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Massive identification of asteroids in three-body resonances

An essential role in the asteroidal dynamics is played by the mean motion resonances. Two-body planet-asteroid resonances are widely known, due to the Kirkwood gaps. Besides, so-called three-body mean motion resonances exist, in which an asteroid and two planets participate. Identification of asteroids in three-body (namely, Jupiter-Saturn-asteroid) resonances was initially accomplished by D.Nesvorny and A.Morbidelli (1998), who, by means of visual analysis of the time behaviour of resonant arguments, found 255 asteroids to reside in such resonances. We develop specialized algorithms and software for massive automatic identification of asteroids in the three-body, as well as two-body, resonances of arbitrary order, by means of automatic analysis of the time behaviour of resonant arguments. In the computation of orbits, all essential perturbations are taken into account. We integrate the asteroidal orbits on the time interval of 100000 yr and identify main-belt asteroids in the three-body Jupiter-Saturn-asteroid resonances up to the 6th order inclusive, and in the two-body Jupiter-asteroid resonances up to the 9th order inclusive, in the set of ~250000 objects from the"Asteroids - Dynamic Site"(AstDyS) database. The percentages of resonant objects, including extrapolations for higher-order resonances, are determined. In particular, the observed fraction of pure-resonant asteroids (those exhibiting resonant libration on the whole interval of integration) in the three-body resonances up to the 6th order inclusive is approximately 0.9% of the whole set; and, using a higher-order extrapolation, the actual total fraction of pure-resonant asteroids in the three-body resonances of all orders is estimated as approximately 1.1% of the whole set.


Introduction
A substantial role of resonances in the dynamics of asteroids became evident with the discovery of resonant "gaps" in the asteroid belt by D. Kirkwood in the perturbed pendulum model (Murray et al., 1998;Nesvorný andMorbidelli, 1998, 1999;Shevchenko, 2007).
An important parameter of a mean motion resonance is its order q, equal to the absolute value of the algebraic sum of the coefficients at the mean longitudes in the resonant argument: The resonant order q is important, because it is the power in which the eccentricity is raised in the coefficient of the leading resonant term in the expansion of the perturbing function (Nesvorný and Morbidelli, 1998). The corresponding subresonance width (characterizing also its "strength") is proportional to the square root of this coefficient. Thus the value of q determines this important property of the leading subresonance.
In the case of two-body resonances, the role of the resonant order q (defined below in Section 6) is analogous: the coefficient of the leading resonant term is proportional to e q (Nesvorný and Morbidelli, 1998), where e is the asteroidal eccentricity.
However note that, when there is no strong overlapping of subresonances, the resonant order q is not related to the width of the whole resonant multiplet, because the separation of subresonances depends solely on the secular precession rates of the pericentres (Nesvorný and Morbidelli, 1999); thus the degree of overlap (and hence, chaos) in the multiplets is expected to asymptotically decrease with the resonant order (Nesvorný and Morbidelli, 1999;Morbidelli and Guzzo, 1997).
One may expect that, generally, broader the leading subresonance of a mean motion resonance, greater is the number of objects residing in this mean motion resonance. However, no strict correlation exists, due to a competition of various dynamical and physical processes, populating or depopulating the resonances. We shall discuss this further in more detail.
In our procedure of resonance identification, described in detail below, we limit the set of possible combinations of the integers m J , m S , m by adopting the following conditions: where q max = 6 and M max = 8. Nesvorný and Morbidelli (1998) used condition (5) (presumably with q max = 10, as follows from data in table 3 in Nesvorný and Morbidelli 1998). In (Nesvorný and Morbidelli, 1999), instead of (6), the following truncation condition was used: (see eqs. (29) and (30) and comments on them in Nesvorný and Morbidelli 1999).
We identify the three-body resonances in the current motion of asteroids with known orbital elements. The limitations of our study are as follows: solely the asteroids in the main belt are considered (i.e., the semimajor axes are in the range from 2 to 4 AU); solely the three-body resonances with Jupiter and Saturn are taken into account; the resonances are considered in the planar problem, i.e., the longitudes of nodes in the expression for the resonant argument are ignored; the maximum considered order q max of the three-body resonances is set equal to 6.
