altitude-corrected
ion mobility, *μ*, and the mean of formerly measured ionisation rates, they
determined the ion–ion recombination coefficients for different altitudes
according to Eqs. (31) and (32):

where

with *μ*_{0} = 1.3 × 10^{−4} m^{2} V^{−1} s^{−1}. The altitude-resolved values for *q* are the means of three independent
measurements between the 1930s and the 1970s, although *q* varies with the
11-year solar cycle which casts doubt on the validity of the values in the
calculations.

On the other hand, both Rosen and Hofmann (1981) and Morita (1983) measured
the positive ion number concentration *n*_{+} directly along with the
ionisation rate *q* in a concerted measurement campaign. Thus, Rosen and
Hofmann's data, being available earlier than Morita's, were considered to be
the most reliable data at that time because they measured the relevant
parameters simultaneously (Arijs, 1983). Applying Eq. (2), they calculated
*α* for different altitude levels. Additionally, for altitudes above
32 km, they used the alternative method given in Eq. (31) to calculate
*α*. The derived data points followed a profile suggested by a theory
that accounted for both binary and ternary recombination. The data points
derived with Eq. (31) fit the theoretical predictions better. However, below
9 km, the derived values for the ion–ion recombination were unexpectedly
large. As the authors themselves wrote, in the troposphere, the losses of
ions due to aerosol particle attachment have to be taken into account,
otherwise the loss due to ion–ion recombination is overestimated when using
Eq. (2); this is why only the values above 9 km are reliable. Nevertheless,
these measurements have led to further adjustments of the parameterisations,
such as the ones by Arijs et al. (1983) and Brasseur and Chatel (1983).
Arijs et al. (1983) presented a formula that contains two terms, accounting
for binary and ternary reactions, as shown in Eq. (33):

where [M] is the number density of air molecules in cm^{−3} (representing
the pressure dependence), given by Eq. (34):

Independently, Brasseur and Chatel (1983) proposed a very similar formula that only differs in the factor of the ternary recombination term (Eq. 35):

Due to the *T*^{−1} dependence of [M], the ternary recombination coefficient ultimately shows a *T*^{−5} dependence in Arijs et al. (1983) and Brasseur and Chatel (1983), which is even stronger than previously discussed. The temperature dependence of *T*^{−0.5} in the binary term is in agreement with Hickman (1979) (but not with the more recent parameterisation of Miller et al. (2012) that describes a *T*^{−0.9} dependence). The pressure dependence of *α* is *p*^{1} in the ternary terms in Eqs. (33) and (35) through the linear *p* dependence of [M] (see Eq. 34). A proportional pressure dependence is also observed in some Thomsonian theories (see Sect. 2).

Parallel to Rosen and Hofmann, Morita (1983) conducted atmospheric field measurements and also found reasonable results for altitudes above 6 km; however, for the above-mentioned reason, strong disagreement of the observed results from the theoretically expected ones below 6 km was found. Bates (1985) synthesised his earlier model results (see Sect. 6) and the measurements by Morita to define another parameterisation that is merely dependent on the altitude, as shown in Eq. (36):

which is valid for the range of 10–25 km. Below 10 km, *α* is
expected to be constant at 1.7 × 10^{−6} cm^{3} s^{−1}.

More recently, Franchin et al. (2015) reported experimental data for the
recombination coefficient for atmospheric conditions. They have examined the
dependency of *α* on the temperature, relative humidity (RH), and the
number concentrations of sulfur dioxide [SO_{2}] and ozone [O_{3}]
in a series of chamber experiments. Their experimental setup did not allow
for pressures below 1013 hPa, therefore, it is not directly possible to
derive new insights with regard to processes in the upper troposphere or
stratosphere. However, they did show that *α* is dependent on RH; with
increasing RH, the recombination coefficient decreases. At
70 % RH, *α* is 2.0 × 10^{−6} cm^{3} s^{−1}, which is within the known range of uncertainty; however, for 7 % RH, it is as high as 8.1 × 10^{−6} cm^{3} s^{−1} (both at 293.15 K). They convincingly explain this by an increase in ion sizes with increasing RH. With
a higher humidity, more water ligands are added to the ion cluster, and
thus its size and mass increase while its mobility decreases. This effect
could not be reproduced quantitatively by any theory (Franchin et al.,
2015). Their data also revealed the temperature dependence of *α*: at
293.15 K, the value was (2.3 ± 0.7) × 10^{−6} cm^{3} s^{−1} and, at 218.15 K, it was (9.7 ± 1.2) × 10^{−6} cm^{3} s^{−1} (both at 40 % RH).
Unfortunately, the standard deviations of the data points are large, thus
any temperature dependence derived from the four data tuples is inaccurate
in itself. Nevertheless, we derived a temperature dependence of *T*^{−3} from
their data. This is in a similar order of magnitude to the findings of Smith
and Church (1977) (*T*^{−2.5} to *T*^{−3}) and is still comparable to Arijs et al. (1983) and Brasseur and Chatel (1983) (both teams: *T*^{−5}) for the
ternary recombination, considering that ternary recombination is the
predominant process at atmospheric pressure. Besides this, the recombination
coefficient was found to be independent of [O_{3}] and [SO_{2}].

After 1985, no further improvements of the parameterisation for direct
application in the atmosphere have been made. One reason could be that the
need for this value has become less urgent, since, from that year, trace
gases could be measured directly in their neutral forms (Arnold and Hauck,
1985). In addition, most of the parameterisations were in good accordance
for the altitude range of 10–40 km (Arijs, 1983) so that no further
improvement appeared to be necessary. As yet, for the troposphere,
experimental validation of the parameterisations remains open until this
day. The best estimate available is the assumption that *α* remains
constant between 0 and 10 km due to the cancellation of the opposing
temperature and pressure effects. However, theories concerning the
ion–aerosol attachment have been further developed. The most important
theories and their applicability to the ion–ion recombination will be
discussed in the next section.

