Abstract
How our planet was formed, how life came about, and whether life exists elsewhere in the universe are among some of the long-standing questions in human history. The latter, which has been the main drive behind many decades of searching for planets outside the solar system, is one of the most outstanding problems in planetary science and astrobiology. Although no Earth-like planet has yet been found, the success of observational techniques in identifying now more than 350 extrasolar planets has greatly contributed to addressing this question, and has extended the concept of habitability to billions of miles beyond the boundaries of our solar system. It is now certain that our planetary system is not unique and many terrestrial-size planets may exist throughout the universe.
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Notes
- 1.
The phrase “binary-planetary system” is used to identify binary star systems in which one of the stars is host to a giant planet.
- 2.
An earlier classification by Szebehely (1980) divides the planetary orbits in binary systems into three categories: inner orbit, where the planet orbits the primary star, satellite orbit, where it orbits the secondary star, and the outer orbit, where the planet orbits the entire binary system.
- 3.
In an elliptical restricted three-body problem, the planet is considered to be a massless particle and its motion is studied in the gravitational field of two massive stars. The stars of the binary revolve around their center of mass in an unperturbed elliptical Keplerian orbit.
- 4.
Orbits with semimajor axes smaller than the lower value or larger than the upper value are certainly unstable.
- 5.
Test-computations for μ = 0. 3, 0. 5 and 0.7, up to 100,000 time units showed the same qualitative results.
- 6.
- 7.
The influence zone of a planetary object with a mass m p around a star with a mass M is defined as the region between 3R H − a p (1 − e p ) and 3R H + a p (1 + e p ), where a p and e p are the semimajor axis and eccentricity of the planet, and R H = a p (1 − e p )(m p ∕ 3M)1 ∕ 3 is its Hill radius.
- 8.
For colliding bodies with different sizes, depending on the size distribution of small objects, and the radius of each individual planetesimal, the process of the alignment of periastra may instead increase the relative velocities of the two objects, and cause their collisions to become eroding (Thébault et al. 2006).
- 9.
It is important to emphasize that the delivery of water to the inner part of the solar system might not have been entirely due to the radial mixing of planetary embryos. Smaller objects such as planetesimals in the outer region of the asteroid belt, and comets originating in the outer solar system, might have also contributed Raymond et al. (2007).
- 10.
It is, also, important to note that, because the stellar luminosity, and therefore the location of the habitable zone, are sensitive to stellar mass (Kasting et al. 1993; Raymond et al. 2007), the minimum binary separation necessary to ensure habitable planet formation will vary significantly with the mass of the primary star.
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Haghighipour, N., Dvorak, R., Pilat-Lohinger, E. (2010). Planetary Dynamics and Habitable Planet Formation in Binary Star Systems. In: Haghighipour, N. (eds) Planets in Binary Star Systems. Astrophysics and Space Science Library, vol 366. Springer, Dordrecht. https://doi.org/10.1007/978-90-481-8687-7_11
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