Our project is intended for the resonance analysis of the orbital data presented at the "Asteroids -Dynamic Site" (AstDyS) maintained by A. Milani, Z. Knežević and their coworkers (http://hamilton.dm.unipi.it/cgi-bin/astdys/). We take the orbital data for the analysis from this database. Thus the total set under analysis contains ≈ 250000 objects.
The basic purpose of our work is to identify the current three-body resonances that all the asteroids from the given set are currently involved in. More specifically, each object from the set should be put in correspondence to a threebody resonance (or none, if there is no resonance). The first attempt of massive identification of asteroids in three-body resonances was made by Nesvorný and Morbidelli (1998): 255 objects were identified to be in three-body resonances. The libration/circulation of the resonant argument for asteroids suspected to reside in the resonances was analyzed visually. In our case the data set is much greater, and therefore the procedure ought to be completely automatic. Besides, here we apply a unified bound on the order. This allows one to construct a homogeneous identification list for a further statistical analysis.
To form a general statistical view of the resonant structure of the main belt, we also accomplish a massive identification of asteroids in two-body resonances with Jupiter, and compare the abundances of asteroids in three-body and twobody resonances.

The identification matrix
As a first stage of the identification process we build an "identification matrix". It consists of two main columns. The first one contains designations of resonances, and the second one contains the corresponding resonant values of the semimajor axis.
The designations of resonances are given in the notation m J m S m(q), where m J , m S , m are the integer coefficients in the resonant argument (2), and q is the resonant order, as defined above. The values of m J , m S , m are given with their signs. Thus, examples of this notation look like as follows: 5-2-2(1), 2+2-1(3).
We construct a set of the resonant arguments for all possible three-body resonances up to a fixed order q max in the following way.
We fix the maximum absolute value M max of each integer m J , m S , m to be equal to q max + 2, where q max is the maximum resonant order. It is assumed that where "gcd" stays for the greatest common divisor. It is set to be equal to 1 to avoid the higher order harmonics with greater multiplicity. The multiplicity is defined as equal to gcd (m J , m S , m). The harmonics with multiplicity greater than 1 are not discernible in our identification procedure, because their arguments librate simultaneously, though with different amplitudes. (Consider, e.g., such resonances as 4−2−2 and 8−4−4. The second one, which has multiplicity equal to 2, in our procedure is set to be equivalent to the first one.) Then we search through all possible combinations of m J , m S , m and identify those satisfying the D'Alembert rule (3) and our technical restrictions (5) and (6).
Let us demonstrate how the resonant value of the semimajor axis is calculated. According to the definition of the three-body resonance (1), the time derivativeσ pJ,pS,p should be equal to zero. Let us, following Murray et al. (1998), assume that̟ ≈ 0, in the first approximation. Then, for the resonant value of mean motion, one has Using Kepler's third law, one obtains for the resonant semimajor axis where n res is given by formula (9), and k is the Gauss constant. Holman and Murray (1996) and Murray et al. (1998) obtained an approximate formula for the precession rate of an asteroid's orbit: where µ ≈ 1/1047 is the mass of Jupiter in units of the mass of the Sun, n J and a J are Jupiter's mean motion and the semimajor axis of Jupiter's orbit, respectively, and For a, we substitute here the resonant value of the semimajor axis as given by Eq. (10). Thus the value of̟ is calculated. Iterating, one obtains an adequate value of a res . The second primary column of the identification matrix is filled with the resonant values of the semimajor axes, calculated as described, with the accuracy of no less than 10 −3 AU. This accuracy far exceeds the necessary one, because we check the asteroids for belonging to a given resonance in a far greater neighborhood (±10 −2 AU) of the computed resonant value of a res . Nesvorný and Morbidelli (1999) calculated a res of the leading subresonances (i.e., of the multiplet components σ 0,0,−mJ−mS−m ) of 19 three-body resonances with the accuracy of 10 −4 AU: they equated the time derivative of Eq. (2) to zero, and, using the values ofλ J andλ S as given by Bretagnon (1990) and ̟ as found using the code by Milani and Knežević (1994), calculatedλ. All values of a res given in (Nesvorný and Morbidelli, 1999, table 1) agree quite closely with the corresponding values of a res calculated here iteratively, as described above, for our matrix. The agreement is illustrated in Table 1, where an extract from the identification matrix is presented.

