Eccentricity evolution in mean motion resonance and nonradial solar wind
P. Pástor  J. Klacka  J. Petrzala  L. Kómar
Department of Astronomy, Physics of the Earth, and Meteorology, Faculty of Mathematics, Physics and Informatics, Comenius University, Mlynská dolina, 842 48 Bratislava, Slovak Republic
Received 4 November 2008 / Accepted 4 March 2009
Abstract
Eccentricity evolution of a dust particle in a mean motion orbital
resonance with a planet in circular orbit is investigated. The action
of solar electromagnetic and corpuscular radiation, including nonradial
components of the solar wind velocity, is taken into account.
Various types of eccentricity evolution depend on the angle between
the radial direction and the direction of the solar wind velocity.
The evolution changes at the analytically derived angles.
Its application to exosolar systems is included.
Key words: Sun: solar wind  interplanetary medium  celestial mechanics  stars: planetary systems
1 Introduction
The motion of interplanetary dust particles is influenced by gravitational forces of the Sun and planets and by nongravitational effects. The effect of solar electromagnetic radiation in the form of the PoyntingRobertson (PR) effect and the effect of the radial solar wind are conventionally taken into account (see, e.g. Robertson 1937; Wyatt & Whipple 1950; Whipple 1955; Dohnanyi 1978; Leinert & Grün 1990; Dermott et al. 2001; Grün 2007).
Physics of resonances with Solar System planets has been investigated mainly for the last three decades. The orbital motion of dust particles in mean motion orbital resonances with a planet has been intensively studied since Jackson & Zook (1989) predicted a ring of dust particles in resonances with the Earth. The ring was observed by satellites IRAS (Brownlee 1994; Dermott et al. 1994) and COBE (Reach et al. 1995). The orbital evolution of interplanetary dust particles near zones of mean motion resonances was investigated in many papers (Weidenschilling & Jackson 1993; Beaugé & FerrazMello 1994; Sidlichovský & Nesvorný 1994; Liou et al. 1995; Liou & Zook 1999; Kuchner & Holman 2003; Klacka & Pástor 2004). Liou & Zook (1997) derived the relation between the secular time derivative of eccentricity and the secular time derivative of the inclination of dust particles in mean motion resonance with a planet in a circular restricted threebody problem with the PR effect and the radial solar wind (the authors incorrectly accounted for the radial solar wind). As for the planar case, it is possible to obtain secular time derivative of a particle's eccentricity using the method presented in Liou & Zook (1997). The orbital evolution in mean motion resonance in the planar elliptical restricted threebody problem with the PR effect is discussed in Pástor et al. (2007). The evolution of eccentricity of the particle under the action of the PR effect and the nonradial solar wind in mean motion resonances with a planet in a circular orbit is investigated in Klacka et al. (2008). Measurement of the nonradial component of the solar wind velocity was performed by Helios 2 during its first solar mission in 1976 (Bruno et al. 2003). According to these results, the angle between the direction of the solar wind velocity and the radial direction is practically independent of heliocentric distance, at least for the distances covered by observations. A constant value of this angle is also in accordance with the results of Parker (1958).
We are motivated mainly by the results of Klacka et al. (2008). We want to obtain detailed predictions of orbital evolution in the orbital resonances when the PR effect and the nonradial solar wind are considered.
2 Equation of motion
Let us consider a spherical dust grain under the action of gravitational forces
generated by the Sun and a planet moving around the Sun. Moreover, the grain
is evolving under the action of solar electromagnetic radiation and solar wind.