Apart from ion–ion recombination, the analogous process of ion–aerosol
attachment was further studied as well. For instance, Natanson (1960a) (English translation of the original in Russian: Natanson, 1960b) expanded his approach to the attachment of ions to particles. In general, the ion–ion recombination can be considered as a special case of the ion–aerosol attachment, i.e. when the radius of the aerosol particle is reduced to ionic sizes. While in many ion–ion recombination theories, the concept of the
three-body collision radius, or trapping radius, *d*, can be found, many
ion–aerosol theories additionally use the concept of the limiting sphere,
*δ*. The limiting sphere and its radius are defined slightly
differently depending on the theory. With Fuchs (1963), it is defined as a
concentric sphere around the particle with the radius *δ*_{F} = ${r}_{\mathrm{p}}+{\mathit{\lambda}}^{\prime}$, where *r*_{p} is the particle radius and *λ*^{′} is “the mean distance from the surface of the particle at which the ions collide for the last time with gas molecules before striking this surface” (Fuchs, 1963). Notably, *λ*^{′} is not equal to the mean free path of one ion, *λ*_{ion}, or the ion–ion mean free path, *λ*. Hoppel and Frick (1986) define it as the sum of the ion–aerosol three-body trapping sphere and the ion–ion mean free path (see Eq. 44). Transferred to the ion–ion recombination, the limiting sphere can be defined as the sum of the ion–ion three-body trapping distance and one mean free path (see Eq. 45), as depicted in Fig. 1.

In Fig. 1a, an ion (white circle) approaches the ion in the centre (black circle) which has the opposite charge. The approaching ion experiences its last collision with a neutral gas molecule approximately one mean free path away from the trapping sphere (i.e. on the surface of the limiting sphere according to Hoppel and Frick's definition). When entering the limiting sphere, the white ion collides with another neutral gas molecule on the surface of the trapping sphere. This process is also called three-body trapping, because the gas molecule, which is the third body, “traps” the white ion inside the trapping sphere of the centre ion. However, not all of these collisions lead to the recombination of the two ions. The probability for an ion to collide with a neutral gas molecule is accounted for in many theories. Two possible outcomes of the third-body collision are shown as cases 1 (collision) and 2 (non-collision) in Fig. 1b.

Tamadate et al. (2020b) provided a comprehensive review of those theories and their application to the ion–ion recombination in the introductory part of their work. For the sake of completeness and to identify the potential of these approaches for their application to the lower atmosphere, the most important concepts and formulae are given in the following paragraphs.

In Fuchs's theory, outside the limiting sphere, continuum equations are
used, whereas inside the sphere, kinetic theory is applied because
steady-state, rather than equilibrium conditions, are valid (Fuchs, 1963;
Hoppel and Frick, 1986). Coulomb as well as image forces are taken into
account in this theory, but no third-body processes. The radius *δ*_{F} of the limiting sphere is given in Eq. (37) (Fuchs, 1963), based on considerations by Wright (1960):

where *r*_{coll} is the collision radius, which is the sum of both ion radii (originally, the particle radius *r*_{p}).

Although Fuchs (1963) did not provide a formula for *α* himself,
Tamadate et al. (2020b) have used Fuchs's approach to derive the ion–ion
recombination coefficient, shown in Eqs. (38) to (40):

where

and

where *α*_{δ} is the ion–ion collision rate coefficient at the
limiting sphere surface.

However, there are two main problems with the theory of Fuchs (1963).
Firstly, it ignores the three-body trapping, i.e. collisions of the two ions
(or the ion and the particle) with neutral gas molecules (Hoppel and Frick,
1986; Tamadate et al., 2020b). Hoppel and Frick (1986) showed that Fuchs's
theory would lead to an ever-growing underestimation of the attachment
coefficient for decreasing particle radii (e.g. 4.4 × 10^{−7} cm^{3} s^{−1} for a 1 nm radius) due to the negligence of the three-body trapping. Three-body trapping becomes increasingly more relevant for aerosol particles approaching ionic sizes (or when two ions recombine) and when the pressure is relatively high, as is the case in the lower atmosphere. Secondly, an ion entering the limiting sphere of another ion with the opposite sign does not follow the thermal equilibrium distribution; instead, the equilibrium ion drift velocity, *v* = *μ**E*, in the direction of the ion in the centre of the limiting sphere needs to be considered (Gopalakrishnan and Hogan, 2012; Tamadate et al., 2020b).

Similarly, Tamadate et al. (2020b) derived *α* using the theory of
Filippov (1993), who had examined the ionic charging of small aerosol
particles with respect to the Knudsen number, which was also based on the
considerations of Fuchs (1963). Tamadate et al. (2020b) presented Eq. (41)
that defines the ion–ion recombination coefficient and which already
includes the collision probability for ions entering the limiting sphere,
*ε*_{δ}, and is independent of *α*_{δ}:

with

and

where Ψ_{δ} is the ratio of Coulomb and thermal energy at the
limiting sphere surface and *Kn*_{δ} is the Knudsen number for the limiting sphere. To obtain *ε*_{δ}, Tamadate et al. (2020b) performed molecular dynamics (MD) simulations that will be described in the next section.

Subsequent to Fuchs, Hoppel and Frick (1986) developed a theory for ion–aerosol attachment based on Natanson (1960a), Keefe et al. (1968), and Hoppel (1977) that uses the limiting sphere approach and includes image forces and three-body trapping.