Dynamical identification
We use the following procedure of dynamical identification. First of all, each asteroid's orbit from the adopted set of 249567 objects is computed for 10 5 yr. The perturbations from all planets (from Mercury to Neptune) and Pluto are taken into account. The hybrid integrator of mer-cury6 package (Chambers, 1999) is used. In some cases the orbit9 integrator (http://adams.dm.unipi.it/∼orbmaint/orbfit/) is used as well, to verify the results. The computed trajectories are kept in files for further usage. The trajectories are output with the time step of 1 yr.
After integration is over, the objects are taken from the adopted set, and the mean value of the semimajor axis is computed for each object. Using this value, a set of preliminary resonant arguments σ res is found in the identification matrix. Each argument σ res is then analyzed on the presence of libration/circulation, using the computed trajectory of the object.
We distinguish two types of resonant libration: pure and transient. By definition, the libration is pure, if it lasts during the whole time interval of integration, i.e., 10 5 yr. An example of such libration is given in Fig. 1, where the time behaviour of the resonant argument, alongside with the orbital elements, is demonstrated for asteroid 463 Lola, resonance 4 − 2 − 1.
The libration is defined as transient, if circulation appears at any time during this interval. An example is given in Fig. 2; this is the case of asteroid 490 Veritas, resonance 5 − 2 − 2. In Fig. 2, it may seem unusual that Veritas exhibits circulation of the resonant argument while the semimajor axis remains almost constant (especially in comparison with Fig. 9, which is considered below and which shows the orbital elements and resonant argument of 1915 Quetzálcoatl, residing in the two-body transient resonance 3/1). This difference is explained by a large difference in the widths of the resonances: e.g., at e = 0.1 the width of resonance 3/1 is ∼ 5 times greater than that of resonance 5 − 2 − 2 (see fig. 1 in Morbidelli and Nesvorný 1999). Moreover, 1915 Quetzálcoatl has a very large eccentricity (∼ 0.6-0.8). At e = 0.1, the half-width of the 5 − 2 − 2 resonance is ≈ 0.002 AU (see table 1 in Nesvorný and Morbidelli 1999 and fig. 1 in Morbidelli and Nesvorný 1999). For Veritas, the eccentricity is ∼ 0.06 (see Fig. 2), hence the half-width is even smaller. This makes the shift in a, when σ is circulating, almost imperceptible, especially in the digitally unfiltered a. When a is filtered, such shifts look more obvious; see fig. 2 in (Knežević et al., 2002) and fig. 3 in (Tsiganis et al., 2007). Note that, when the circulations are short-term, the shifts in a can be imperceptible even in the digitally filtered element: see fig. 1 in (Nesvorný and Morbidelli, 1998), where the time behaviour of Veritas in the digitally filtered elements is shown.
To distinguish between transient-resonant and non-resonant behaviours we introduce a technical parameter: the resonance minimum time, which we set to be equal to 20000 yr. Roughly speaking, this is the minimum time interval of resonant librations, for an asteroid to be regarded as resonant. An exact definition is given below.
Nesvorný and Morbidelli (1998) identified resonant behaviour visually and used more subjective criteria, according to which the asteroid is resonant if "(1) the corresponding resonant angle shows evident librations during the integration time span or (2) the resonant angle circulates with a period longer than several thousand years" (Nesvorný and Morbidelli, 1998). In fact the second criterion threshold is analogous to our resonance minimum time, because our automatic procedure measures the time intervals of libration as such when no circulation is present, as described in detail below. Our criterion threshold, being larger, is more restrictive; however, in both cases the threshold is much greater than the timescales of circulation far from resonance; the latter timescales are of the order of asteroidal orbital periods.
