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In astronomy, double planet and binary planet are informal terms used to describe a binary system where both objects are of planetary mass. Though not an official classification, the European Space Agency has referred to the Earth–Moon system as a double planet. The IAU General Assembly in August 2006 considered a proposal that Pluto and Charon be reclassified as a double planet, but the proposal was abandoned.
Definition of a double planet
There has been debate on where to draw the line between a double planet and a planet–moon system. In most cases, this is not an issue because most satellites have small masses relative to their planets. In particular, with the exception of the Earth–Moon system, all satellites of planets in the Solar System have masses less than 0.00025 (1⁄4000) the mass of the host planet. The Moon-to-Earth mass ratio is 0.01230 (≈ 1⁄81). In comparison, the Charon-to-Pluto mass ratio is 0.117 (≈ 1⁄9).
The now-abandoned co-accretion hypothesis of the origin of the Moon is also called the double-planet hypothesis. The idea is that two bodies should be considered a double planet if they accreted together directly from the proto-planetary disk, much as a double star typically forms together.
Once it was realized that both the Moon and Pluto's Charon likely formed from giant impacts, this parallel was noted when calling them double planets. However, an impact may also produce tiny satellites, such as the small outer satellites of Pluto, so this does not determine where the line should be drawn.
A common proposal for a double planet is a system where the center of mass lies outside the primary. This was the basis for the argument that the Pluto–Charon system be considered a double planet when the IAU was debating whether dwarf planets should be considered a class of planet. Under this definition, the Earth–Moon system is not a double planet. However, the center of mass varies with the distance between the bodies. As the Moon migrates outward from Earth, the center of mass of the system will migrate outward as well, until in a few hundred million years Earth will fit the definition. It has been suggested that such a definition would call into question Jupiter's status as a planet, as the center of mass of the Jupiter–Sun system lies outside the surface of the Sun.
Isaac Asimov suggested a distinction between planet–moon and double-planet structures based in part on what he called a "tug-of-war" value, which does not consider their relative sizes. This quantity is simply the relationships between the masses of the primary planet and the Sun combined with the squared distances between the smaller object and its planet and the Sun:
- tug-of-war value = m1⁄m2 × (d1⁄d2)2
where m1 is the mass of the larger body, m2 is the mass of the Sun, d1 is the distance between the smaller body and the Sun, and d2 is the distance between the smaller body and the larger body. Note that the tug-of-war value does not rely on the mass of the satellite or smaller body.
This formula actually reflects the relation of the gravitational effects on the smaller body from the larger body and from the Sun. The tug-of-war figure for Saturn's moon Titan is 380, which means that Saturn's hold on Titan is 380 times as strong as the Sun's hold on Titan. Titan's tug-of-war value may be compared with that of Saturn's moon Phoebe, which has a tug-of-war value of just 3.5. So Saturn's hold on Phoebe is only 3.5 times as strong as the Sun's hold on Phoebe.
Asimov calculated tug-of-war values for several satellites of the planets. He showed that even the largest gas giant, Jupiter, had only a slightly better hold than the Sun on its outer captured satellites, some with tug-of-war values not much higher than one. Yet in nearly every case the tug-of-war value was found to be greater than one, so in every case the Sun loses the tug-of-war with the planets. The one exception was Earth's Moon, where the Sun wins the tug-of-war with a value of 0.46, which means that Earth's hold on the Moon is less than half that of the Sun. Because the Sun's gravitational effect on the Moon is more than twice that of Earth, Asimov reasoned that Earth and the Moon form a binary-planet. This was one of several arguments in Asimov's writings for considering the Moon a planet rather than a satellite.
We might look upon the Moon, then, as neither a true satellite of the Earth nor a captured one, but as a planet in its own right, moving about the Sun in careful step with the Earth. From within the Earth–Moon system, the simplest way of picturing the situation is to have the Moon revolve about the Earth; but if you were to draw a picture of the orbits of the Earth and Moon about the Sun exactly to scale, you would see that the Moon's orbit is everywhere concave toward the Sun. It is always "falling toward" the Sun. All the other satellites, without exception, "fall away" from the Sun through part of their orbits, caught as they are by the superior pull of their primary planets – but not the Moon.[Footnote 1]— Isaac Asimov
See the Path of Earth and Moon around Sun section in the "Orbit of the Moon" article for a more detailed explanation.
Note that this definition of "double planet" depends primarily on the two-body structure's distance from the Sun. If the Earth–Moon system happened to orbit farther away from the Sun than it does now, then Earth would win the tug of war. From the orbit of Mars, the Moon's tug-of-war value would be 1.05, so the Sun would no longer win the tug of war with Earth. Also, several tiny moons discovered since Asimov's argument would qualify as double planets. Neptune's small outer moons Neso and Psamathe, for example, have tug-of-war values of 0.42 and 0.44, less than that of Earth's Moon. Yet their masses are tiny compared to Neptune's, with an estimated ratio of 1.5×10−9 (1⁄700,000,000) and 0.4×10−9 (1⁄2,500,000,000).
|Look up double planet in Wiktionary, the free dictionary.|
- Asimov uses the term "concave" to describe the Earth–Moon orbital pattern around the Sun, whereas Aslaksen uses "convex" to describe the exact same pattern. Which term one uses relies solely upon the perspective of the observer. From the point-of-view of the Sun, the Moon's orbit is concave; from outside the Moon's orbit, say, from planet Mars, it is convex.
- "Welcome to the double planet". ESA. 2003-10-05. Retrieved 2009-11-12.
- "The IAU draft definition of "planet" and "plutons"". International Astronomical Union. 2006-08-16. Retrieved 2008-05-17.
- "A Moon over Pluto (Close up)". August 7, 2014.
- Herbst, T. M.; Rix, H.-W. (1999). "Star Formation and Extrasolar Planet Studies with Near-Infrared Interferometry on the LBT". In Guenther, Eike; Stecklum, Bringfried; Klose, Sylvio. Optical and Infrared Spectroscopy of Circumstellar Matter, ASP Conference Series, Vol. 188. San Francisco, Calif.: Astronomical Society of the Pacific. pp. 341–350. Bibcode:1999ASPC..188..341H. ISBN 1-58381-014-5.
- Asimov, Isaac (1975). "Just Mooning Around", collected in Of Time and Space, and Other Things. Avon. Formula derived on p. 89 of book. p. 55 of .pdf file. Retrieved 2012-01-20.
- Aslaksen, Helmer (2010). "The Orbit of the Moon around the Sun is Convex!". National University of Singapore: Department of Mathematics. Retrieved 2012-01-23.
- Stern, S. Alan (27 February 1997). "Clyde Tombaugh (1906–97) Astronomer who discovered the Solar System's ninth planet". Nature 385 (6619): 778. Bibcode:1997Natur.385..778S. doi:10.1038/385778a0 Pluto–Charon is "the only known example of a true double planet".
- Lissauer, Jack J. (25 September 1997). "It's not easy to make the Moon". Nature 389 (6649): 327–328. Bibcode:1997Natur.389..327L. doi:10.1038/38596 Compares the double-planet theories of Earth–Moon and Pluto–Charon formations.
- Cabrera, J.; Schneider, J. (2007). "Detecting companions to extrasolar planets using mutual events". Astronomy and Astrophysics 464 (3): 1133–1138. arXiv:astro-ph/0703609. Bibcode:2007A&A...464.1133C. doi:10.1051/0004-6361:20066111.