Hoppel and Frick (1986) defined limiting sphere radii for both effects as
well as for their combination, which indicate the maximum distance for which
the ions would recombine with a particle given the respective effect(s).
Since the collisions with a third body (i.e. a gas molecule) only occur with
a certain probability within the limiting sphere, this probability needs to
be taken into account in a similar way as in the Thomson theory. Hoppel and
Frick (1986) show that image forces are not relevant for the case of ion–ion
recombination or for ion–particle attachment when the particle diameter is
small (< 40 nm). For this condition, they define the limiting sphere
radius, *δ*_{HF}, as the sum of the ion–aerosol three-body trapping distance, *d*_{ia}, and the ion–ion mean free path according to Eq. (44):

The value for the attachment coefficient of a singly charged particle
smaller than 2 nm in radius and an ion of opposite sign reported by Hoppel
and Frick (1986) approaches 1.3 × 10^{−6} cm^{3} s^{−1},
and thus approaches the ion–ion recombination coefficient itself. Therefore, by applying Eq. (44) to ion–ion recombination, one can derive Eq. (45) where
the ion–aerosol trapping sphere *d*_{ia} is replaced by the ion–ion trapping sphere *d*_{HF} (see also Tamadate et al., 2020b):

In the following discussion we want to briefly outline how the Hoppel and Frick method is used to determine the ion–aerosol attachment coefficients. Their method does not provide any means of accurately calculating the ion–aerosol trapping distance from theory. Therefore, they adopt the theory by Natanson (1959a) to derive the ion–ion trapping distance from a measured ion–ion recombination coefficient and certain ion properties (they take the value of
*α* = 1.4 × 10^{−6} cm^{3} s^{−1} from Nolan, 1943). The
value of the ion–ion trapping sphere distance can then be used to calculate
the ion–aerosol trapping sphere distance. Since the method by Hoppel and
Frick (1986) was explicitly developed to determine ion–aerosol attachment
coefficients, it is not directly suitable to determine ion–ion recombination
coefficients. One important application for the Hoppel and Frick theory is
the calculation of equilibrium charge distribution of aerosols as a function of
the particle diameter. The knowledge of the charged fractions (as a function
of diameter and the number of elementary charges) are important for aerosol
size distribution measurements with differential mobility analysers after
the aerosol is “neutralised” by passing a strong ion source with high
concentrations of bipolar ions (e.g. Wang and Flagan, 1990). The fact that
the method by Hoppel and Frick (1986) does not include any means of
calculating the ion–aerosol or the ion–ion trapping distance directly was
also discussed by Tamadate et al. (2020b). They highlight that the effect of
changing pressure and temperature on the trapping distance is not taken into
account. Nevertheless, López-Yglesias and Flagan (2013) have improved
some approximations made by Hoppel and Frick (1986) and developed a model to
calculate the ion–aerosol attachment for aerosol particles of different
sizes and charges. The amendment of using Maxwellian speed distributions for
the ion and the colliding gas molecule instead of fixed average speeds led
to the most significant of the deviations from Hoppel and Frick's model.

Tamadate et al. (2020b) provided a set of formulae in order to calculate the
ion–ion recombination rate after Hoppel and Frick, also using Eq. (38).
However, the ion–ion collision rate coefficient *α*_{δ} at
distance *δ* is defined differently for Hoppel and Frick, and is
given in Eq. (46). Here, the ion–ion collision rate *α*_{δ} is
not directly dependent on the collision radius *r*_{coll} (cf. Eq. 39), but on the ion–ion trapping distance *d*_{HF}. Furthermore, the additional probability factor for ions entering the trapping sphere, *ε*_{d}, is introduced to the ion–ion collision rate:

with

and

where *θ* is the critical angle to enter the trapping sphere and *b* is
the critical collision parameter (Tamadate et al., 2020b). Again, to obtain
a value for *α*, one needs to know the given trapping sphere radius,
*d*_{HF}. However, to determine *d*_{HF}, Hoppel and Frick used a known ion–ion recombination coefficient. This circular logic arises because we divert their theory that is meant to determine ion–aerosol attachment processes to ion–ion recombination processes. Nevertheless, it can be tested to calculate *α* for different altitudes of the atmosphere by keeping a constant value for *d*_{HF} while varying *T* and *p*.

Tamadate et al. (2020b) highlight the fact that there is no single calculation approach that yields accurate ion–ion recombination rates for a wide range
of pressures, temperatures, gas compositions, and ion chemical compositions.
This deficiency motivated their development of a so-called hybrid
continuum–MD approach. This method couples the limiting
sphere method, when the two ions are sufficiently far apart from each other
and their motion is controlled by diffusion, with MD simulations that model
the ion motions within a critical distance *δ*. The calculations are
applied to a system where NH${}_{\mathrm{4}}^{+}$ and NO${}_{\mathrm{2}}^{-}$ ions recombine
in helium at 300 K under varying pressure. Collisions between the ions and
neutral gas molecules are taken into account. Excellent agreement is found
when the model results are compared with the laboratory measurements at two
different pressures (Lee and Johnsen, 1989). The equation for calculating
the ion–ion recombination coefficient (Eq. 41) is derived from Filippov (1993). For their test case, Tamadate et al. (2020b) show that the limiting sphere distance suggested by Fuchs (1963) (*δ*_{F}, see Eq. 37)
can be used as the initial distance between the two ions when the MD
simulations commence. For larger distances, the calculated recombination
rates do not change, demonstrating that the proposed method is
independent of the choice of the limiting sphere radius, as long as it is
sufficiently large. The quantity that is determined by the simulations is
the probability, *ε*_{δ}, that a successful collision
occurs when the initial speeds of the ions in 3D are drawn from probability
density functions based on Boltzmann distributions. A collision is defined
as being successful if the distance between the two ions gets smaller than a
threshold value, whereas it is not successful if the distance eventually
exceeds *δ*_{F}. Especially for low pressures (and correspondingly
large *δ*_{F}), *ε*_{δ} can become very small,
hence it requires many simulations for achieving results with small
statistical errors. The MD simulations require, in addition, Lennard-Jones
parameters and partial charges on atoms as input variables. In a separate
publication, Tamadate et al. (2020a) apply their continuum–MD approach to a
system where positively charged polyethylene glycol ions (1 to 7 charges,
mass of 4600 Da) recombine with NO${}_{\mathrm{2}}^{-}$ ions in nitrogen. The
comparison between the experimentally determined recombination rates and the
calculated ones indicates that they agree within a factor of 2. These
results show that the hybrid continuum–MD approach is well suited to yield
accurate ion–ion recombination rates for a wide range of applications and
conditions, including studies of the different layers of the atmosphere.