The equation of motion of the particle is considered in the form
where is velocity vector of the particle, , , , is transversal unit vector, and are position vectors of the particle and the planet (mass m_{P}) with respect to the Sun (mass ), , G is the gravitational constant, u is the speed of the solar wind km s^{1}, c is the speed of light, , is the angle between the radial direction and the direction of the solar wind velocity (the angle lies between 2.3 and 2.9 degrees, according to Bruno et al. (2003), and the value of does not significantly depend on heliocentric distance). Parameter is defined as the ratio of the radial component of the electromagnectic radiation force and the gravitational force between the Sun and the particle with zero velocity
is solar luminosity, W (Bahcall 2002), is the efficiency factor for radiation pressure integrated over the solar spectrum and calculated for the radial direction ( for a perfectly absorbing sphere), R is the radius of the spherical particle and its density. is the ratio of solar wind energy to electromagnetic solar energy, both radiated per unit of time
where n_{w} is the concentration of the solar wind particles at distance r from the Sun, and m_{1} is the mass of the solar wind particle(s). for the Sun. The force caused by the solar wind is derived using the method presented in Klacka & Saniga (1993) and Klacka (1994). For details of the PR effect, we refer to Poynting (1903), Robertson (1937) and Klacka (2008a,b) and Klacka et al. (2009). In the derivation of Eq. (1) it is assumed that is approximately in the interval (5, 5). This interval enables us to consider in the derivation of Eq. (1). Moreover, we assume that the inclination of a dust particle with respect to the solar equator is approximately in the interval (5, 5). More complicated expressions for the nonradial solar wind force should be used outside the above presented intervals.
3 Mean motion orbital resonances with planets
A particle is in the qth order exterior mean motion resonance with a planet if the ratio of its mean motion n and the mean motion of the planet n_{P} approximately satisfies the equation n_{P}/n = (p+q)/p, where p and q are natural numbers. Similarly, the qth order interior mean motion resonance is defined by the relation n_{P} / n = p / ( p + q ). The special case mean motion 1/1 resonance corresponds to q = 0. In terms of orbital periods: T / T_{P} = ( p + q ) / p for the exterior, T / T_{P} = p / ( p + q ) for the interior resonance and T / T_{P} = 1 for mean motion 1/1 resonance.
We can determine the semimajor axis of the particle in the mean motion
resonance from Kepler's third law. We have
where a, a_{P} are semimajor axes of the particle characterized by the optical parameter and a planet with mass m_{P} orbiting the Sun of mass . The first part of Eq. (4) uses the fact that central Keplerian acceleration is given by the sum of solar gravitational acceleration and the dominant radial component of radiation pressure acceleration. With the assumption that we obtain from Eq. (4)
On the basis of the definition of mean motion resonance and Eq. (5), we can write
for the semimajor axis of the particle in the qth order exterior resonance with a planet of mass m_{P}. A similar relation can be obtained for the interior resonance. For mean motion 1/1 orbital resonance we can put q = 0 in Eq. (6).
4 Evolution of eccentricity in a mean motion resonance
A dust particle is captured in a mean motion orbital resonance with a planet
and the PR effect and the nonradial solar wind affect its motion.
The secular time derivative of the eccentricity of the particle
is (Klacka et al. 2008)
where . In the derivation of this equation it is assumed that . The ratio a/a_{P} can be expressed through the ratio n_{P}/n from Eq. (5). If the initial eccentricity equals 0, then the derivation of Eq. (7) does not allow any conclusions since the partial derivative of the Tisserand parameter with respect to eccentricity is 0 (see Klacka et al. 2008).
We define a new function W (e) as
The differentiation of the function W (e) with respect to eccentricity is
It is easy to show that d for all e (0, 1) and for . Thus, W (e) is a decreasing function for these values. The value W (e = 0) is
4.1 Exterior mean motion resonances
Figure 1 depicts the function W (e) for exterior mean motion 4/3 resonance for various values of . If W (e) is positive, then the eccentricity increases from a given value of eccentricity e. If W (e) is negative, then the eccentricity decreases.
For the exterior mean motion resonances, Eq. (10) reduces to
The value W (0) is positive or zero for .
Figure 1: The function W (e) for exterior mean motion 4/3 resonance. Various values of are used. 

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4.1.1 1
If
,
then the function W(e)is a decreasing function of eccentricity (see Eq. (9) and Fig. 1).
One root of the function W(e) exists,
since W(0) > 0 and
.
We denote this root as .
