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AMPLE 3 òÀÔ Multi-purpose Software Package for Asteroids
and Comets
Dealing
with minor bodies of the Solar System one badly needs appropriate software tool
to plan and treat observations, to estimate parameters of selected groups, to
visualize orbital motion, and more. There are several tools of that kind that
scientific community has at its disposition, nevertheless we would like to
present the new one, AMPLE 3, having a number of merits.
The
AMPLE 3 software package does have profound background and reach experience
accumulated in its implementation. The very first version of AMPLE (Adaptable
Minor PLanet Ephemerides) package had been put forward in 1995. The package got
acknowledgement and respect within astronomical community due to its various
abilities and features. Abilities of the package are based on, among other
factors, high precision
elements of minor planets, annually published by the Institute of Applied
Astronomy. They are prepared with retention of full accuracy on the basis
of orbital elements of new minor planets and elements of improved orbits
monthly distributed by Minor Planet Center.
The last fifteen years have seen tremendous progress in both printed
version of minor planet ephemerides yearbook and accompanied software package
AMPLE. Numerous improvements were made in all parts of the package. Two
variants of the package were developed and put in use for specific tasks, i.e.,
Ample for Comets and MUSE.
The
very idea of the new version is to put all innovations together, and gain a
stand-alone, consistent, multi-purpose, cross-platform, robust, and easy to use
software package AMPLE 3.
AMPLE
3 is integrated software package to deal with a number of problems concerning
minor bodies of the Solar System. Among these problems are the following.
The
use case model of the AMPLE 3 package is presented in figure below. We put in
green features released in version 0.4 (December 2009).
What
are most important new features of the AMPLE 3 in comparison with previous
versions and clones? To put it in short these are five.
Every entity that could be considered
as a parameter is really the parameter in the AMPLE 3 and could be reset if
needed. It could be done by editing XML files with configuration information.
For example, we can alter definitions of families and groups as it is shown in
the Elem.xml file
below. One may edit this xml file on his own responsibility.
To
make the package do something one have to put the task with standard dialog.
All forms for all use cases look alike. The prototype form is shown below.
User
has to put parameters of the task one by one in several tabs at the right, and the
resulting task appears at the left. To run the current task user has to press
Run button, to give it up òÀÓ Cancel button, to save it òÀÓ Save As button, to
restore saved one òÀÓ Load button, and to set default task one has to press
Default button. Make note that Asteroids and Comets check boxes could be checked
or unchecked independently any time.
The list of minor planet names/preliminary
designations, osculating orbital elements, and photometric parameters used in
AMPLE 3 contains data on numbered minor planets for some standard epoch lying
within the title year of the package. The data base includes 204962 asteroids
numbered as of January 2009 and 217 short-periodic comets. Their elements were
calculated on 2010 July 23.0 TT. Orbital elements of comets and parameters of
nongravitational acceleration A1 , A2 and A3 have been improved by program
developed in Institute of Applied Astronomy of RAS.
Present section of the package enables one:
ˆ§
to
make selection out of the total number of minor planets in accordance with the
restrictions imposed on some element or on a variety of elements;
ˆ§
to
sort the obtained selection in order of ascending or descending value of any
element;
ˆ§
to
draw the histogram of element distribution for obtained selection;
ˆ§
to
construct dotty picture of minor planet distribution in two- or three-dimension
space of elements.
Following designations of elements/ parameters are used
in AMPLE 3.
H òÀÔ photometric parameter, absolute magnitude in V band
G òÀÔ photometric parameter, so called slope parameter
M òÀÔ mean anomaly
Peri òÀÔ argument of perihelion
Node òÀÔ longitude of ascending node
i òÀÔ inclination
e òÀÔ eccentricity
n òÀÔ mean motion
a òÀÔ semi-major axis.
The angular quantities are expressed in degrees,
n òÀÔ in degrees per day,
a òÀÔ in astronomical units (AU).
Apart conventional orbital elements AMPLE gives
possibility to calculate for each minor planet the following often used
functions:
q = a(1òÀÓe) òÀÔ
perihelion distance
Q = a(1+e) òÀÔ
aphelion distance
p = a(1òÀÓe2)
òÀÔ orbital parameter
P = a 3/2 òÀÔ period of revolution in years
T òÀÔ moment of perihelion passage
Peri+ Node òÀÔ longitude of perihelion
L = Peri+ Node + M òÀÔ mean longitude
n"= nºç3600 òÀÔ mean motion in arcsec/day
dist_ascNode = a(1òÀÓe2)/(1+ecos(Peri)) òÀÔ heliocentric distance of ascending node
dist_dscNode = a(1òÀÓe2)/(1òÀÓecos(Peri))
òÀÔ heliocentric distance of descending node
MOID òÀÔ Minimum Orbit Intersection Distance
CT òÀÔ Tisserand criterion
Dphot òÀÔ photometric diameter
To calculate MOID or CT user should put name or number
of major or minor planet through dialog.
To gain access to the table of elements press ˆàˆàElements
button. Select elements dialog appears (see below). To set constraints on
elements choose element, enter values and press Put button. User may select
types, groups and families of minor bodies in one click on appropriate
checkbox. User may use prepared file with names and numbers of objects also.
All subselections are united with logical OR (disjunction). Header tab allows one
to chose elements to be shown in the table, no matter what elements are used in
constraints. Task description panel shows current task. To run task user should
press Run button.
Table of elements for selected bodies appears.
The distribution of elements can
be visualized in different ways. See examples below.
To create task for visualization of orbital motion press
Orbits button . Orbits visualization dialog appears (see below). To
choose the set of objects to be visualized user may:
ˆ§
click checkbox for
major planets;
ˆ§
input name or
number of minor bodies;
ˆ§
fill special form
with parameters for arbitrary noncatalogued object.
To set interval of visualization choose start and end
dates. Swarm tab allows to choose large amount of bodies in the same manner as
in Elements dialog. Method tab allows to choose the method of calculating
coordinates of bodies: by unperturbed elements of orbits, or by nodes, or by
numerical integration. Approaches tab allows one to define pair of objects,
which approaching is wanted to observe.
Task description panel shows current task. To run task
user should press Run button.
Result
for task Orbits for example can be like below one.
Left hand
side panel allows to:
ˆ§
change
color palette;
ˆ§
start,
stop, suspend and resume motion visualization;
ˆ§
show
or hide names, planet spheres and elliptic orbits;
ˆ§
change
step and thus speed of motion visualization;
ˆ§
see
current time of motion visualization;
ˆ§
depict
line of nodes for selected object;
ˆ§
change
view point in several ways;
ˆ§
print
or save current picture.
Moreover,
package shows special graphical effect (color blinking), when approaching
of two objects takes place. The distance between bodies where the effects is
triggered is set in Approaches tab. The minimum distance and the instance when
it is attained are shown in Task info panel.
ˆé Institute
of Applied Astronomy RAS 2009-2010
E-mails:
shor@ipa.nw.ru,
fedornovikov@rambler.ru
Mail:
Institute of Applied Astronomy, naberezhnaya Kutuzova, 10, Saint Petersburg, 191187,
Russia
FAX: +7-812-275-11-19