The Tunguska 1908 Explosion’s Region as an International Park of Studies of the Ecological Consequences of Collisions of the Earth with the Solar System Small Bodies

There are different ways of estimating the distortions that help us find the best cartographic projections and recommend them for a specific range of tasks from mapping the Earth to extraterrestrial mapping. Besides the planets and their satellites there are small bodies in the Solar System. For mapping these bodies it is advisable to use morphographic projections to show their non-spherical shape. These projections were developed by Philip Stooke. He also proposed replacement of a regular reference surface with a phoboid and methods for estimating distortions but practically implemented them on the example of a body with a regular shape approximated by test triaxial ellipsoid with a ratio of axes 4:3:2. In this regard we set the task of developing and implementing the method for determining distortions in morphographic projections for a body with an irregular shape. We used the algorithm of comparison cartographic cell on projection and on phoboid in order to estimate distortion. The object of mapping is Phobos, a satellite of Mars. Phobos is a non-spherical celestial body for which morphographic projections were first applied. Comparing our results by the values of distortions with the results obtained by Philip Stooke we can conclude that using morphographic projections makes less distortion at portraying a phoboid than a test triaxial ellipsoid.

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On secular resonances of small bodies in the planetary systems

Proceedings of the International Astronomical Union ◽

10.1017/s1743921307003092 ◽

2006 ◽

Vol 2 (S236) ◽

pp. 77-84

Author(s):

Jianghui Ji ◽

L. Liu ◽

G. Y. Li

Keyword(s):

Solar System ◽

Planetary System ◽

Planetary Systems ◽

Giant Planets ◽

Small Bodies ◽

Secular Resonances ◽

Mean Motion Resonances ◽

The Earth ◽

Habitable Zones ◽

Earth Like Planets

AbstractWe investigate the secular resonances for massless small bodies and Earth-like planets in several planetary systems. We further compare the results with those of Solar System. For example, in the GJ 876 planetary system, we show that the secular resonances ν1 and ν2 (respectively, resulting from the inner and outer giant planets) can excite the eccentricities of the Earth-like planets with orbits 0.21≤ a <0.50 AU and eject them out of the system in a short timescale. However, in a dynamical sense, the potential zones for the existence of Earth-like planets are in the area 0.50≤ a ≤1.00 AU, and there exist all stable orbits last up to 105 yr with low eccentricities. For other systems, e.g., 47 UMa, we also show that the Habitable Zones for Earth-like planets are related to both secular resonances and mean motion resonances in the systems.

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The IMPACTON Project: Pole and Shape of Eight Near-Earth Asteroids

Proceedings of the International Astronomical Union ◽

10.1017/s1743921315008637 ◽

2015 ◽

Vol 10 (S318) ◽

pp. 181-184

Author(s):

José Sergio Silva ◽

Daniela Lazzaro ◽

Teresinha Rodrigues ◽

Jorge Márcio Carvano ◽

Fernando Roig ◽

...

Keyword(s):

Solar System ◽

Complex Problem ◽

Inversion Method ◽

Rotational Period ◽

Small Bodies ◽

Formation And Evolution ◽

Set Up ◽

Earth Orbits ◽

Near Earth Asteroids ◽

Solar System Small Bodies

AbstractThe formation and evolution of Solar System small bodies, in particular those in near-Earth orbits, is a complex problem which solution strongly depends on a better knowledge of their physical properties. To contribute to the international efforts in this direction the IMPACTON project (www.on.br/IMPACTON) set up a dedicated facility denominated Observatório Astronômico do Sertão de Itaparica (OASI). Using the 1-m telescope several dozens of NEAs were observed between March 2012 and October 2014. Here we will present the results obtained for 8 objects. Relative magnitudes were used to obtain lightcurves and derive rotational periods. Applying the inversion method developed by Kaasalainen and Torppa (2001) and Kaasalainen et al. (2001), along with lightcurves from literature, allowed to refine the rotational period of these asteroids as well as to derive their pole direction and shape. The obtained results confirm a lack of poles toward the ecliptic and with a majority of retrograde rotators. A more representative sample, however, is needed in order to drive robust conclusions.

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