Various functions W (e) in Fig. 1
intersect at eccentricity e_{y} for which is Y (e) = 0. W (e_{y})is negative. The statement follows from the inequality
which holds for all e [0, 1). , because W(e)is a decreasing function of eccentricity and > W (e_{y}). If , then W(e) > 0. Thus, the secular evolution of eccentricity is an increasing function of time and the eccentricity asymptotically increases to the value (since ). If , then W(e) < 0 and the eccentricity asymptotically decreases to the value . The value of is a decreasing function of (for more details see Appendix A). If reaches the value , then W (0) = 0. Thus, . We assumed that 5 , in the derivation of Eq. (1). Thus, for the case , we can define the angle for which . We get
Let us denote e_{x} the value of the eccentricity at which X(e) = 0for exterior resonances. We have (see also Liou et al. 1995)
If the value of increases from 0 (the radial solar wind and the PR effect) to , then the value of decreases from e_{x} to 0 (circular orbit).
4.1.2 1 < < 3
If for an exterior mean motion resonance, then W (e) does not have a root for e [0,1), since W (0) < 0 and W (e) is a decreasing function of eccentricity. The secular evolution of eccentricity is always a decreasing function of time and the eccentricity nonasymptotically decreases to 0 (zero eccentricity can be reached).
4.1.3 3
If
3
for exterior mean motion resonances, then W (0) < 0. The
function W (e) also can be an increasing function of eccentricity, but only
if the following inequality holds:
see Eq. (9).
Three possibilities exist:
 1.
 W (e) does not have a root for e [0,1);
 2.
 W (e) has only one root for e [0,1)  we will denote it ;
 3.
 W (e) has two roots for e
[0,1) 
we will denote them
and
.
Possibility 1:
The secular evolution of eccentricity is always a decreasing
function of time. The eccentricity nonasymptotically decreases to 0.
Possibility 2:
We can write for
since corresponds to the maximum of the function W (e). If the initial eccentricity is greater than , then eccentricity asymptotically decreases to the value . If the initial eccentricity is less than , then the value of the eccentricity nonasymptotically decreases to 0.
Possibility 3:
In this case we put
.
If the initial eccentricity is greater than
,
then the eccentricity asymptotically decreases to the value
.
If the initial eccentricity lies between
and
,
the eccentricity asymptotically increases to the value
.
Finally, if the initial eccentricity is smaller than the value
,
then the eccentricity nonasymptotically decreases to 0.
4.2 Interior mean motion resonances
The graph of the function W (e) for the interior mean motion 2/3 resonance is depicted in Fig. 2. Various values of are used.
For interior mean motion resonances, Eq. (10) reduces to
The value W (0) is negative for .
Figure 2: The function W (e) for interior mean motion 2/3 resonance for various values of . 

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4.2.1 < 1
If , then W (0) < 0 and W (e) is a decreasing function. Secular evolution eccentricity is always a decreasing function of time. The eccentricity nonasymptotically decreases to 0.
4.2.2 1
If , then W (0) = 0. Thus, = 0 is a root of W (e). The eccentricity asymptotically decreases to (circular orbit). For the value we can define (similarly to exterior resonances) an angle for which . We can calculate for the interior resonances from the condition .
If
,
then W (0) > 0. In this case, at
least one root
of W (e) exists. We will show that W (e)has only one root
for e
[0,1). If eccentricity fulfills
the inequality given by Eq. (15) (we can apply this inequality also for
interior resonances), then W (e) is an increasing function.
If the following inequality
is fulfilled, then the function W (e) is a decreasing function (see Eq. (9)). Since W (0) > 0 and , the function W (e) has only one root for e [0,1). This behavior is also consistent with evolutions for depicted in Fig. 2 for mean motion 2/3 resonance. is an increasing function of (for more details see Appendix B). If the initial eccentricity is greater than the value , then the eccentricity asymptotically decreases to the value . If the initial eccentricity is less than the value , then the eccentricity asymptotically increases to the value .
4.3 Mean motion 1/1 resonance
Finally, let us consider the special case mean motion 1/1 orbital resonance (q = 0). The graph of the function W (e) for 1/1 resonance is shown in Fig. 3. Various values of are used.
For the mean motion 1/1 resonance, Eq. (10) reduces to
Thus, one root of the function W (e) always exists, for the mean motion 1/1 resonance.
Figure 3: The function W (e) for mean motion 1/1 resonance for various values of . 

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4.3.1
W (e) is a decreasing function and W (0) = 0. Thus, W (e) < 0for e (0,1). The eccentricity asymptotically decreases to 0.