The complete procedure of identification is as following. When computing each trajectory, the resonant argument value for the guiding subresonance is calculated at each step in time, and these values are written in a file, in function of time. After the trajectory computation is over, the time behaviour of the resonant argument is analyzed. If a current value of the resonant argument is different from its previous value by more than 2π, this means that there is a break, which takes place if there is either circulation or apocentric libration. To distinguish between these two cases, the same procedure is repeated, but with an artificial shift of the resonant argument. This shift is equal to π. Then, if there is apocentric libration, it turns into pericentric one, and there are no breaks.
At the beginning of the trajectory analysis, two variables are initiated: the first one is the duration of current libration, and the second one is the total time of libration. If circulation whenever starts, the first variable value is added to the second one and the first variable is reset to zero. At the end of the analysis, it is checked whether the second variable (total time of libration) is equal to the full time of computation (10 5 yr). If yes, then the asteroid is regarded to be in pure resonance. If no, but the second variable value exceeds the resonance minimum time, then the asteroid is in transient resonance. If the second variable value is less than the resonance minimum time, then the asteroid is regarded to be non-resonant. The adopted pure/transient division of resonances is thus mostly technical, because it depends on the chosen time interval of computation.
We use solely the direct method of identification, i.e., the resonant argument is checked on the subject of libration. Any secondary and/or auxiliary criteria, such as the semimajor axis behaviour, the location of objects in the proper "semimajor axis -eccentricity" plane, the Lyapunov exponents are left for future explorations, -with a partial exception in the latter case, see Section 5.
In our identification procedure, it is formally possible that an asteroid might be identified as belonging to two or even more resonances, because all resonances in a rather broad neighbourhood in semimajor axis (±10 −2 AU, as mentioned above) in the identification matrix are scanned on the subject of libration. If two three-body resonances are close enough in semimajor axis, and especially if they also overlap with a strong two-body resonance, an asteroid may intermittently diffuse from one to another resonance; a small number of such objects have been identified, as belonging to two resonances. In our lists, each object of this kind has been finally attributed to the resonance where it stayed for a longer time, to avoid complication of statistics. Analysis of such objects (we call them "rogue-resonant" asteroids) will be given elsewhere.
Besides, since the data used is unfiltered, some misidentifications may take place when the libration amplitude is high. To estimate the formal statistical error of our procedure, we randomly chose 300 asteroids identified as pureresonant and visually checked the libration of their resonant arguments. It turned out that only 4 objects (1.3% of the set) were misidentified. Thus the statistical error of the procedure is ≈ 1%.
All identified pure three-body-resonant asteroids, grouped according to association to a given resonance, are listed in the Appendix A. The top ten resonances, that are most "populated", are listed in Table 2. The last column of Table 2 contains analytical estimates of the resonance width (at the asteroidal eccentricity e = 0.1), according to (Nesvorný and Morbidelli, 1999, table 1). One can see that, generally, broader the resonance, greater is the number of objects residing in it. However, this tendency is not strict. The reason is that the dynamics here is strongly interrelated with physics: e.g., a collisional disintegration of an asteroid can strongly increase abundance of objects in a particular resonance, thus disturbing the expected correlation.
For each resonance, statistics on the asteroids in pure and transient librations have been calculated. The statistical results are summarized in Table 3 be ≈ 4.4% of the whole set. This is rather close to the value 4.6% (≈ 1500 in the set of ≈ 32400) found by Nesvorný and Morbidelli (1998) to serve as a lower bound for the relative number of resonant asteroids. As follows from Table 3, the fraction of asteroids in pure three-body resonances turns out to be ≈ 0.94% of the whole set. The third column of Table 3 contains a prediction for the numbers of asteroids residing in resonances of all orders; this subject is discussed in the next Section.
