Rogue planet

From Wikipedia, the free encyclopedia
Jump to: navigation, search
This article is about a type of astronomical object. For other uses, see Rogue planet (disambiguation).
This video shows an artist's impression of the free-floating planet CFBDSIR J214947.2-040308.9.
Artist's conception of a Jupiter-size rogue planet.

A rogue planet, also known as an interstellar planet, nomad planet, free-floating planet or orphan planet, is a planetary-mass object that orbits the galaxy directly. They have either been ejected from the planetary system in which they formed or never been gravitationally bound to any star or brown dwarf.[1][2][3]

Some planetary-mass objects are thought to have formed in a similar way to stars, and the IAU has proposed that those objects be called sub-brown dwarfs[4] (an example of this is Cha 110913-773444, which may be an ejected rogue planet or may have formed on its own and be a sub-brown dwarf).[5] The closest free-floating planetary mass object to Earth yet discovered, WISE 0855–0714, is around 7 light years away.

In December 2013 a candidate exomoon of a free-floating planet was announced.[6]

Observation[edit]

Most methods of detecting exoplanets rely on periodicity of the planet orbiting a host star and thus cannot be used to detect rogue planets. Two methods to detect rogue planets still can be used: gravitational microlensing and direct imaging.

Direct imaging allows astronomers to observe rogue planets continuously. However, only young and massive rogue planets can be observed this way because they emit enough radiation to be detected. On the other hand, without the glare of the host star, the planet itself can be observed more easily once found.

When a planetary-sized object passes in front of a background star, its gravitational field causes a momentary increase in the visible brightness of the background star. This is known as microlensing. The disadvantage of microlensing is that the planet cannot be continuously observed. However, it works better than direct imaging for older and lower-mass planets. Astrophysicist Takahiro Sumi of Osaka University in Japan and colleagues, who form the Microlensing Observations in Astrophysics (MOA) and the Optical Gravitational Lensing Experiment (OGLE) collaborations, carried out a study of microlensing which they published in 2011. They observed 50 million stars in our galaxy using the 1.8 meter MOA-II telescope at New Zealand's Mount John Observatory and the 1.3 meter University of Warsaw telescope at Chile's Las Campanas Observatory. They found 474 incidents of microlensing, ten of which were brief enough to be planets of around Jupiter's size with no associated star in the immediate vicinity. The researchers estimated from their observations that there are nearly two free-floaters for every star in our galaxy.[7][8][9] Other estimations suggest a much larger number, up to 100,000 times more free-floating planets than stars in our Milky Way.[10] In November 2012 astronomers discovered a rogue planet around 100 light-years from Earth.[11]

Retention of heat in interstellar space[edit]

In 1998, David J. Stevenson theorized[12] that some planet-sized objects drift in the vast expanses of cold interstellar space and could possibly sustain a thick atmosphere that would not freeze out. He proposes that atmospheres are preserved by the pressure-induced far-infrared radiation opacity of a thick hydrogen-containing atmosphere.

It is thought that, during planetary-system formation, several small protoplanetary bodies may be ejected from the forming system.[13] With the reduced ultraviolet light that would normally strip the lighter components from an atmosphere, due to its increasing distance from the parent star, the planet's predominantly hydrogen- and helium-containing atmosphere would be easily confined even by an Earth-sized body's gravity.[12]

It is calculated that, for an Earth-sized object at a kilobar hydrogen atmospheric pressures in which a convective gas adiabat has formed, geothermal energy from residual core radioisotope decay will be sufficient to heat the surface to temperatures above the melting point of water.[12] Thus, it is proposed that interstellar planetary bodies with extensive liquid-water oceans may exist. It is further suggested that these planets are likely to remain geologically active for long periods, providing a geodynamo-created protective magnetosphere and possible sea floor volcanism which could provide an energy source for life.[12] Thus humans could theoretically live on a planet without a sun, although food sources would be limited. The author admits these bodies would be difficult to detect due to the intrinsically weak thermal microwave radiation emissions emanating from the lower reaches of the atmosphere, although later research suggests[14] that reflected solar radiation and far-IR thermal emissions may be detectable if one were to pass within 1000 AU of Earth.