4.3.2 > 3
If > 3, then another root of W (e) exists, because W (e) is also an increasing function for the values of eccentricity determined by inequality Eq. (15) and W (0) = 0. If the initial eccentricity is greater than , then the eccentricity asymptotically decreases to . If the initial eccentricity is less than , then the eccentricity asymptotically increases to .
5 Discussion
The case
yields, qualitatively,
the same secular evolution of eccentricity as the case
.
For the exterior mean motion resonances, eccentricity exhibits two
monotonous parts (an increasing and a decreasing one) asymptotically
approaching the limiting value of the eccentricity. For
the interior mean motion resonances, eccentricity is a decreasing function
of time and the eccentricity nonasymptotically decreases to 0.
The evolution of eccentricity changes for both types of resonances,
exterior and interior, at the value
.
Evolution of the eccentricity changes to a nonasymptotically
decreasing evolution for the exterior mean motion resonances, and
to an asymptotic behavior for the interior mean motion resonances.
represents the smallest value of
for which the secular evolution of eccentricity changes
(two such values exist for exterior resonances,
but only one value for interior resonances).
If we use Eq. (6) and a similar equation for
the interior resonances, then we get (see Eq. (13))
for the exterior resonances and
for the interior resonances.
Table 1 presents the values of for , , u= 400 km s^{1}, , 1 and 3/2, for several exterior and interior resonances with a planet in a circular orbit of radius a_{P}= 30.058 AU (approximately the semimajor axis of planet Neptune).
Table 1: Values of (in degrees) for various exterior and interior resonances with a planet in a circular orbit of radius a_{P}= 30.058 AU. The particle is characterized by and the solar wind by and u = 400 km s^{1}.
Figure 4: Evolution of eccentricity obtained from Eq. (7). A dust particle with and is captured in the exterior mean motion 4/3 orbital resonance with a planet of semimajor axis a_{P}=30.058 AU and eccentricity e_{P}= 0. Solar wind parameter . Evolution curve for various initial conditions of eccentricity are shown. 

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Figure 5: Evolution of eccentricity obtained from Eq. (7). A dust particle with and is captured in the exterior mean motion 4/3 orbital resonance with a planet of semimajor axis a_{P}= 30.058 AU and eccentricity e_{P}= 0. The solar wind parameter . 

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Figures 4 and 5 depict secular evolution of the particle's eccentricity in the exterior mean motion 4/3 resonance with a planet in a circular orbit of radius a_{P}= 30.058 AU for the case and . Figure 4 holds for and Fig. 5 holds for . If , then the evolution of the eccentricity is similar to Fig. 4. If 1.762 , then the secular evolution of the eccentricity is similar to Fig. 5. The detailed numerical integrations of Eq. (1) are consistent with Eq. (7). Evolutions depicted in Figs. 4 and 5 are calculated from the numerical solution of Eq. (7).
Figure 6: Evolution of eccentricity of a dust particle with and captured in the exterior mean motion 5/4 orbital resonance with a planet of semimajor axis a_{P}= 80 AU and eccentricity e_{P}= 0. Solar wind parameter . Evolution curves for various initial eccentricity are shown. 

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Figure 6 depicts the evolution of eccentricity for the case when the function W (e) has two roots ( ). Various evolutions differ only in initial values of eccentricity. A dust particle with and is captured in the exterior mean motion 5/4 resonance with an artificial planet in a circular orbit of radius a_{P}= 80 AU. The speed of the solar wind is u=400 km s^{1} and the angle between the radial direction and the direction of the solar wind velocity is . An asymptotic approach to the limiting value is evident. The evolution of eccentricity is always a decreasing function of time, below the initial eccentricity .
Figure 7: Orbital evolution of a spherical dust particle with and captured in the exterior mean motion 5/4 resonance with a planet of mass m_{P} = 20 in a circular orbit with a semimajor axis a_{P} = 80 AU. Solar wind parameter . 

