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Extrasolar Planetary Systems

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The Earth as a Distant Planet

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Abstract

The stability of a planet depends not only on its physical properties or distance to the star, but also on the configuration of the planetary system where it was born. A unique process, gravitational collapse of a molecular cloud, can give rise to different planetary systems. The detailed configuration of this cloud, such as its mass, rotation and metallicity, will give the genetic print of the newborn system, conditioning the destiny of the different planets. Following this biological approach, the gravitational interactions between the different components during the first phase of the evolution of the system will let only the fittest, the stablest, to survive.

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Notes

  1. 1.

    A type of interstellar cloud, cool and dense enough to allow for the formation of molecules.

  2. 2.

    From the Arabic ‘Fun al Hut’ (the fish mouth), it is also known as HD216956 and alpha-Piscis Austrini, a 200-Ma-old A3 star located at a distance of 22light years.

  3. 3.

    For a complete list of the orbital elements of the planets of the Solar System, see http://ssd.jpl.nasa.gov

  4. 4.

    It was preceded, in November 1684, by a short manuscript entitled De motu corporum in gyrum (On the motion of bodies in an orbit), sent by Newton to E. Halley, who later edited the Principia.

  5. 5.

    r is the distance between the orbiting body and the central body, and θ the direction of the orbiting body, the true anomaly.

  6. 6.

    The third body has a mass small enough that it does not influence other objects, which are usually assumed to be in circular orbits. Our Solar System can be separated into several subsystems of this kind (e.g. Sun-planet-satellite, Sun-planet-asteroid etc.), making the numerical solution more accurate.

  7. 7.

    There were some important errors in the calculations of Adams and Leverrier. Following the Titius–Bode law, they estimated the distance Neptune–Sun at 38AU. Fortunately, between 1790 and 1850, Uranus and Neptune were in conjunction (aligned with the Sun on the same side of the planetary system), and this helped to minimize errors.

  8. 8.

    In fact, Galileo first observed Neptune on 28 December 1612 and 28 January 1613, but he believed it to be a fixed star (Kowal and Drake 1980).

  9. 9.

    It first appeared as an introduction to the third edition of his Théorie Analytique des Probabilitiés, which was originally published in 1812. There is an English version of the complete essay published by Dover in 1951.

  10. 10.

    The jury members for the competition were K. Weierstrass (1815–1897), G. Mittag-Leffler (1846–1927) and C. Hermite (1822–1901), who awarded him the prize.

  11. 11.

    English version by D. Goroff (1993) published by the American Institute of Physics and reprinted by Springer in 2007.

  12. 12.

    English translation: Science and Method, Lancaster, PA: Science Press 1913.

  13. 13.

    Excess depletion of asteroids both on the inner edge of the belt and in the outer edges of each Kirkwood gap.

  14. 14.

    Cruithne was discovered on 10 October 1986 by Duncan Waldron on a photographic plate taken with the UK Schmidt Telescope at Siding Spring Observatory, Australia. It is approximately 5km in diameter.

  15. 15.

    Discovered on 9 January 2002 has a diameter of about 40–100m.

  16. 16.

    Such is the case with the ESA/NASA satellite SOHO, observing the Sun since 1995.

  17. 17.

    Valid for the Solar System, corresponds to a disk with Σ 1=10 and α=3∕2.

  18. 18.

    A torque is a measure of how much a force acting on an object causes the object to rotate.

  19. 19.

    This study investigates orbital stability numerically within the elliptic restricted three-body problem. That is, the planets are modelled as test particles moving in the gravitational field of a pair of stars on fixed eccentric orbits about each other.

  20. 20.

    Semimajor axis at which the test particles at all initial longitudes survived the full integration time

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    M. Vázquez, E. Pallé & P. Montañés Rodríguez

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Vázquez, M., Pallé, E., Rodríguez, P.M. (2010). Extrasolar Planetary Systems. In: The Earth as a Distant Planet. Astronomy and Astrophysics Library. Springer, New York, NY. https://doi.org/10.1007/978-1-4419-1684-6_8

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