Stability of gravitationally-bound many-body systems

Rubčić, Antun and Rubčić, Jasna (1995) Stability of gravitationally-bound many-body systems. Fizika B, 4 (1). pp. 11-28. ISSN 1330-0016

PDF - Published Version
Language: English

Download (459kB) | Preview


The semimajor axes of planetary orbits and of major satellites of the planets in the solar system are described by a simple parabolic law, r_n = const×n^2, where n is an integer. The orbital periods T_n are proportional to n_3 , thus obeying the third Kepler's law. The radical change, compared with the previous approaches, is that n = 1 is assigned to all terrestrial planets, n = 2 to Jupiter, etc. This is strongly suggested by the analysis of astronomical data. Hence, terrestrial planets are considered as a subgroup of Jovian planets, and have been formed between the Sun and Jupiter in place of one giant planet of the Jovian group. The reason seems to be the temperature limit of about 200 K, corresponding to a distance of about 5×10^11 ^m (3.4 a.u.), that causes similar consequences as the well-known Roche limit for satellites of a planet. Relationships for r^n, T_n and other relevant quantities, which also depend on the integer n, are related to the discretization of angular momentum per unit mass of orbiting body. The mass of a central body appears as a scaling factor giving a unique approach to all systems. The mean deviation of observed orbital radii from the parabolic law for r_n is from 3.5% to 7.6% , depending on the system. On the basis of the analysis, we propose the hypotheses on stability of gravitationally-bound many-body systems.

Item Type: Article
Date: 1995
Subjects: NATURAL SCIENCES > Physics
Divisions: Faculty of Science > Department of Physics
Publisher: Hrvatsko fizikalno društvo
Depositing User: Gordana Stubičan Ladešić
Date Deposited: 09 Mar 2014 09:25
Last Modified: 09 Mar 2014 09:25

Actions (login required)

View Item View Item

Nema podataka za dohvacanje citata