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Figure 7 depicts results of numerical integration of Eq. (1). A particle with and is captured in a mean motion 5/4 resonance with a planet of mass m_{P} = 20 ( kg) in a circular orbit with a semimajor axis 80 AU. The solar wind is characterized by u= 400 km s^{1}, , . As the mass of the star we use solar mass. Initial conditions of the particle are AU, e = 0.6, , , where a_{5/4 0.01} is the semimajor axis calculated from Eq. (6) using p = 4, q = 1 and . is the argument of perihelion and f is the true anomaly. The planet's initial position is on the Xaxis (the axis from which the argument of perihelion is measured). The initial eccentricity of the fifth evolution of eccentricity from the top of Fig. 6 is also 0.6. This evolution of eccentricity corresponds to the evolution of eccentricity obtained by numerical integration of Eq. (1) shown in Fig. 7. Numerical integration shown in Fig. 7 is in accordance with our analytical theory, since evolution of eccentricity asymptotically increases to the value .
We found that the function W(e) can have two roots for the first order exterior resonances also for smaller values of if we use greater p (when the other parameters in the function W (e)are constant). But the resonance overlap begins to be significant for the first order exterior resonances with higher p (see e.g. Murray & Dermott 1999). The particle is captured into a 1/1 resonance with a higher probability than into the first order exterior resonance with a high value of p.
Now, we find how
depends on the individual physical
quantities characterizing the star, planetary orbit and dust grain.
We will carry out our analysis for a given resonance, defined by numbers p and q. Putting Eqs. (2) and (3) into Eq. (7) yields
using Eq. (5) and the notation 4 . We may assume that the value of n_{l} is a constant independent of the distance from the star. Equation (22) also provides a dependence of on physical quantities characterizing a given system.
Now, we can find how
depends on individual variables.
It is evident that the value of
decreases with
an increasing value of the semimajor axis of the planet a_{P}(see Eq. (22)).
is an increasing function
of a particle's radius R and mass density .
The function
f_{1}(x_{1})=(1+a_{1}x_{1})/(a_{1}x_{1}) has a derivative with
respect to x_{1} equal to
f'_{1}(x_{1})= 1/(a_{1}x_{1}^{2}).
f_{1}(x_{1}) is a decreasing function for positive values of a_{1}.
Thus,
will be a decreasing function of n_{l} and m_{1}.
The function
has a derivative equal to
.
.
Since
for particles captured
in a mean motion resonance, we obtain
.
Thus,
will be an increasing function of M.
The function
f_{3}(x_{3})=(1 + a_{3}x_{3})/(a_{3}x_{3}^{2}) has a derivative
equal to
f'_{3}(x_{3})=(2 + a_{3}x_{3})/(a_{3}x_{4}^{3}). f_{3} is a decreasing
function of x_{3}, for positive a_{3} and x_{3}. Thus,
is a decreasing function of u.
The function
f_{4}(x_{4})=(1+a_{4}/x_{4})(1b_{4}x_{4})^{1/3}/(a_{4}/x_{4})has a derivative equal to
f'_{2}(x_{4})=(3a_{4}b_{4}4b_{4}x_{4})/[3a_{4}(1b_{4}x_{4})^{2/3}],
a_{4} > 0 and
Thus, can be an increasing or a decreasing function of L and for arbitrary values of , and .
We can conclude that will be always a decreasing function of a_{P}, n_{l}, m_{1}, u, and, an increasing function of M, R, . Equation (22) yields that may be neither an increasing nor a decreasing function of L and if the other parameters are fixed (we do not take into account that luminosity of a star may depend on its mass).
To obtain the evolution presented in Fig. 6 we need to minimize the value of or maximize value of in order to have the maximum of the value . Thus, is larger for stars with strong stellar wind (high n_{l}, m_{1}, u) or with large a value of . The value of can be sufficiently high also for a particle in a resonance with a planet in orbit with a large semimajor axis a_{P}. Known systems with a star similar to the Sun and a planet in an orbit with large a semimajor axis are: GQ Lup ( , Seperuelo et al. 2008; AU, Neuhäuser et al. 2005), 1RXS J160929.1210524 ( M = 0.85^{+0.20}_{0.10} ; AU, Lafreniere et al. 2008). Also AB Pic has a planet candidate at a separation of 258 AU (Chauvin et al. 2005). But AB Pic is classified as a dwarf star, similar to many known systems with large semimajor axes. If we calculate for an exosolar system and its value is higher than 3, then secular evolution of the particle's eccentricity in an exterior mean motion resonance can be similar to some of the evolutions shown in Fig. 6.