A study of simulated planet ejection scenarios has suggested that around five percent of Earth-sized planets with Moon-sized natural satellites would retain their satellites after ejection. A large satellite would be a source of significant geological tidal heating.[15]

Proplyds of planetars[edit]

Recently, it has been discovered that some exoplanets such as the planemo 2M1207b, orbiting the brown dwarf 2M1207, have debris discs. If some large interstellar objects are considered stars (sub-brown dwarfs), then the debris could coalesce into planets, meaning the disks are proplyds. If these are considered planets, then the debris would coalesce as satellites. The term planetar exists for those accretion masses that seem to fall between stars and planets.

Known or possible rogue planets[edit]

There is no current way of telling whether these are planets that have been ejected from orbiting a star or were originally formed on their own as sub-brown dwarfs.

Planet Mass (MJ) Distance (ly) Status Discovery
WISE 0855–0714 3-10 7.1 Confirmed 2014
S Ori 52 2–8 (or brown dwarf) Mass not constrained
UGPS J072227.51-054031.2 5–40 13 Mass not constrained 2010
Cha 110913-773444 5–15 163 Mass not constrained 2004
CFBDSIR 2149-0403 4–7 130±13 Confirmed 2012
PSO J318.5-22 6.5 80 Confirmed 2013
MOA-2011-BLG-262 ~4 May be a red dwarf 2013

See also[edit]

References[edit]

  1. ^ Orphan Planets: It's a Hard Knock Life, Space.com, 24 Feb 2005, retrieved 5 Feb 2009.
  2. ^ Free-Floating Planets – British Team Restakes Dubious Claim[dead link], Space.com, 18 Apr 2001, retrieved 5 Feb 2009.
  3. ^ Orphan 'planet' findings challenged by new model, NASA Astrobiology, 18 Apr 2001, retrieved 5 Feb 2009.
  4. ^ Working Group on Extrasolar Planets – Definition of a "Planet"[dead link] POSITION STATEMENT ON THE DEFINITION OF A "PLANET" (IAU)
  5. ^ Rogue planet find makes astronomers ponder theory
  6. ^ A sub-Earth-mass moon orbiting a gas giant primary or a high-velocity planetary system in the galactic bulge
  7. ^ Homeless' Planets May Be Common in Our Galaxy by Jon Cartwright, Science Now ,18 May 2011, Accessed 20 may 2011
  8. ^ Planets that have no stars: New class of planets discovered, Physorg.com, May 18, 2011. Accessed May 2011.
  9. ^ [T. Sumi, et al. (2011). "Unbound or Distant Planetary Mass Population Detected by Gravitational Microlensing". arXiv:1105.3544v1 [astro-ph.EP].
  10. ^ "Researchers say galaxy may swarm with 'nomad planets'". Stanford University. Retrieved 29 February 2012. 
  11. ^ (BBC) (Astron. & Asrophys.)
  12. ^ a b c d Stevenson, David J.; Stevens, CF (1999). "Life-sustaining planets in interstellar space?". Nature 400 (6739): 32. Bibcode:1999Natur.400...32S. doi:10.1038/21811. PMID 10403246. 
  13. ^ Lissauer, J.J. (1987). "Timescales for Planetary Accretion and the Structure of the Protoplanetary disk". Icarus 69 (2): 249–265. Bibcode:1987Icar...69..249L. doi:10.1016/0019-1035(87)90104-7. 
  14. ^ Dorian S. Abbot; Eric R. Switzer (2 Jun 2011). "The Steppenwolf: A proposal for a habitable planet in interstellar space". arXiv:1102.1108.
  15. ^ Debes, John H.; Steinn Sigurðsson (20 October 2007). "The Survival Rate of Ejected Terrestrial Planets with Moons". The Astrophysical Journal Letters 668 (2): L167–L170. arXiv:0709.0945. Bibcode:2007ApJ...668L.167D. doi:10.1086/523103. 

External links[edit]