Cleared the neighbourhood
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In the end stages of planet formation, a planet will have cleared the neighbourhood of its own orbital zone, meaning it has become gravitationally dominant, and there are no other bodies of comparable size other than its own satellites or those otherwise under its gravitational influence. The current definition of a planet adopted by the International Astronomical Union (IAU) only includes those bodies which have "cleared the neighbourhood of its orbit."[1] A large body which meets the other criteria for a planet but has not cleared its neighbourhood is classified as a dwarf planet. This includes Pluto, which shares its orbital neighbourhood with Kuiper Belt Objects such as the plutinos. The IAU's definition does not attach specific numbers or equations to this term, but the extent to which all the planets have cleared their neighbourhoods is much greater, by any measure, than that of any dwarf planet or any candidate for dwarf planet known so far.
The phrase may be derived from a paper presented to the general assembly of the IAU in 2000 by Alan Stern and Harold Levison. The authors used several similar phrases as they developed a theoretical basis for determining if an object orbiting a star is likely to "clear its neighboring region" of planetesimals, based on the object's mass and its orbital period.[2]
Clearly distinguishing "planets" from "dwarf planets" and other minor planets had become necessary because the IAU had adopted different rules for naming newly discovered major planets and newly discovered minor planets, without establishing a basis for telling them apart. The naming process for Eris stalled after the announcement of its discovery in 2005, pending clarification of this first step.
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[edit] Details
The phrase refers to an orbiting body (a planet or protoplanet) "sweeping out" its orbital region over time, by gravitationally interacting with smaller bodies nearby. Over many orbital cycles, a large body will tend to cause small bodies either to accrete with it, or to be disturbed to another orbit. As a consequence it does not then share its orbital region with other bodies of significant size, except for its own satellites, or other bodies governed by its own gravitational influence. This latter restriction excludes objects whose orbits may cross but which will never collide with each other due to orbital resonance, such as Jupiter and the Trojan asteroids, Earth and 3753 Cruithne or Neptune and the plutinos.[2]
Steven Soter of the Department of Astrophysics, American Museum of Natural History, has written that "A heliocentric body with Λ > 1 [viz., a planet] has cleared a substantial fraction of small bodies out of its orbital neighborhood."[3] Λ (Lambda) is a parameter proposed by Stern and Levison[2] that measures the extent to which a body scatters smaller masses out of its orbital zone over a long period of time. Mathematically Λ is defined as
where k is approximately constant and M and P are the scattering body's mass and orbital period, respectively. Two bodies are defined to share an orbital zone if their orbits cross a common radial distance from the primary, and their non-resonant periods differ by less than an order of magnitude. The order-of-magnitude similarity in period requirement excludes comets from the calculation, but the combined mass of the comets turn out to be negligible compared to the other small solar system bodies anyway so their inclusion would have little impact on the results. Stern and Levison found a gap of five orders of magnitude in Λ between the smallest terrestrial planets and the largest asteroids and Kuiper Belt Objects (KBOs).
Soter went on to propose a parameter he called the "planetary discriminant", designated with the symbol µ (mu) , that represents an experimental measure of the actual degree of cleanliness of the orbital zone. µ is calculated by dividing the mass of the candidate body by the total mass of the other objects that share its orbital zone.