6 Conclusion
We investigated the evolution of eccentricity of an interplanetary spherical dust particle under the action of resonant perturbation of a planet in a circular orbit, the PR effect and nonradial solar wind.
Eccentricity asymptotically approaches (increases or decreases) a limiting value in exterior mean motion resonances (simple asymptotic behavior) if the PR effect and radial solar wind are considered. If also the nonradial component of the solar wind velocity is taken into account, then various possibilities exist. If the angle between the radial direction and the velocity of the solar wind fulfills 0 , then the eccentricity evolution is similar to the case of a radial solar wind. If , then the eccentricity is a decreasing function of time and the eccentricity nonasymptotically decreases to zero.
For interior mean motion orbital resonances, eccentricity is always a nonasymptotically decreasing function of time for the PR effect and the radial solar wind. The behavior of particle's eccentricity is inverse to the behavior in the exterior resonances for . If we take into account the nonradial component of the solar wind velocity and , then the evolution of eccentricity is similar to the case of the radial solar wind. If , then eccentricity asymptotically approaches the limiting value (simple asymptotic behavior).
If , then the eccentricity nonasymptotically decreases to 0 or may asymptotically decrease or increase to a limiting value, for exterior resonances. If , then the eccentricity evolution has a simple asymptotic behavior for interior resonances.
For the special case of the mean motion 1/1 resonance, the eccentricity asymptotically decreases to 0, for . If , then simple asymptotic behavior of the eccentricity exists.
For the case , the evolution of eccentricity of a particle captured in an exterior mean motion resonance is characterized by simple asymptotic behavior. Eccentricity nonasymptotically decreases to 0 in an interior resonance. The special case of the mean motion 1/1 resonance is characterized by an asymptotic decrease of eccentricity to 0.
We have not found eccentricity evolution characterized by two roots of the function W (e), for a dust particle under the action of electromagnetic and corpuscular radiation of the Sun in an exterior mean motion resonance with a planet in the Solar System.
The values of , and numbers pand q determine types of eccentricity evolution. The value of is:
 i)
 an increasing function of mass of a star and particle's radius and mass density,
 ii)
 a decreasing function of stellar wind speed, mass and concentration
of the stellar wind particles, and
 iii)
 an increasing or a decreasing function of luminosity of the star and particle's dimensionless efficiency factor of radiation pressure.
Acknowledgements
The authors would like to thank the anonymous reviewer for fruitful comments. The paper was supported by the Scientific Grant Agency VEGA grant No. 2/0016/09 and by the Comenius University grants UK/405/2009.
Appendix A: Exterior mean motion resonances 
We will show how the value of the root
depends on
.
We calculate derivatives of the functions
X (e) and Y (e) with respect to the eccentricity
A.1
According to Eq. (9), W (e) is a decreasing function of eccentricity, for . Derivatives of the functions X (e) and Y (e)fulfill d and . Thus, the functions X (e) and Y (e) are decreasing functions of eccentricity.
Inserting e_{x} (given by Eq. (14)) into the function W (e), we obtain W (e_{x}) > 0. The statement follows from the inequality Eq. (12). This means that must be greater than e_{x}, since the function W (e) is a decreasing function of eccentricity. If we assume that eccentricity is greater than e_{x} and less than , then X (e) < 0 and W (e) = X (e)  Y (e)> 0, thus Y (e) > 0. Both X (e) and Y (e) decrease with increasing eccentricity. A positive value of Y (e) is proportional to . If we decrease the ratio , then the value of X (e) < 0 must decrease more rapidly in order to reach the condition . If X (e) and Y (e) approach such values that , then the eccentricity e approaches . The condition will be fulfilled since and (only decreasing X (e) and Y (e) is not sufficient to fulfill this condition). Thus, will be a decreasing function of .
A.2 0 1
Derivatives of functions X (e) and Y (e) with respect to eccentricity are d and d (see Eqs. (A.1) and (A.2)). Thus, the functions X (e) and Y (e) are decreasing functions of eccentricity. It is easy to show that dX/d for all e (0, 1), if .