Numerical simulations using MC methods have been another
powerful tool for gaining insights into ion–ion recombination or ion–particle
attachment rates and their dependencies on parameters such as gas pressure
and temperature. In contrast to the MD simulations, the ion–ion and the
ion–neutral interactions are generally much more simplified, e.g. the
collisions with neutral gas molecules are treated by the use of random
numbers for the collision frequencies, energies, and angles. In the majority
of cases, the collisions are treated as elastic, while spherical geometry is
assumed for the collision partners. The first MC calculations to include
three-body trapping were conducted by Feibelman (1965), who found good
agreement with a measured recombination rate. Later, MC simulations studied
the recombination in oxygen for varying pressure from zero pressure, i.e.
for the binary condition, up to approximately 1000 hPa where ternary
recombination is clearly dominant (Bates and Mendaš, 1978). The results
showed that the ion–ion recombination rates peak between 1000 and 2000 hPa,
as expected from theory. Besides the pressure dependence of the
recombination rate, Bardsley and Wadehra (1980) also studied the temperature
dependence using MC simulations. The results indicate a dependence stronger than *T*^{−3} for low pressures and a strongly reduced temperature
dependence for pressures above approximately 5000 hPa. Bates (1982) reported
ion–ion recombination rates calculated with an MC model for the atmospheric
conditions ranging between 0 and 40 km altitude, which agree well when compared to the values from the balloon measurements (see Sect. 7.1). Filippov (1993) developed an MC model for the charging of aerosol particles. The numerical results show fairly good agreement with the measured values in the range of 5 and 80 nm when using either air or helium as the neutral gas.

In Table 2, all theories, parameterisations, field and laboratory data sets, and model results discussed in the previous sections are listed for a better overview. In the following sections, they will be addressed by the abbreviations listed in Table 2. In order to determine the most suitable single formula to determine the ion–ion recombination coefficient for different altitudes, we compare the above-mentioned parameterisations and theories to the field, laboratory, and model data.

## 7.1 Comparison to field and model data

In a first step, the parameterisations and theories were compared to the
field and model data. The temperature, pressure and air density data of the
US Standard Atmosphere were used here (National Oceanic and Atmospheric
Administration et al., 1976). Furthermore, we used the parameters
*m*_{ion} = *m*_{+} = *m*_{−} = 90 Da, *μ*_{0} = 1.35 × 10^{−4} m^{2} V^{−1} s^{−1}
(López-Yglesias and Flagan, 2013), *d*_{HF} = 18 nm for HF86 (the proposed value of Hoppel and Frick (1986) for an ion of 90 Da, assuming an ion–ion recombination coefficient of 1.7 × 10^{−6} cm^{3} s^{−1}), and EA = 3.94 eV (Weaver et al., 1991). *r*_{coll} was calculated according to
Eq. (A1). The results are plotted in Fig. 2. Here, the *y* axes represent the
altitude *h* and the x axes represent the ion–ion recombination coefficient
*α*. In Fig. 2a to d, the field measurements Gr78, RH81, and Mo83
are shown for better comparability. Note that the data are inaccurate
below 10 km. For RH81, there are two data sets for altitudes above 32 km:
one is calculated based on Eq. (2), the other one is based on Eq. (31). One
should bear in mind that these data sets, which were determined with similar
methods, may also suffer from systematic errors such as losses inside the
instrument that were not accounted for; however, these remain the most
reliable data from field measurements available to this day. The challenge
for the theories and parameterisations is to accurately determine the
ion–ion recombination coefficient for the different regimes: the ternary
recombination regime between 0 and approximately 25 km, the transition
regime between 25 and approximately 40 km, and the binary recombination
regime above 40 km. Note that the binary theories (i.e. Fu63, Hi79, and
Mi12) are therefore only plotted above 40 km altitude.

In Fig. 2a, the Thomsonian theories (Ga38, Lo60, Is57, and Na59) are
depicted. In Fig. 2b, the semi-empirical adjustments to the Thomson
theory (Ar83 and BC83) as well as the MC simulation (Ba82) are shown
and in Fig. 2c, the binary complex potential models (Hi79 and Mi12) as well
as the solely altitude-dependent parameterisations (SA82 and Ba85) are
plotted. Figure 2d shows Fu63 and HF86, the ion–aerosol attachment
theories that are applied to the ion–ion recombination. Figure 2e
provides an overview of the most relevant theories and data sets for an
altitude range of up to 12 km with a linear *x* scale, whereas the other
subplots use a logarithmic *x* scale.

The Thomsonian theories (Ga38, Lo60, Is57, and Na59; see Fig. 2a and e)
all show a similar behaviour; from ground level up to 11 km (tropopause), the *α* value slightly increases, and above 11 km, it decreases more
strongly. Above 16 km, Ga38, Na59, and Lo60 yield almost the same values,
while Is57 yields lower values throughout the stratosphere. Close to the
ground, Ga38, Lo60, and Is57 predict *α* values identical or close to
1.7 × 10^{−6} cm^{3} s^{−1}, whereas it is slightly
elevated for Na59. Comparing these theories to the field data, Is57 shows a
striking agreement in the altitude range of 11–22 km. However, none of
the theories predict the slower decrease and asymptotic approach towards a
constant value due to the binary recombination predominating over the
ternary process. Apparently, the binary process is not sufficiently taken
into account in these theories, thus, their validity is limited to the
altitude range of 0–22 km. However, within this range, the
parameterisation of Is57 yields the most promising results.