Let us consider the location of three-body-resonant asteroids in the "semimajor axis -eccentricity" plane. For each asteroid in a given resonance we calculate the average values (over the whole time interval of integration) of the semimajor axis and eccentricity and plot these values in the "a-e" plane. We have accomplished this procedure for each resonance with known structure of the resonant multiplet, as calculated by Nesvorný and Morbidelli (1999), so that the separatrix of the leading subresonance could be drawn. An example of such a plot is given in Fig. 3. It is clear that the percentage of "outliers" (objects out of the separatrix cell) is zero. This confirms the good accuracy of the accomplished identification procedure in the case of this particular resonance. A detailed study of the "a-e" plots will be given elsewhere.
We have cross-checked the lists of resonant objects identified in our study and in (Nesvorný and Morbidelli, 1998). It turns out that the number of resonant objects listed by Nesvorný and Morbidelli (1998) but not identified as resonant in our study does not exceed 1% of the list of Nesvorný and Morbidelli (1998). This confirms that the differences in the methodologies of identification in the two studies do not play any significant role in what concerns the reliability of results.

Expected abundances of asteroids in highorder three-body resonances
The obtained list of resonant asteroids is obviously not complete, due to the limitations of identification criteria. First of all, the resonant order q ≤ 6. Presumably, there is a lot of objects in resonances of higher orders. To take account of them, let us analyze the asteroid distribution in the resonant order q. The necessary data as derived from the results of the identification procedure are presented in Table 4. The constructed differential distributions (histograms) in q are shown in where a and b are two fitting parameters; b < 0. We have also tried the exponential law N ∝ exp(cq) (where c < 0), but it has turned out to be inappropriate, the statistical significance of fitting being very low.
Since we are interested in the tail behaviour of the distributions, we have  used the data for q ≥ 1, ignoring the specific case q = 0. In the case of all resonant (transient-resonant plus pure-resonant) asteroids (see Fig. 4) we find a = 2821 ± 454, b = −0.57 ± 0.18; and the correlation coefficient R 2 = 0.71. As soon as |b| < 1, the predicted number of asteroids in high-order resonances is formally infinite; in practice this means that it can comprise up to ∼ 100% of the whole set.
In the case of pure-resonant asteroids (see Fig. 5) we find a = 1095 ± 103, b = −1.64 ± 0.28; R 2 = 0.94. As soon as |b| > 1, the predicted total number of asteroids in high-order resonances is finite. Using Eq. (13), the number of objects with q ≥ 7 in the studied set is estimated to be equal to ≈ 516, or ≈ 22.1% of the identified number (2338). Therefore, the predicted total number of asteroids in pure three-body resonances is estimated as 2854, constituting 1.1% of the whole set (249567).
A note of caution is in order here. One has to admit that the fits made in this Section are based on few points, and, therefore, any statistical predictions, made with these formulas, are uncertain. What is more, one cannot even expect to find smooth distributions and/or strict correlations in this field of research, where dynamics is strongly interrelated with physics: the abundances of objects in resonant groups are regulated by various processes, e.g., by collisions and the Yarkovsky effect. Interactions with asteroidal families are important. Of course, higher order resonances should be directly analyzed in the future.
Another complicating factor is that the subresonance overlap (and hence, the degree of chaoticity) in the multiplets is expected to decrease asymptotically at q ≫ 1. The reason is that the subresonance typical width scales with q as ∼ e q (where e is the eccentricity), whereas the subresonances separation (determining the multiplet width) remains basically constant, depending solely on the secular precession rates of the pericentres; thus the overlap/interaction of subresonances in the multiplets decreases asymptotically at q ≫ 1 (Nesvorný and Morbidelli, 1999, p. 268-269). When the ratio of the subresonances separation to the width of the leading subresonance is much greater than one, the separatrix chaotic layers are exponentially thin with this ratio, see (Chirikov, 1979;Shevchenko, 2008Shevchenko, , 2011. It is straightforward to suppose that, if one fixes the asteroidal eccentricity, three-body resonances with increasing order become basically regular (Nesvorný and Morbidelli, 1999). Thus, if the resonances are populated uniformly in the eccentricity, the power-law extrapolation for the high-order transient-resonant populations fails beyond some order. Only if this critical order is high enough, the extrapolation-based estimates might be appropriate.