Inserting e_{x} into the function W (e), for the case , we obtain W (e_{x}) < 0. This means that must be smaller than e_{x}, since the function W (e) is a decreasing function of eccentricity. If we assume that eccentricity is greater than and less than e_{x}, then X (e) > 0 and Y (e) > 0. We have also W (e) = X (e)  Y (e) < 0, i.e. X (e) < Y (e). X (e) increases faster than Y (e) for decreasing e. If X (e) and Y (e) approach such values that , then the eccentricity e approaches . The value of Y (e) is proportional to . The greater the more rapid an increase of X (e) is necessary in order to reach the condition X (e)Y (e) 0. Thus, is a decreasing function of . If the value of increases from 0 to , then the value of decreases from e_{x} to 0.
Appendix B: Interior mean motion resonances 
The root was derived for . Derivatives of the functions X (e) and Y (e) are d and d (see Eqs. (A.1) and (A.2)). Thus, the functions X (e) and Y (e) are decreasing functions of eccentricity.
If , inequalities X (e) < 0 and Y (e) < 0 hold for the case of the interior resonances. If the initial eccentricity is smaller than , then W (e) > 0, and thus  X (e) <  Y (e). If the inequality represented by Eq. (18) is fulfilled, then the function X (e) increases faster than the function Y (e), with an increasing eccentricity (see Eqs. (A.1) and (A.2)). This is necessary in order to reach the condition X (e)  Y (e) 0. The value of Y (e) is proportional to , and, thus, is an increasing function of .
References
 Bahcall, J. N. 2002, Phys. Rev. C, 65, 025801 [NASA ADS] [CrossRef] (In the text)
 Beaugé, C., & FerrazMello, S. 1994, Icarus, 110, 239 [NASA ADS] [CrossRef] (In the text)
 Brownlee, D. E. 1994, Nature, 369, 706 [NASA ADS] [CrossRef]
 Bruno, R., Carbone, V., SorrisoValvo, L., & Bavassano, B. 2003, J. Geophys. Res., 108(A3), 1130 (In the text)
 Chauvin, G., Lagrange, A.M., Zuckerman, B., et al. 2005, A&A, 438, L29 [NASA ADS] [CrossRef] [EDP Sciences] (In the text)
 Dermott, S. F., Jayaraman, S., Xu, Y. L., Gustafson, B. A. S., & Liou, J. C. 1994, Nature, 369, 719 [NASA ADS] [CrossRef] (In the text)
 Dermott, S. F., Grogan, K., Durda, D. D., et al. 2001, in Interplanetary Dust, ed. E. Grün, B. A. S. Gustafson, S. F. Dermott, & H. Fechtig (Berlin: SpringerVerlag), 569 (In the text)
 Dohnanyi, J. S. 1978, Particle dynamics, in Cosmic Dust, ed. J. A. M. McDonnell (WileyInterscience, Chichester), 527 (In the text)
 Grün, E. 2007, Solar System Dust, in Encyclopedia of the Solar System, ed. L.A. McFadden, P. R. Weissman, & T. V. Johnson 2nd edn. (San Diego: Academic PressElsevier Inc.), 621 (In the text)
 Jackson, A. A., & Zook, H. A. 1989, Nature, 337, 629 [NASA ADS] [CrossRef] (In the text)
 Klacka, J. 1994, Earth Moon Planets, 64, 125 [NASA ADS] [CrossRef] (In the text)
 Klacka, J. 2008a [arXiv:0807.2795] (In the text)
 Klacka, J. 2008b [arXiv:0807.2915]
 Klacka, J., & Saniga, M. 1993, Earth Moon Planets, 60, 23 [NASA ADS] [CrossRef] (In the text)
 Klacka, J., Petrzala, J., Pástor, P., & Kómar, L. 2009 [arXiv:0904.0368] (In the text)
 Klacka, J., Kómar, L., Pástor, P., & Petrzala, J. 2008, A&A, 489, 787 [NASA ADS] [CrossRef] [EDP Sciences]
 Klacka, J., & Pástor, P. 2004 [arXiv:astroph/0411691] (In the text)
 Kuchner, M. J., & Holman, M. J. 2003, ApJ, 588, 1110 [NASA ADS] [CrossRef] (In the text)
 Lafreniere, D., Jayawardhana, R., & van Kerkwijk, M. H. 2008, ApJL, submitted [arXiv:0809.1424] (In the text)
