Abstract
The scenario for the origin and evolution of planetary systems (and in particular, the solar system) is based on fundamental theoretical concepts and astrophysical data involving the process of star formation. Mechanical and cosmochemical properties of the solar system through radioisotope dating place important constraints on such a scenario. The sequence of events includes formation of a protoplanetary gas-dust accretion disk around a parent star from a primordial nebula, followed by disk instability and fragmentation into the first solid bodies (planetesimals), and their collisional interactions giving rise eventually to planets.
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- 1.
Jeans instability occurs when the internal gas pressure is not strong enough to prevent gravitational collapse of a region filled with gas-dust matter.
- 2.
Depending on the spectral energy distribution in the protostar and surrounding disk due to a change in the distribution of masses, velocities, and temperatures, classes I and II are also distinguished (see below).
- 3.
An example of a stellar system with a debris disk and with no observable planets is Tau Ceti, while a system with both a debris disk and cold planets is Epsilon Eridani. Our solar system belongs to the systems with gaseous cold giants at r >> 0.1 AU, in contrast to the systems with hot gaseous giants at r < 0.1 AU (see Chap. 7).
- 4.
Note that the accretion rate from the disk onto the protostar (M·) can be a factor of 3–4 lower than that from the envelope onto the disk (M·d) due to the mass loss in the protostellar flows/winds.
- 5.
Eucrites are a group of achondrite class meteorites enriched with calcium; they are also referred to as basaltic achondrites.
- 6.
Some chondrules were likely formed during local heating caused by impact processes.
- 7.
This is regarded as a sort of Boltzmann kinetic equation when dealing with coagulation processes.
- 8.
It was also supposed that these jets, in combination with emitted radiation and/or radiation from nearby massive stars, may help to drive away the surrounding cloud from which the star was formed.
- 9.
KOI is the acronym for Kepler Object of Interest.
- 10.
Gliese means that a star is taken from the Gliese Catalogue listing stars within 25 pc from Earth.
- 11.
The Roche lobe is the radial distance from a planet where tidal forces exceed internal forces holding a solid body together, and it can be destroyed within this limit.
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Marov, M.Y. (2015). Planetary Systems: Origin and Evolution. In: The Fundamentals of Modern Astrophysics. Springer, New York, NY. https://doi.org/10.1007/978-1-4614-8730-2_8
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DOI: https://doi.org/10.1007/978-1-4614-8730-2_8
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