http://www.ta3.sk/~mjakubik/AstroDyn/INNER_OC_FORMATION/ ======================================================== This web page contains the initial (input) and the second part of resultant (output) data of the simulation of Oort cloud (OC) formation. The simulation covers the period from 1001 to 2000 mega-years of the OC formation. Its more detailed description can be found in the paper: Leto G., Jakubik M., Paulech T., Neslusan L., Dybczynski P.A.: 2008, "The structure of the inner Oort cloud from the simulation of its formation for two giga-years", in: Monthly Notices of the Royal Astronomical Society, submitted. (The first part of the output data can be found on the web page: http://www.ta3.sk/~ne/OUTER_OC_FORMATION/ linked to the paper: Dybczynski P.A., Leto G., Jakubik M., Paulech T., Neslusan L.: 2008, Astronomy & Astrophysics, submitted.) The animations of the evolution of some distributions characterizing the simulated process are provided, too. ----------------------------------------------------------------------- THE CONTENT OF THE ARCHIVE: (A) Input data: (A1) small0000.xyz - the initial rectangular coordinates and velocity vectors of the followed test particles (TPs). The structure of this file is identical to that for the corresponding output data (files "small&&&&.xyz"; see B2a). (A2) small0000.qew - the initial orbital elements of the followed TPs. The structure of this file is identical to that for the corresponding output data (files "small&&&&.qew"; see B2b). (A3) jupiter.lst, saturn.lst, uranus.lst, neptune.lst, kbelt.lst - the lists of the TPs initially residing in the Jupiter, Saturn, Uranus, Neptune, and Kuiper-belt region, respectively, of the initial proto-planetary disc. (B) Output data: (B1) decompress.sh - OS-Linux-based script for the complete decompresion of all output data (see B2) into the common subdirectory TPS_DATA (the directory must not exist before the script is run; by command: sh decompress.sh or ./decompress.sh). (B2) res####_$$$$.tgz - the archive of output data archives for the period ranging from #### to $$$$ Myr. After its decompression (command: tar xzvf res####_$$$$.tgz), subdirectory RES####_$$$$/ is created and following archives occur inside it: (B2a) xyz@@@@_****.tgz - zipped TAR archive of the rectangular position and velocity coordinates of the integrated test particles (TPs) being in the integration region, at least for a while, during the integration period spanning from @@@@ to **** (in Myr). After a decompression (command: tar xzvf xyz@@@@_****.tgz), the files -- "small&&&&.xyz" will occur. Symbol &&&& indicates the time in Myr, for which the coordinates are given. The data about each TP are written in three lines. The structure of these lines is following: 1st line: identification string of the TP, epoch for which the data are given (in days from the beginning of the simulation; it corresponds to &&&&); 2nd line: rectangular coordinates X, Y, Z of the TP in AU; 3rd line: components of the velocity vector VX, VY, VZ of the TP in AU/day (both vectors are referred to the modified galactic heliocentric coordinate system). (B2b) qew@@@@_****.tgz - zipped TAR archive of the orbital elements of the TPs being in the integration region. After a decompression, the files -- "small&&&&.qew" will occur. Symbol &&&& indicates again the time, in Myr, for which the orbital elements are given. In days, this epoch is also given in the first line of the "small&&&&.qew" file. The data about the TPs are written in further lines, one line for a given TP. This line contains: perihelion distance, q [AU]; eccentricity, e; argument of perihelion, omega [deg]; longitude of ascending node, Omega [deg]; inclination, i [deg]; identification code of the given TP. The angular elements are referred to the modified galactic heliocentric coordinate system. (B2c) col@@@@_****.tgz - zipped TAR archive with the files -- "col&&&&.inf" containing information of which TPs collided with a massive body (Sun or planet) during the interval ranging from &&&&-1 to &&&& Myr. In a particular line, the code of a given TP is followed by information of which massive body was hit. (B2d) eje@@@@_****.tgz - zipped TAR archive with the files -- "eje&&&&.inf" containing the names of TPs, which were ejected into the interstellar space during the interval ranging from &&&&-1 to &&&& Myr. (C) Animations: - the individual animations show the distributions plotted in Figs. 3-12 in the paper (Leto et al., 2008); while the plots in these figures illustrate the state in 2 Gyr (or also for few other times), the animations show their evolution during the entire studied period of 2 Gyr, with the snapshots of every Myr. - all the animations are provided in "avi" format (C1) fig03.avi - the 2-Gyr evolution of the comet