 Leinert, Ch., & Grün, E. 1990, Interplanetary dust, in Physics of the Inner Heliosphere I, ed. R. Schwen, & E. Marsch (Berlin: SpringerVerlag), 207 (In the text)
 Liou, J.Ch., & Zook, H. A. 1997, Icarus, 128, 354 [NASA ADS] [CrossRef] (In the text)
 Liou, J.Ch., & Zook, H. A. 1999, AJ, 118, 580 [NASA ADS] [CrossRef] (In the text)
 Liou, J.Ch., Zook, H. A., & Jackson, A. A. 1995, Icarus, 116, 186 [NASA ADS] [CrossRef] (In the text)
 Murray, C. D., & Dermott, S. F. 1999, Solar System Dynamics (New York: Cambridge Univ. Press) (In the text)
 Neuhäuser, R., Guenther, E. W., & Wuchterl, G., et al. 2005, A&A, 435, L13 [NASA ADS] [CrossRef] [EDP Sciences]
 Parker, E. N. 1958, ApJ, 128, 664 [NASA ADS] [CrossRef] (In the text)
 Pástor, P., Klacka, J., & Kómar, L. 2009, Cel. Mech. and Dynam. Astron., 103, 343 [NASA ADS] [CrossRef]
 Poynting, J. M. 1903, MNRAS , 64, A 1 (In the text)
 Reach, W. T., Franz, B. A., & Welland, et al. 1995, Nature, 374, 521 [NASA ADS] [CrossRef] (In the text)
 Robertson, H. P. 1937, MNRAS, 97, 423 [NASA ADS] (In the text)
 Seperuelo, E., Alencar, S. H. P., Batalha, C., & Lopes, D. 2008, A&A, 489, 349 [NASA ADS] [CrossRef] [EDP Sciences] (In the text)
 Sidlichovský, M., & Nesvorný, D. 1994, A&A, 289, 972 [NASA ADS] (In the text)
 Weidenschilling, S. J., & Jackson, A. A. 1993, Icarus, 104, 244 [NASA ADS] [CrossRef] (In the text)
 Whipple, F. L. 1955, ApJ, 121, 750 [NASA ADS] [CrossRef] (In the text)
 Wyatt, S. P., & Whipple, F. L. 1950, ApJ, 111, 134 [NASA ADS] [CrossRef] (In the text)
All Tables
Table 1: Values of (in degrees) for various exterior and interior resonances with a planet in a circular orbit of radius a_{P}= 30.058 AU. The particle is characterized by and the solar wind by and u = 400 km s^{1}.
All Figures
Figure 1: The function W (e) for exterior mean motion 4/3 resonance. Various values of are used. 

Open with DEXTER  
In the text 
Figure 2: The function W (e) for interior mean motion 2/3 resonance for various values of . 

Open with DEXTER  
In the text 
Figure 3: The function W (e) for mean motion 1/1 resonance for various values of . 

Open with DEXTER  
In the text 
Figure 4: Evolution of eccentricity obtained from Eq. (7). A dust particle with and is captured in the exterior mean motion 4/3 orbital resonance with a planet of semimajor axis a_{P}=30.058 AU and eccentricity e_{P}= 0. Solar wind parameter . Evolution curve for various initial conditions of eccentricity are shown. 

Open with DEXTER  
In the text 
Figure 5: Evolution of eccentricity obtained from Eq. (7). A dust particle with and is captured in the exterior mean motion 4/3 orbital resonance with a planet of semimajor axis a_{P}= 30.058 AU and eccentricity e_{P}= 0. The solar wind parameter . 

Open with DEXTER  
In the text 
Figure 6: Evolution of eccentricity of a dust particle with and captured in the exterior mean motion 5/4 orbital resonance with a planet of semimajor axis a_{P}= 80 AU and eccentricity e_{P}= 0. Solar wind parameter . Evolution curves for various initial eccentricity are shown. 

Open with DEXTER  
In the text 
Figure 7: Orbital evolution of a spherical dust particle with and captured in the exterior mean motion 5/4 resonance with a planet of mass m_{P} = 20 in a circular orbit with a semimajor axis a_{P} = 80 AU. Solar wind parameter . 

Open with DEXTER  
In the text 
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