Sudarsky's gas giant classification

Sudarsky classification as used on Celestia.
Class I
Class I
Class II
Class II
Class III
Class III
Class IV
Class IV
Class V
Class V

Sudarsky's classification of gas giants for the purpose of predicting their appearance based on their temperature was outlined by David Sudarsky and colleagues in the paper Albedo and Reflection Spectra of Extrasolar Giant Planets[1] and expanded on in Theoretical Spectra and Atmospheres of Extrasolar Giant Planets,[2] published before any successful direct or indirect observation of an extrasolar planet atmosphere was made. It is a broad classification system with the goal of bringing some order to the likely rich variety of extrasolar gas-giant atmospheres.

Gas giants are split into five classes (numbered using Roman numerals) according to their modeled physical atmospheric properties. In the Solar System only Jupiter and Saturn are within the Sudarsky classification, and both are Class I. The appearance of planets that are not gas giants cannot be predicted by the Sudarsky system, for example terrestrial planets such as Earth, HD 85512 b (3.6 Earth masses) and OGLE-2005-BLG-390Lb (5.5 Earth masses), or ice giants such as Uranus (14 Earth masses) and Neptune (17 Earth masses).

Background

The appearance of extrasolar planets is largely unknown because of the difficulty in making direct observations of extrasolar planets. In addition, analogies with planets in the Solar System can apply for few of the extrasolar planets known; because most are wholly unlike any of our planets, for example the hot Jupiters.

Bodies that transit their star can be spectrographically mapped, for instance HD 189733 b.[3] That planet has further been shown to be blue with an albedo greater (brighter) than 0.14.[4] Most transiting planets are hot Jupiters.

Speculation on the appearances of unseen extrasolar planets currently relies upon computational models of the likely atmosphere of such a planet, for instance how the atmospheric temperature–pressure profile and composition would respond to varying degrees of insolation.

Planetary classes

Class I: Ammonia clouds

Jupiter, a Sudarsky class I planet.

Planets in this class have appearances dominated by ammonia clouds. These planets are found in the outer regions of a planetary system. They exist at temperatures less than about 150 K (−120 °C; −190 °F). The predicted Bond albedo of a class I planet around a star like the Sun is 0.57, compared with a value of 0.343 for Jupiter[5] and 0.342 for Saturn.[6] The discrepancy can be partially accounted for by taking into account non-equilibrium condensates such as tholin or phosphorus, which are responsible for the coloured clouds in the Jovian atmosphere, and are not modelled in the calculations.

The temperatures for a class I planet require a cool star or a distant orbit. The former stars might be too dim for us even to know about them, and the latter orbits might be too unpronounced for notice until several observations of those orbits' "years" (cf. Kepler's third law). Superjovians would have enough mass to improve these observations; but a superjovian of comparable age to Jupiter will have more internal heating than said planet, which could push it to a higher class.

As of 2015, 47 Ursae Majoris c and d could be Class I planets. Upsilon Andromedae e and 55 Cancri d may also be Class I planets.

Class II: Water clouds

Planets in class II are too warm to form ammonia clouds: instead their clouds are made up of water vapor. These characteristics are expected for planets with temperatures below around 250 K.[2] Water clouds are more reflective than ammonia clouds, and the predicted Bond albedo of a class II planet around a Sun-like star is 0.81. Even though the clouds on such a planet would be similar to those of Earth, the atmosphere would still consist mainly of hydrogen and hydrogen-rich molecules such as methane.

Examples of possible class II planets: HD 45364 b and HD 45364 c, HD 28185 b, Gliese 876 b and c, Upsilon Andromedae d, 55 Cancri f, 47 Ursae Majoris b, PH 2b, Kepler-90 h, HD 10180 g.

Class III: Cloudless

Planets with equilibrium temperatures between about 350 K (170 °F, 80 °C) and 800 K (980 °F, 530 °C) do not form global cloud cover, because they lack suitable chemicals in the atmosphere to form clouds.[2] These planets would appear as featureless blue globes because of Rayleigh scattering and absorption by methane in their atmospheres, appearing like Jovian-mass versions of Uranus and Neptune. Because of the lack of a reflective cloud layer, the Bond albedo is low, around 0.12 for a class-III planet around a Sun-like star. They exist in the inner regions of a planetary system, roughly corresponding to the location of Mercury.