Lyapunov exponents in three-body resonances
The AstDyS database provides information on the maximum Lyapunov exponents for almost all asteroids contained in it. The provided values are computed on time intervals of 2 mln yr, i.e., on time intervals 20 times greater than that we use in our identification procedure. It is instructive to check how the data on Lyapunov exponents correlate with the pure/transient division (adopted in our study) of the resonant asteroids.
In the transient case the motion is expected to be chaotic, and in the pure case to be essentially regular, because transitions from libration to circulation and vice versa are inevitable in a separatrix chaotic layer of resonance. However, the adopted relatively short integration time may imply that many "pure"resonant asteroids become transient on longer timescales.
First of all, let us build distributions of resonant asteroids in L (the maximum Lyapunov exponent). The constructed differential distributions (histograms) are presented in a single plot in Fig. 6. The Lyapunov exponents are given in units of (mln yr) −1 . (Note that in the AstDyS database they are given in units of yr −1 .) N is the number of objects in the interval (L, L + ∆L), where ∆L = 10. The grey histogram is for the asteroids in transient resonances, and the black one is for the asteroids in pure resonances. The histograms are cut off at L = 500, because the objects with greater values of L are rare; they are all transients.
From Fig. 6 it is clear that the transients have a much more extended distribution in L, in comparison with the pure-resonant objects, as expected. This difference is uniform in all resonant groups, as can be directly seen from Fig. 7, where the maximum Lyapunov exponents are plotted versus the semimajor axis a: the positions of open dots (representing transients) extend to much greater heights, in comparison with the pure-resonant objects, in all resonant groups. Note that this plot is built without any cut-off in L, i.e., all objects are shown. It is evident that only transients have very large Lyapunov exponents, corresponding to Lyapunov times as small as ≈ 570 yr. Among all identified pure-resonant objects, the average L is 34.3 (mln yr) −1 , and among all identified transients it is 49.7 (mln yr) −1 . The Lyapunov times are ≈ 29200 and ≈ 20100 yr, respectively. Among all objects of the AstDyS database with measured Lyapunov exponents, the average L = 20.8 (mln yr) −1 , corresponding to the Lyapunov time ≈ 48100 yr. Thus both pure-resonant and transient-resonant objects turn out to be more chaotic than a typical asteroid. The fact that many pure-resonant asteroids have definitely non-zero Lyapunov exponents signifies that they become transient on the timescales longer than the adopted integration time (10 5 yr). This underlines the conditional character of the "pure/transient" technical classification adopted in our study.

Two-body resonances with Jupiter
To form a more general statistical view of the actual resonant structure of the main belt, it is instructive to compare the abundances of asteroids in three-body resonances with the abundances of asteroids in two-body resonances. For this purpose, we have performed a procedure of identification of asteroids in twobody resonances with Jupiter, analogous to that described above for the case of three-body resonances. In this identification procedure, we assume circular and zero inclination orbits of perturbing planets. Taking into account the D'Alembert rule, the resonant argument for the resonance of order q is defined by the following formula (Murray and Dermott, 1999;Morbidelli, 2002;Gallardo, 2006): where λ J and λ are the mean longitudes of Jupiter and an asteroid, respectively, and ̟ is the longitude of perihelion of the asteroid; q is the resonant order, p is integer.
Of course, this setting of the identification problem is a rather simplified one. When real resonant asteroids are considered, the "circular" subresonance term is not expected to dominate universally; what is more, the resonant asteroid might reside in another component of a multiplet (see Holman and Murray 1996;Murray and Holman 1997). We regard the adopted approach as a first approximation, and leave considerations of all possible subresonances for the future.
The resonant value of the semimajor axis of an asteroidal orbit is given by where a J is the semimajor axis of Jupiter's orbit, and µ is the mass of Jupiter in units of the mass of the Sun (see, e.g., Murray and Dermott 1999;Gallardo 2006). The identification matrix is constructed in the way analogous to that described in Section 2. Similar to the case of three-body resonances, it is assumed that gcd (p, q) = 1. Besides, 1 ≤ p ≤ 11.