The MC simulation Ba82 (see Fig. 2b and e) reproduces the
ground-level value of 1.7 × 10^{−6} cm^{3} s^{−1} and
yields almost constant values for 0, 5, and 10 km altitudes, while
decreasing above 10 km, reproducing the field data with remarkable
agreement. The semi-empirical parameterisations Ar83 and BC83 (see Fig. 2b and e) contain both a binary and a ternary recombination term and were
developed to reproduce the data set of RH81; BC83 does so between 11 and
approximately 20 km, while Ar83 reproduces the data set between
approximately 20 and 35 km. Moreover, BC83 predicts a ground-level value
of 1.9 × 10^{−6} cm^{3} s^{−1} for *α*, which is much
closer to the expected value than that of 3.8 × 10^{−6} cm^{3} s^{−1} by Ar83. Close to 50 km, both parameterisations
approach a similar value because their binary term is identical and becomes
increasingly more dominant at higher altitudes. The strong deviations,
especially in the troposphere, show that small changes in the prefactor of
the ternary term can have substantial effects on the resulting recombination
coefficient. For altitudes above 25 km, Ar83 can be chosen to parameterise
the ion–ion recombination coefficient because it reproduces the field data
sufficiently well. It is worth noting that BC83 and Ar83 both have a strong
temperature dependence of *T*^{−5}, while the Thomsonian theories have a much
weaker temperature dependence of *T*^{−1.5}, although they do still yield
similar results in the troposphere.

The solely altitude-dependent empirical parameterisations SA82 and Ba85 (see
Fig. 2c and e) are valid from 10 to 60 km and from 10 to 25 km,
respectively. The Ba85 parameterisation, indeed, reproduces the field data of RH81 well within
this range, while Sa82 overestimates the recombination coefficient below an
altitude of 30 km but fits the field data reasonably well between 32 and
45 km; this is because it features the slower decrease of *α* for
increasing altitudes above 30 km where the binary recombination process
predominates. Given their solely empirical nature and their limited validity
ranges, these two parameterisations appear to be useful in applications
where only information about the altitude is available but knowledge of
the temperature or pressure is lacking.

The two binary theories Hi79 and Mi12 (see Fig. 2c, only shown above 40 km altitude) yield lower recombination coefficients than the field data while still being in the same order of magnitude as SA82, Ar83, and BC83. However, as the data coverage is scarce above 35 km altitude, it is difficult to compare these theories to the field data and draw appropriate conclusions.

The two ion–aerosol attachment theories Fu63 and HF86 (see Fig. 2d and
e), when applied to the ion–ion recombination process, do not reproduce the
field measurements. While Fu63 only accounts for the binary recombination
process and is therefore only shown in the binary regime, i.e. above 40 km
altitude, it yields reasonable results with values for *α* that are
only slightly lower compared to the field data. On the other hand, HF86
yields results that are in the correct order of magnitude within the
troposphere; however, the *α* value of 2.9 × 10^{−6} cm^{3} s^{−1} at ground level is higher than expected. Within the stratosphere, one can observe the increasing dominance of the binary recombination process in HF86 with increasing altitude since the curve approaches a constant value, as seen in other theories discussed above. The recombination coefficient is in excellent agreement with the field data above 30 km altitude, however, it is underestimated between 15 and 25 km. One possible source for these inaccuracies could be the assumption of a constant value of 18 nm for the ion–ion trapping sphere radius *d*_{HF}; in other theories, this value is dependent on *T* and/or *p*. An altitude-dependent trapping distance may improve the performance of HF86 (see Sect. 8).

In summarising the intercomparison, it becomes obvious that there is no theory that can accurately reproduce the known ground-level
value for the recombination coefficient *α* as well as the field data
between 10 and 45 km altitude. Within the troposphere, it is reasonable to
assume that the recombination coefficient remains almost constant due to the
counterbalancing temperature and pressure effects. In the stratosphere, on
the other hand, it decreases, although the decline lessens in the upper
stratosphere, approaching an almost constant value at the top of the
stratosphere. For altitudes between 0 and 22 km, the Thomsonian
parameterisation Is57 most accurately reproduces the ground-level data and the field data. The semi-empirical parameterisation BC83 yields similar
results in this altitude range, although it misses the exact values
slightly. The Thomsonian theories and the semi-empirical parameterisations
show similar results to each other in the troposphere despite having very
different temperature dependencies in the ternary term. Between 10 and 25 km,
Ba85 reproduces the field data of RH81 accurately, however, its application is limited because it is only dependent on *h* and does not contain physical
information about the *p* and *T* dependencies. Above this altitude range, the picture is more complicated. Field data coverage above 35 km is sparse, hence it is difficult to judge the performance of the different theories and
parameterisations. Based on the available field data, HF86 shows the best
performance, followed by Ar83 and SA82, although both parameterisations come
with certain constraints: the ternary term of Ar83 has a weak performance
below 25 km; SA82 is solely dependent on *h* and contains no physical
information about *T* and *p*, similar to Ba85. This intercomparison ultimately shows that the question regarding an accurate parameterisation or theory of the recombination coefficient *α* for the troposphere and stratosphere is not yet solved and further research is necessary in the future.

## 7.2 Comparison to laboratory data

In a second step, the parameterisations and theories are compared to the
constant-pressure (1013.25 hPa assumed) and temperature-dependent (218.15–293.15 K) data set reported by Franchin et al. (2015). Here, only theories
and parameterisations are used that include the temperature as a parameter
and account for the ternary recombination mechanism (i.e. Ga38, Is57, Na59,
Lo60, Ar83, BC83, and HF86). Parameterisations that predict *α* based
solely on the altitude or only describe the binary recombination mechanism
are therefore excluded (i.e. Fu63, Hi79, SA82, Ba85, and Mi12). We used
the same parameters as in the previous subsection. The result of the
intercomparison is shown in Fig. 3. For Fr15, there is a general trend
towards higher recombination coefficient values for lower temperatures,
although the fluctuation is comparably strong. One should be mindful of the
possible sources of error from wall losses in the aerosol chamber and
sampling-line losses of the Neutral cluster and Air Ion Spectrometer (NAIS),
the instrument used to determine the mobility distribution of the ions from
which the ion–ion recombination rate could be derived. The reported
uncertainties for *α* can be as high as 30 % (Franchin et al.,
2015).

