Up: An algorithm for determining
Subsections
The algorithm is designed to work with two arbitrary elliptical orbits.
Due to its nature some classes of problem (i.e. objects in secular,
mean-motion and Kozai resonances, including extreme cases of
(e,
)-coupling) may be inappropriate for this approach. The
basic assumptions involved are:
- 1.
- each orbit has fixed semi-major-axis (a), eccentricity (e)
and inclination (i);
- 2.
- the rate of variation of the argument of perihelion (
)is greater than that of any of the other elements;
- 3.
- the variations of the respective arguments of perihelia are not
correlated.
In addition, we assume that the objects are of small size compared to
their orbits, and that there is no significant gravitational focusing.
The algorithm is readily extended to incorporate the latter, as we show
in Sect. 3.
Let us suppose that each orbit has semi-major axis, eccentricity and
inclination (a1, e1, i1) and (a2, e2, i2) respectively. The
longitudes of the ascending nodes (
respectively) are
assumed to be fixed, as are the inclinations, and hence so too is the
mutual inclination
of the two orbital planes. We allow the
arguments of perihelion of each object,
and
, to
take all possible values in the range (
). This defines a
two-dimensional phase space in which the differential collision
probability at each point,
, can be evaluated.
The total collision probability is then
|  |
(1) |
Over most of this phase space the collision probability
is zero because interactions can only occur when
the mutual nodes are sufficiently close. Without loss of generality the
coordinate system can be chosen so that the origin lies at the focus of
the two orbits, the (x,y)-plane coincides with the orbital plane of the
first orbit, and the x-axis lies along the line of intersection of the
two orbital planes (Fig. 1). In each case
and
are measured in the orbital plane from the mutual node.
![\begin{figure}
\includegraphics[width=8.5cm]{ds7564f1.eps}\end{figure}](/articles/aas/full/1998/21/ds7564/Timg10.gif) |
Figure 1:
Intersection of orbital planes, illustrating the mutual
inclination, , and the definition of the argument of
perihelion, , of one orbit measured with respect to the mutual
line of nodes |
In general, the heliocentric distances r of the ascending or descending
nodes are given by
|  |
(2) |
and collisions may occur at the ascending node when
|  |
(3) |
with a similar expression
|  |
(4) |
for collisions at the descending node. Choosing the ascending node and
replacing a(1-e2) with p, and solving for
we obtain:
|  |
(5) |
This relation takes the general form
|  |
(6) |
where
|  |
(7) |
and
|  |
(8) |
This can be differentiated to give
|  |
(9) |
Relations (6) through (8) and corresponding equations for
the descending node define the locus of the points in
-space where collisions may occur, illustrated
in Figure 2. Equation (9) is used to determine the tangent and
normal to this curve. We note that the curve is symmetrical on both axes,
so that looking at one point of intersection there are at most three
others with conjugate configurations.
![\begin{figure}
\includegraphics[angle=-90,width=8.5cm]{ds7564f2.eps}\end{figure}](/articles/aas/full/1998/21/ds7564/Timg22.gif) |
Figure 2:
The figure illustrates the symmetry of the solutions of
Eq. (6) in ( )-space for two typical pairs of
orbits. Each pair of orbits has two solutions. The first pair has
solutions denoted "1" and "2"; the second has solutions denoted "3" and
"4". In each case these correspond to an intersection at the ascending or
descending node. The important points to note are that (i) each solution
shows four-fold symmetry, and one can be obtained from the other; and
(ii) is always a monotonically increasing or decreasing
function of in the principal quadrant, depending on whether
the intersection occurs at the the ascending or descending node
respectively |
We emphasize that, due to the finite size of real objects, collisions
may occur not only on this curve but also in its immediate vicinity,
over a range
measured in the
-plane perpendicular to the curve of
intersection. For spherical particles
is proportional
to the combined radius of interaction R=R1+R2 of the two
bodies. Moreover, moving perpendicular to the curve of intersection,
it is straightforward to show that the differential collision
probability at a distance
from the collision point
is
, so the
differential collision probability integrated normal to the curve of
intersection is
.
The total collision probability is then calculated by integrating
along the curves of intersection, choosing small line elements of each
curve, determining their dimensions and summing their resulting
contributions to the total probability. The direction along each curve
of intersection is chosen using
from
Eq. (9). The stepping can be mirrored to allow for the
symmetry, but differing geometry (associated with the particles'
relative velocities at collision) means that P and
may be different for different mirrored points.
Determination of
and
requires a model of the encounter
geometry. We adopt a simple vector approach in which each body is
assumed to move at a constant velocity, denoted
and
respectively, during the close encounter. The respective vectors
(see Fig. 3) are determined using the classical formulae for
heliocentric elliptical motion (Roy 1988):
|  |
(10) |
where
and G is the gravitational constant, M is the mass
of the central body and m is the mass of the orbiting particle. If we
choose
, M=1 and m=0 we have:
|  |
(11) |
and for the angle
between the velocity and radius vectors at the
node
|  |
(12) |
(Note that
is measured from the mutual node, and that for
simplicity we have dropped subscripts 1 and 2 from
Eqs. (10)-(12).)
For the first orbit, which lies in the (x,y)-plane, the velocity vector
is (Fig. 3):
|  |
(13) |
and for the second, whose plane is inclined at an angle
to the
first, we have
|  |
(14) |
 |
Figure 3:
Diagram to illustrate the simplified vector encounter geometry
described in the text |
In order for a collision to take place, both particles must arrive at
the point of intersection of their respective orbits at the same
moment, within a small time interval
. We use
to
calculate the collision probability
at the
point
on the curve of intersection, and then use
the vectors
and
to evaluate the range
associated with this point on the curve.
Moving the origin of the coordinate system to the point at which the
two paths cross, the motion of the two particles near the mutual node
or collision point can be described by
|  |
(15) |
where
is the angle between the two position vectors
and
in the new frame. By replacing the maximum value of
impact parameter b which produces a collision, namely b=R where R
is the radius of interaction for both particles (i.e. R = R1
+ R2 for spheres of radius R1 and R2 respectively), we
calculate the maximum value of
, and hence obtain
using
|  |
(16) |
Since the temporal window for a collision is
per
revolution, the differential collision probability per unit time for
such intersecting orbits is
, where
and
denote the orbital periods of each particle.
We now determine the magnitude of the range
perpendicular to the curve of intersection. We define
to be
the vector that describes the relative motion of the two encounter
vectors as
and
are varied normal to the curve of
intersection, and introduce a separation parameter S, analogous to
the impact parameter b, whose value equals R at the extremum
. We thus have
|  |
(17) |
where
|  |
(18) |
and
and
denote the respective
variations of
and
perpendicular to the curve of
intersection, with
. Here, r
is the distance from the Sun where the interaction occurs.
Therefore
is simply calculated from
|  |
(19) |
and the total collision probability is evaluated by summing the values
of
along the curve of intersection in the
-plane for a
statistically sufficient number of points.
Up: An algorithm for determining
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