Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufm.p51a1190l&link_type=abstract
American Geophysical Union, Fall Meeting 2006, abstract #P51A-1190
Astronomy and Astrophysics
Astrophysics
6200 Planetary Sciences: Solar System Objects, 7500 Solar Physics, Astrophysics, And Astronomy, 7504 Celestial Mechanics, 7537 Solar And Stellar Variability (1650), 7539 Stellar Astronomy
Scientific paper
The planetary orbits are not stable and increase with time. For the beginning of the solar systems, all planets were closer to the Sun, and will be more distant in the future. The cause is the relative instability of the planetary orbits and solar mass loss by radiation and solar wind. The potential energy of planetary orbits relative to the solar escape energy (escape velocity) determines the stability of planetary orbits. Using fundamental physical concepts, the planetary potential energy relative to the solar surface was obtained by calculating the launch energy (~ launch velocity) that is necessary to move an object from the solar surface to the planetary orbit (`planetary launch velocity'). The launch energy is equal to the planetary potential energy relative to the solar surface. The planetary launch velocities range from 613.830 (Mercury) to 617.526 km/s (Pluto). The difference between solar escape velocity (617.547km /s) and planetary launch speeds ranges from 3.7km/s (Mercury) to 0.037 km/s (Pluto)which responds to 0.6 and 0.006 percent of escape speed. Because of solar radiative and solar wind mass (~gravity) loss, the gravitational interaction between Sun and planets decreases with time. This reduces the solar escape velocity, while the planetary orbital potential energy is invariant. Changes of planetary orbits with time were calculated based on the solar mass-loss rate constant. At the beginning of the solar system (-4.5byrs), the planetary orbits were closer to the sun, and orbital periods were shorter. For example, the orbits of Mercury and Pluto at -4.5Byr were 5.61E+07 and 1.47E+06 Km (presently 5.80E+07, 10.2E+09), and the orbital periods were 0.23 and 26.4 yr (0.24 and 248.4 yr). These original orbits must be used for the formation of the solar system. The orbits are expanding with time and orbital periods are increasing. The planets will escape the solar system when the solar escape velocity decreases below the planetary potential energy (launch velocity). The planetary escape time is calculated for the current solar mass loss rate, e.g., 1.3 and 0.76 billion years for Pluto and UB313, respectively. Present orbital separation rates are obtained, which are within the range of experimental observation.
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