All theories and parameterisations agree within a reasonable range at ground-level temperatures (270–300 K). This is especially the case for the Thomsonian theories Ga38, Is57, Na59, and Lo60; in Ga38, Is57, and Lo60, almost the same values are yielded throughout the considered temperature range. However, the Thomsonian theories differ tremendously from the semi-empirical parameterisations (Ar83 and BC83) for tropopause temperatures (around 220 K). The
weaker temperature dependence (*T*^{−1.5}) of the group – Ga38, Is57, Na59, and Lo60 – results in a negligible increase of *α* with decreasing
temperatures. The laboratory data of Fr15, on the other hand, show a
stronger *T* dependence (around *T*^{−3}) that is best reproduced by Ar83 and
BC83. These parameterisations assume a *T*^{−5} dependence for the ternary recombination that is dominant at ground-level pressure; BC83 appears to reproduce the data points slightly better than Ar83. For
278 and 293 K, HF86 is in the same range as Fr15, although it yields much lower values for 248 K compared to Fr15. However, HF86 shows an unexpected behaviour below 230 K, with fluctuating *α* values that can even become negative. This feature occurs at different temperatures, depending on the input chosen for the ion masses.

In summary, all considered theories and parameterisations can reproduce the
laboratory data for warm temperatures (270 and 300 K), while only BC83 and
Ar83 can reproduce the *α* values for colder temperatures (218 and
248 K) because their temperature dependence is more similar to the
temperature trend in Fr15. The Thomsonian theories (Ga38, Lo60, Is57, and
Na59) only show a weak reaction to reducing temperatures, while HF86
displays an unexpected behaviour within the temperature range considered
here.

Franchin et al. (2015) have additionally used the model by López-Yglesias and Flagan (2013) to simulate the ion–ion recombination coefficient for the discussed temperature range. This model describes the ion–aerosol attachment coefficient, although it can also be applied to the special case of two ions recombining. However, the model is unable to reproduce the measured data in the low-temperature regime (Franchin et al., 2015).

As discussed in the previous section, the ion–ion trapping sphere radius *d* is an important parameter in the process of the ion–ion recombination. It is
connected with the recombination rate *α* according to Eq. (16)
(Natanson, 1959a). In order to find the values for the ion–ion trapping
radius as a function of pressure and temperature from the measured ion–ion
recombination rates (Rosen and Hofmann, 1981; Morita, 1983; Gringel et al.,
1978), the equation needs to be solved for *d*_{N}. Since this cannot be done analytically, it is performed numerically using the Newton–Raphson method. The results are listed in Table B1 and shown in Fig. 4a as an altitude plot, where each data point for *d* is based on the measured *α*. Only *α* values above 10 km are considered due to the erroneous determination of the ion–ion recombination coefficient below 10 km, as discussed previously. The values for the temperature and pressure are taken from the US Standard Atmosphere (National Oceanic and Atmospheric
Administration et al., 1976). The reference value for the electrical
mobilities, *μ*_{0}, for the conditions of 288.15 K and 1013.25 hPa is
1.3 × 10^{−4} m^{2} V^{−1} s^{−1} for Gr78 and Mo83, whereas 1.5 × 10^{−4} m^{2} V^{−1} s^{−1} is used for
the RH81 data set. The mobility values, *μ*, were adjusted for temperature and pressure according to Eq. (32), with a reference temperature of *T*_{0} = 288.15 K. For the calculations, it is further assumed that the masses are 90 Da for both the positive and negative ions (see Sect. 7).

All data sets yield similar results for *d* (see Fig. 4a). The resulting
values of *d* show an increasing trend with altitude; this trend is
approximately linear for a logarithmic *x* axis. A linear fit of all data
points using a logarithmic *x* axis yields the altitude-dependent
parameterisation given in Eq. (51) and a multivariate fit is performed to
determine the *T* and *p* dependencies (see Eq. 52):

It is not possible to extrapolate the parameterisations beyond the input data range of 10–45 km. Especially in the troposphere, the temperature trend is opposite to the one in the stratosphere, while the pressure trend is the same. Thus, a conclusion for the altitude range of 0–10 km cannot be drawn from these calculations. Furthermore, the significance of the pressure- and temperature-dependent fit is limited because the temperature only changes by approximately 15 % between 10 and 45 km altitude which could lead to imprecise results in the temperature dependence.

The gained values for the altitude-dependent Eq. (51) are 15 nm for 10 km,
22 nm for 20 km, and 57 nm for 44 km. The values for the temperature- and
pressure-dependent Eq. (52) are similar: 17 nm for 10 km, 21 nm for 20 km, and 59 nm for 44 km. These results are in contrast to the values calculated for Na59 according to Eq. (17) (see Fig. 4a). Natanson's trapping distance *d*_{N} is 15 nm at 0 km altitude, 22 nm at 10 km, and 29 nm at 20 km, reaching a maximum of 30 nm at 30 km; above this altitude, *d*_{N} decreases again, with a value of 27 nm at 44 km. For HF86 on the other hand, *d*_{HF} is assumed to be
constant at 18 nm. The divergence of the numerical determination presented
here, the calculation according to Natanson's formula, and the constant
value of Hoppel and Frick highlight that the determination of *d* is anything but trivial; further research has to be conducted to determine the ion–ion trapping distance for theories that use this parameter in their formulae.

The formula used in Eq. (41) by Filippov (1993) and Tamadate et al. (2020b) to determine the ion–ion recombination coefficient is generally valid. Other
theories, experiments, or models, therefore, only need to determine the
collision probability for ions entering the limiting sphere, *ε*_{δ}, in order to be compared with other theories or data sets. To
be able to validate the determined values with the field data,
*ε*_{δ} is calculated by analytically solving Eq. (41)
for *ε*_{δ} and using the balloon-borne ion–ion
recombination rates mentioned above as the input variable. The results are
listed in Table B1 and are shown in the altitude plot in Fig. 4b. All
data sets yield similar results and show a decreasing trend for increasing
altitudes. With a logarithmic *x* axis, this trend is linear and can be
described by the parameterisation given in Eq. (53):

For the above-mentioned reasons, this parameterisation is only valid between
10 and 45 km. For instance, *ε*_{δ} is 0.33 for 10 km
altitude, 7.9 × 10^{−3} for 20 km, and 1.0 × 10^{−6} for 44 km. The multivariate fit for *T* and *p* does not yield a satisfactory parameterisation for *ε*_{δ}; the deviation from the initially determined values can be as high as 1 order of magnitude for higher altitudes, therefore, the *T*- and *p*-dependent parameterisation is omitted.