Here is a list of planets by planetary discriminant, as defined by Steven Soter, in decreasing order, where the planetary discriminant μ is the ratio between the mass of the body and the total mass of the other non-resonating and non-satellite bodies in the same orbital zone, as defined by Soter. Also listed is the Stern-Levinson parameter Λ, the square of the mass over the orbital period, normalized to the Earth values(Λ/ΛE). (Note that ΛE ~ 1.5×105, so that the unnormalized values of Λ for the eight planets defined by the IAU are orders of magnitude greater than 1, and the values of Λ for the dwarf planets are orders of magnitude less than 1.)[3]
The calculated parameters for major solar system bodies are:[3]
| Rank | Name | Image | Stern-Levinson parameter Λ/ΛE; |
Planetary discriminant μ |
Mass (kg) | Type of object |
|---|---|---|---|---|---|---|
| 1 | Earth |
 |
1.00 | 1.7×106 | (5.9736×1024 kg) | 3rd planet |
| 2 | Venus |
 |
1.08 | 1.35×106 | (4.8685×1024 kg) | 2nd planet |
| 3 | Jupiter |
 |
8510 | 6.25×105 | (1.899×1027 kg) | 5th planet |
| 4 | Saturn |
 |
308 | 1.9×105 | (5.6846×1026 kg) | 6th planet |
| 5 | Mars |
 |
0.0061 | 1.8×105 | (6.4185×1023 kg) | 4th planet |
| 6 | Mercury |
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0.0126 | 9.1×104 | (3.302×1023 kg) | 1st planet |
| 7 | Uranus |
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2.51 | 2.9×104 | (8.6832×1025 kg) | 7th planet |
| 8 | Neptune |
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1.79 | 2.4×104 | (1.0243×1026 kg) | 8th planet |
| 9 | Ceres |
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8.7×10−9 | 0.33 | 9.5×1020 kg | 1st dwarf planet |
| 10 | Eris |
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3.5×10−8 | 0.10 | (1.66×1022 kg) | 3rd dwarf planet |
| 11 | Pluto |
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1.95×10−8 | 0.077 | (1.29×1022 ± 10% kg) | 2nd dwarf planet |
[edit] Controversy
Stern, currently leading the NASA New Horizons mission to Pluto, objects to the reclassification of Pluto on the basis that—like Pluto—Earth, Mars, Jupiter and Neptune have not cleared their orbital neighbourhoods either. Earth co-orbits with 10,000 near-Earth asteroids, and Jupiter has 100,000 Trojan asteroids in its orbital path. "If Neptune had cleared its zone, Pluto wouldn't be there," he now says.[4]
However, in 2000 Stern himself wrote, "we define an überplanet as a planetary body in orbit about a star that is dynamically important enough to have cleared its neighboring planetesimals ..." and a few paragraphs later, "From a dynamical standpoint, our solar system clearly contains 8 überplanets"—including Earth, Mars, Jupiter, and Neptune.[2] Most planetary scientists understand "clearing the neighborhood" to refer to an object being the dominant mass in its vicinity, for instance Earth being many times more massive than all of the NEAs combined, and Neptune "dwarfing" Pluto and the rest of the KBOs.[3]
Stern and Levison's paper shows that it is possible to estimate whether an object is likely to dominate its neighborhood given only the object's mass and orbital period, known values even for extrasolar planets. In any case, the recent IAU definition specifically limits itself only to objects orbiting the Sun.[1]
[edit] See also
- Planet
- List of planetary bodies
- List of solar system objects by mass
- List of solar system objects by radius
- List of solar system objects
- List of noteworthy asteroids
- Definition of planet
- 2006 definition of planet
- Mesoplanet
[edit] References
- ^ a b "The Final IAU Resolution on the definition of "planet" ready for voting", IAU, 24 August 2006. Retrieved on 2006-08-26.
- ^ a b c d Stern, S. Alan; and Levison, Harold F. (2002). "Regarding the criteria for planethood and proposed planetary classification schemes" (PDF). Highlights of Astronomy 12: 205–213, as presented at the XXIVth General Assembly of the IAU–2000 [Manchester, UK, 7 August-18 August 2000].
- ^ a b c d Soter, Steven (2006-08-16). What is a Planet? (PDF). Retrieved on 2006-08-24. submitted to The Astronomical Journal, 16 August 2006
- ^ Rincon, Paul (25 August 2006). Pluto vote 'hijacked' in revolt. BBC News. Retrieved on 2006-09-03.
[edit] External links
- Ottawa Citizen: The case against Pluto (P. Surdas Mohit) Thursday, August 24, 2006
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