The resonant order range is limited to 0 ≤ q ≤ 9. Recall that in the case of three-body resonances we have set 0 ≤ q ≤ 6. Choosing the upper bounds with the difference equal to 3 allows one to adequately compare identification statistics for two-body and three-body resonances, because "a three-body resonance of a given order q should have roughly the same strength as a usual resonance of order q + 3 for eccentricity of about 0.05-0.10" (Nesvorný and Morbidelli, 1998). Such a trick was used in Nesvorný and Morbidelli (1998) for similar purposes.
Figs. 8 and 9 show the time behaviour of the resonant argument and orbital elements of 1915 Quetzálcoatl and 190 Ismene, as two typical examples. The top ten most "populated" resonances, identified in our study, are listed in Table 5. All identified pure two-body-resonant asteroids, grouped according to association to a given resonance, are listed in the Appendix B. 1 The resulting statistics of identified objects are listed in Tables 6 and 7. As follows from Table 6, a half of all identified asteroids in pure two-body resonances are Trojans (1669/3132 ≈ 53%). Pure Trojans plus pure Hildas constitute ≈ 85% of all asteroids in pure two-body resonances in our set. In Table 7, the q dependence of the resonant asteroid abundances is presented. The dependence is obviously irregular and does not permit any smooth decay approximation. Especially one should point out the negligible asteroid abundances at q = 3 and q = 9.     If Trojans and Hildas are not excluded, the fraction of pure-resonant asteroids among the transient+pure-resonant asteroids is ≈ 3.3 times greater in the two-body case than in the three-body one (≈ 70.4% versus ≈ 21.2%); thus it might seem that the two-body resonances are much more "pure" on average. However, if one excludes Trojans and Hildas, the fractions become comparable: 26.1% versus 21.2%.
One should outline that the comparative analysis given here is merely statistical and, thus, formal. However, such an analysis might provide a necessary preliminary stage for a deeper study of the comparative role of two-body and three-body resonances; such a study should comprise consideration of the physical (collisions and the Yarkovsky effect) and dynamical (transport and diffusion) processes, which lead to populating or depopulating the resonances. 2. The fraction of asteroids in three-body resonances (transient plus pure) up to the 6th order inclusive turns out to be ≈ 4.4% of the total studied set of 249567 asteroids. The fraction of asteroids in pure three-body resonances of the same orders turns out to be ≈ 0.94% of the total studied set.
4. Using a high-order extrapolation (in the form of a power law) of the q dependence of the number of identified resonant objects, the actual total fraction of asteroids in pure three-body resonances of all orders is estimated as ≈ 1.1% of the whole set. In what concerns the case of transient three-body resonances, the situation is much less certain, because the power-law extrapolation diverges.

5.
We have also identified all objects residing in two-body resonances (of order 0 ≤ q ≤ 9) with Jupiter in the main asteroid belt, taking the same database of asteroids. The list of all asteroids identified as residing in pure two-body resonances is given in Appendix B.
6. The half of all identified asteroids in pure two-body resonances are Trojans (≈ 53%). The pure Trojans plus pure Hildas constitute ≈ 85% of all asteroids in the pure two-body resonances. The q dependence of the two-body resonant abundances is clearly irregular and does not permit any smooth decay approximation. Especially one should point out the negligible asteroidal abundances at q = 3 and q = 9.
7. In the transient plus pure resonances, the identified asteroids are ≈ 2.5 times more abundant in the three-body resonances than in the two-body resonances; and in the pure resonances the abundances are comparable. However, if one excludes Trojans and Hildas, the abundance of three-bodyresonant asteroids becomes overwhelming. What is more, taking into account extrapolated abundances in high-order resonances may substantially increase this overwhelming domination. Thus our analysis quantitatively verifies the assertion by Nesvorný and Morbidelli (1998) that "the threebody mean motion resonances seem to be the main actors structuring the dynamics in the main asteroid belt".
8. We would like to point out that our results confirm the general concept of Molchanov (1968Molchanov ( , 1969 on the omnipresence of resonances in the Solar system, however at a new level of understanding of this phenomenon.