The history of theoretical and empirical approaches to quantify the ion–ion
recombination coefficient *α* and its parameterisations have been
reviewed. The parameterisations and theories have been compared to field and
laboratory data and to a model calculation of *α* with a focus on
temperature and pressure dependence and their applicability to the
troposphere and stratosphere, i.e. from 0 to 50 km altitude. For standard
conditions (i.e. 273.15 K, 1013 hPa), the value of 1.7 × 10^{−6} cm^{3} s^{−1} is recommended to be used. Evidence is strong
that this value is accurate because several authors have derived it
independently from both laboratory measurements and model
calculations. As of today's knowledge, it is the best assumption to use a
nearly constant value for altitudes between 0 and 10 km; this is due to the
roughly counterbalancing effects of temperature and pressure on the
recombination coefficient. Above 10 km, however, a temperature- and
pressure-dependent parameterisation must be used to account for the
decreasing value of the ion–ion recombination coefficient. The
parameterisation of Israël (1957) shows the best agreement with the
field and model data of *α* for the altitude range of 0–22 km.
Between 0 and 20 km, the parameterisation by Brasseur and Chatel (1983) also
yields good results and, furthermore, it reproduces the recent laboratory
measurements the most faithfully. Between 10 and 25 km, the
altitude-dependent parameterisation of Bates (1985) reproduces the field
data accurately, while for altitudes above 25 km, the parameterisations of
Smith and Adams (1982) and Arijs et al. (1983) show the closest resemblance
to the field data, although it is difficult to judge this for altitudes
above 35 km because of the sparse data coverage above this altitude. Above
30 km altitude, the theory of Hoppel and Frick (1986) shows an excellent
agreement with the (sparse) field data.

However, the understanding of the processes in ion–ion recombination is far from complete. Binary and ternary recombination mechanisms both play a role; however, their specific temperature and pressure dependencies are not fully resolved up to the present day. Additionally, the ion–ion recombination is influenced by the mobilities and masses of the ions. Moreover, this work only focussed on the recombination in air; additional gases can be investigated in future studies. More experiments and state-of-the-art model simulations, including MD simulations, are needed to determine the ion–ion recombination coefficient in dependence of temperature, pressure, ion masses, and ion mobilities. This is crucial in order to accurately calculate the recombination loss of ions for the diverse ambient conditions we observe in our atmosphere.

They collision radius *r*_{coll} is defined as the sum of the radii of the positive and the negative ion, ${r}_{+}+{r}_{-}$, respectively. These can be
calculated in dependence of the masses of the two ions, the temperature, and
the pressure, according to Eqs. (A1) to (A4) (López-Yglesias and Flagan,
2013):

where *r*_{gas} is the radius of the gas molecule, *m*_{+} is the mass of the positive ion in kg, *m*_{gas} is the mass of the gas molecule in kg, *η* is the viscosity of the gas, *η*_{0} is the viscosity of the gas at standard temperature, and *S*_{C} is the Sutherland's constant. Accordingly, *r*_{−} can be calculated by replacing *m*_{+} for *m*_{−}, *v*_{+} for *v*_{−}, and *D*_{+} for *D*_{−}, respectively. Here, *T*_{0} = 298.15 K, for *m*_{gas}, we assumed 29 Da, for *η*_{0}, we used 1.827 × 10^{−5} Pa s (López-Yglesias and Flagan, 2013), and for *S*_{C}, we used 113 K (Chapman and Cowling, 1960).

b |
Critical collision parameter, in m |

d |
Ion–ion trapping distance or trapping sphere radius, in m |

d_{ia} |
Three-body trapping distance in ion–aerosol attachment (after Hoppel and Frick), in m |

d_{HF,N} |
Ion–ion trapping distance (after Hoppel and Frick, Natanson), in m |

d_{T} |
Ion–ion trapping distance, radius of the collision sphere around each ion, or radius of mutual Coulomb attraction between two ions of opposite charge (after Thomson), in m |

D |
Diffusion coefficient, sum of D_{+} and D_{−}, in m^{2} s^{−1} |

${D}_{+,-}$ | Diffusion coefficient of the positive, negative ion, in m^{2} s^{−1} |

${D}_{+/-,\mathrm{0}}$ | Diffusion coefficient of the positive/negative ion at standard temperature and pressure, in m^{2} s^{−1} |

D_{ion} |
Diffusion coefficient of one ion, in m^{2} s^{−1} |

e |
Electron charge, 1.602177 × 10^{−19} C |

E |
External electrical field, in V m^{−1} |

EA | Electron affinity, in eV |

h |
Altitude, in km |

k_{B} |
Boltzmann constant, 1.380649 × 10^{−23} J K^{−1} |

Kn _{δ} |
Knudsen number for the limiting sphere |

L |
Loss rate to the electrodes, in cm^{−3} s^{−1} |

[M] | Number density of air molecules, in cm^{−3} |

${m}_{+,-}$ | Mass of the positive, negative ion, in Da (unless noted otherwise) |

m_{gas} |
Molecular mass of the gas, in kg |

m_{ion} |
Ion mass, in Da (unless noted otherwise) |

m_{red} |
Reduced mass, in kg (unless noted otherwise) |

n |
Number concentration of ions in the gas phase, in cm^{−3} |

${n}_{+,-}$ | Number concentration of the positive, negative ions in the gas phase, in cm^{−3} |