population moved into the inner OC from the Jupiter, Saturn, Uranus, Neptune, and Kuiper-belt regions. The green bars illustrate the numbers of bodies in 0.5-AU-wide intervals of the initial proto-planetary disc, which reside in the inner OC at the just shown time. The red bars do so for the bodies occuring in the inner OC, at least for a short period, whenever from the beginning of the simulation to the just shown time. (C2) fig04.avi - the 2-Gyr evolution of the cumulative distribution of bodies in the region of heliocentric distance from 100 to 100,000 AU (in the logarithmic scale). (C3) fig05.avi - the 2-Gyr evolution of the heliocentric distance distribution of the OC comets (crosshatched bars). The same distribution of all comets, still bound to the Sun, is also shown (empty bars). In the region of heliocentric distance r < 10,000 AU, the distribution of all comets is outside of the chosen vertical scale because of a better transparency of the OC-comet distribution. If all comets in the given interval are in the OC, the crosshatched bar overlaps the entire empty bar, which is not visible in this interval, then. (C4) fig06.avi - the 2-Gyr evolution of the orbital semi-major axis distribution of bodies residing in the OC (crosshatched bars). The same distribution of all comets, still bound to the Sun, is also shown (empty bars). (C5) fig07.avi - the 2-Gyr evolution of the orbital eccentricity of bodies residing in the inner OC. (C6a) fig08a.avi - the 2-Gyr evolution of the inclination to the Galactic-Equator-plane distribution of bodies residing in the inner OC. (C6b) fig08b.avi - the 2-Gyr evolution of the inclination to the Ecliptic distribution of bodies residing in the inner OC. (C6c) fig08c.avi - the 2-Gyr evolution of the argument-of-perihelion distribution of bodies residing in the inner OC. The referrence frame is galactical. (C6d) fig08d.avi - the 2-Gyr evolution of the argument-of-perihelion distribution of bodies residing in the inner OC. The referrence frame is ecliptical. (C6e) fig08e.avi - the 2-Gyr evolution of the longitude-of-ascending- node distribution of bodies residing in the inner OC. The referrence frame is galactical. (C6f) fig08f.avi - the 2-Gyr evolution of the longitude-of-ascending- node distribution of bodies residing in the inner OC. The referrence frame is ecliptical. (C7a) fig09a.avi - the 2-Gyr evolution of the aphelion-point directional distribution of the bodies residing in the inner OC. The referrence frame is galactical. The green curve shows the position of the Ecliptic. (C7b) fig09b.avi - the 2-Gyr evolution of the aphelion-point directional distribution of the bodies residing in the inner OC. The referrence frame is ecliptical. The green curve shows the position of the Galactic Equator. (C8a) fig10a.avi - the 2-Gyr evolution of the inclination to the Galactic Equator of the bodies residing in the inner OC as the function of their semi-major axis. (C8b) fig10b.avi - the 2-Gyr evolution of the perihelion distance, "q", of the bodies residing in the inner OC as the function of their semi-major axis, "a". The "q-a" phase space above the green line is forbidden. (C8c) fig10c.avi - the 2-Gyr evolution of the argument of perihelion of bodies residing in the inner OC as the function of their semi-major axis. The referrence frame is galactical. (C8d) fig10d.avi - the 2-Gyr evolution of the longitude of ascending node of bodies residing in the inner OC as the function of their semi- major axis. The referrence frame is galactical. (C9a) fig11a.avi - the 2-Gyr evolution of the inclination to the Ecliptic vs. semi-major axis of bodies on the orbits with semi-major axis in the interval 50 < a < 22,000 AU. The bodies residing in a given time in the inner OC are shown with red-green asterisks, the other bodies with red crosses. (C9b) fig11b.avi - the 2-Gyr evolution of the inclination to the Ecliptic vs. semi-major axis of bodies on the orbits with semi-major axis in the interval 50 < a < 500 AU. (C10a) fig12a.avi - the 2-Gyr evolution of the ecliptical rectangular z-component vs. heliocentric distance, "r", of bodies being in the interval 50 < r < 25,000 AU. The bodies residing in a given time in the inner OC are shown with red-green asterisks, the other bodies with red crosses. Because of the obvious fact that "z" cannot be larger than "r", no point can occur above the green line. (C10b) fig12b.avi - the 2-Gyr evolution of the ecliptical rectangular z-component vs. heliocentric distance, "r", of the bodies being in the interval 50 < r < 5,000 AU. The bodies residing in a given time in the inner OC are shown with red-green asterisks, the other bodies with red crosses. No TP can occur above the green line. ========================================================================