Possible class-III planets are HD 37124 b, HD 18742 b, HD 178911 B b, 55 Cancri c, Upsilon Andromedae c, Kepler-89e, Corot-9b and HD 205739 b. Above 700 K (800 °F, 430 °C), sulfides and chlorides might provide cirrus-like clouds.[2]

Class IV: Alkali metals

Above 900 K (630 °C/1160 °F), carbon monoxide becomes the dominant carbon-carrying molecule in a gas giant's atmosphere (rather than methane). Furthermore, the abundance of alkali metals, such as sodium substantially increase, and spectral lines of sodium and potassium are predicted to be prominent in a gas giant's spectrum. These planets form cloud decks of silicates and iron deep in their atmospheres, but this is not predicted to affect their spectrum. The Bond albedo of a class IV planet around a Sun-like star is predicted to be very low, at 0.03 because of the strong absorption by alkali metals. Planets of classes IV and V are referred to as hot Jupiters.

55 Cancri b was listed as a class IV planet.[2]

HD 209458 b at 1300 K (1000 °C) would be another such planet, with a geometric albedo of, within error limits, zero; and in 2001, NASA witnessed atmospheric sodium in its transit, though less than predicted. This planet hosts an upper cloud deck absorbing so much heat that below it is a relatively cool stratosphere. The composition of this dark cloud, in the models, is assumed to be titanium/vanadium oxide (sometimes abbreviated "TiVO"), by analogy with M class dwarf stars, but its true composition is yet unknown; it could well be as per Sudarsky.[7][8]

HD 189733 b, with measured temperatures 920–1200 K (650–930 °C), also qualifies as class IV. However, in late 2007 it was measured as deep blue, with an albedo over 0.14 (possibly due to the brighter glow of its "hot spot"). No stratosphere has been conclusively proven for it as yet.

TrES-2b was measured with the lowest albedo, and therefore listed as class IV.

Class V: Silicate clouds

For the very hottest gas giants, with temperatures above 1400 K (2100 °F, 1100 °C) or cooler planets with lower gravity than Jupiter, the silicate and iron cloud decks are predicted to lie high up in the atmosphere. The predicted Bond albedo of a class V planet around a Sun-like star is 0.55, due to reflection by the cloud decks. At such temperatures, a gas giant may glow red from thermal radiation but the reflected light generally overwhelms thermal radiation. For stars of visual apparent magnitude under 4.50, such planets are theoretically visible to our instruments.[9] Examples of such planets might include 51 Pegasi b.[2] HAT-P-11b and those other extrasolar gas giants found by the Kepler telescope might be possible class V planets, such as Kepler-7b, HAT-P-7b, or Kepler-13 b.

See also

References

  1. ↑ Sudarsky, D.; Burrows, A.; Pinto, P. (2000). "Albedo and Reflection Spectra of Extrasolar Giant Planets". The Astrophysical Journal 538 (2): 885–903. arXiv:astro-ph/9910504. Bibcode:2000ApJ...538..885S. doi:10.1086/309160.
  2. 1 2 3 4 5 6 Sudarsky, D.; Burrows, A.; Hubeny, I. (2003). "Theoretical Spectra and Atmospheres of Extrasolar Giant Planets" (PDF). The Astrophysical Journal 588 (2): 1121–1148. arXiv:astro-ph/0210216. Bibcode:2003ApJ...588.1121S. doi:10.1086/374331.
  3. ↑ http://web.archive.org/web/20071016161601/http://www.spitzer.caltech.edu:80/Media/releases/ssc2007-09/ssc2007-09a.shtml. Archived from the original on October 16, 2007. Retrieved November 23, 2007. Missing or empty |title= (help)
  4. ↑ Berdyugina, Svetlana V.; Andrei V. Berdyugin; Dominique M. Fluri; Vilppu Piirola (20 January 2008). "First detection of polarized scattered light from an exoplanetary atmosphere" (PDF). The Astrophysical Journal 673: L83. arXiv:0712.0193. Bibcode:2008ApJ...673L..83B. doi:10.1086/527320.
  5. ↑ Jupiter Fact Sheet
  6. ↑ Saturn Fact Sheet
  7. ↑ Ivan Hubeny; Adam Burrows (2008). "Spectrum and atmosphere models of irradiated transiting extrasolar giant planets". arXiv:0807.3588v1 [astro-ph].
  8. ↑ Ian Dobbs-Dixon (2008). "Radiative Hydrodynamical Studies of Irradiated Atmospheres". arXiv:0807.4541v1 [astro-ph].
  9. ↑ Leigh, C., Collier, C. A., Horne, K., Penny, A., & James, D. (2003). A new upper limit on the reflected starlight from Tau Bootis b. MNRAS, 344, 1271

External links

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