n_{total} |
Number concentration of the sum of negative and positive ions in the gas phase, in cm^{−3} |

p |
Pressure, in hPa |

p_{0} |
Standard pressure, 1013.25 hPa |

q |
Ion pair production rate, in cm^{−3} s^{−1} |

r |
Distance of the two ions, in m |

r_{0} |
Initial distance of the two ions, in m |

r_{coll} |
Collision radius, sum of the radii of the positive and negative ions, in m |

r_{gas} |
Radius of the gas molecule, in m |

r_{p} |
Particle radius, in m |

RH | Relative humidity, in % |

S_{C} |
Sutherland's constant, 113 K for air |

t |
Time, in s |

T |
Temperature, in K |

T_{0} |
Standard temperature, 273.15 K |

v |
Equilibrium ion drift velocity, in m s^{−1} |

${v}_{+,-}$ | Mean thermal speed of the positive, negative ion, in m s^{−1} |

v_{rel} |
Relative thermal speed of two ions, in m s^{−1} |

w_{T,N} |
Function of x (used in Thomson theory and Natanson's theory) |

x |
Function of d_{T} and λ_{ion} (used in Thomson theory) |

x^{′} |
Function of T and p (used in Thomson theory) |

x_{N} |
Function of d_{N} and λ_{ion} (used in Natanson's theory) |

α |
Ion–ion recombination coefficient, in cm^{3} s^{−1} |

α_{2} |
Binary ion–ion recombination coefficient, in cm^{3} s^{−1} |

α_{3} |
Ternary ion–ion recombination coefficient, in cm^{3} s^{−1} |

α_{δ} |
Ion–ion collision rate coefficient at distance δ (limiting sphere surface), in m^{3} s^{−1} |

γ |
Function of r_{coll} or d_{HF} (used for the theories of Fuchs and Hoppel and Frick) |

δ |
limiting sphere radius, in m |

δ_{F} |
Limiting sphere radius of Fuchs, in m |

δ_{HF} |
Limiting sphere radius of Hoppel and Frick, in m |

Δα_{2} |
Enhancement to the ion–ion recombination coefficient due to the binary channel, in cm^{3} s^{−1} |

ε_{0} |
Vacuum permittivity, 8.854188 × 10^{−12} A s V^{−1} m^{−1} |

ε_{d} |
Probability factor for ions entering the trapping sphere |

ε_{L,T} |
Ratio of successful recombinations per collision (after Langevin, Thomson) |

ε_{N} |
Ion–gas molecule collision probability, also named “adsorption coefficient” (after Natanson) |

ε_{δ} |
Collision probability for ions entering the limiting sphere |

η |
Viscosity of a gas, in Pa s |

η_{0} |
Viscosity of air at 298.15 K, 1.827 × 10^{−5} Pa s |

θ |
Critical angle to enter the trapping sphere |

λ |
Ion–ion mean free path, in m |

${\mathit{\lambda}}_{+,-}$ | Mean free path of the positive, negative ion, in m |

λ_{air} |
Mean free path of air, in m |

λ_{ion} |
Mean free path of one ion, in m |

λ^{′} |
Mean distance of the last collision of a particle with a gas molecule before striking the limiting sphere surface (after Fuchs), in m |

μ |
Ion mobility, in m^{2} V^{−1} s^{−1} |

${\mathit{\mu}}_{+,-}$ | Ion mobility of the positive, negative ion, in m^{2} V^{−1} s^{−1} |

μ_{0} |
Ion mobility at standard temperature and pressure, in m^{2} V^{−1} s^{−1} |

σ |
Electrical conductivity of the air, in S m^{−1} |

Ψ_{δ} |
Ratio of Coulomb and thermal energy at distance δ (limiting sphere surface) |

The data shown in the figures are available on the data repository Zenodo: https://doi.org/10.5281/zenodo.7044018 (Zauner-Wieczorek et al., 2022).

MZW designed the study, surveyed the literature and compared the parameterisations, models and data sets. MZW and AK modelled the parameterisations and theories. MZW, AK, and JC discussed the results. MZW and AK wrote the manuscript; JC provided input for revision before submission.

The contact author has declared that none of the authors has any competing interests.

Publisher’s note: Copernicus Publications remains neutral with regard to jurisdictional claims in published maps and institutional affiliations.

We thank the three anonymous referees for their valuable feedbacks.

Marcel Zauner-Wieczorek is funded by the Heinrich Böll Foundation. This open-access publication was funded by the GRADE Center Sustain of Goethe University Frankfurt.

This paper was edited by Veli-Matti Kerminen and reviewed by three anonymous referees.

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- Abstract
- Introduction
- The fundamental theories
- Binary ion–ion recombination
- Field and laboratory measurements and semi-empirical parameterisations
- Application of ion–aerosol theories
- Numerical simulations
- Comparison of the parameterisations and theories
- Determination of the ion–ion trapping distance and the collision probability in the limiting sphere
- Conclusion and outlook
- Appendix A: Calculation of the collision radius
- Appendix B: Values for the ion–ion trapping distance and the collision probability in the limiting sphere
- Appendix C: Nomenclature
- Data availability
- Author contributions
- Competing interests
- Disclaimer
- Acknowledgements
- Financial support
- Review statement
- References

^{−6}cm

^{3}s

^{−1}, and recommend different theories or parameterisations depending on the altitude.

- Abstract
- Introduction
- The fundamental theories
- Binary ion–ion recombination
- Field and laboratory measurements and semi-empirical parameterisations
- Application of ion–aerosol theories
- Numerical simulations
- Comparison of the parameterisations and theories
- Determination of the ion–ion trapping distance and the collision probability in the limiting sphere
- Conclusion and outlook
- Appendix A: Calculation of the collision radius
- Appendix B: Values for the ion–ion trapping distance and the collision probability in the limiting sphere
- Appendix C: Nomenclature
- Data availability
- Author contributions
- Competing interests
- Disclaimer
- Acknowledgements
- Financial support
- Review statement
- References