Carbon planet

Last updated

Artist's concept of a carbon planet. The surface is dark and reddish from hydrocarbon deposits. Carbon Planet.JPG
Artist's concept of a carbon planet. The surface is dark and reddish from hydrocarbon deposits.

A carbon planet is a hypothetical type of planet that contains more carbon than oxygen. [1] Carbon is the fourth most abundant element in the universe by mass after hydrogen, helium, and oxygen.

Contents

Marc Kuchner and Sara Seager coined the term "carbon planet" in 2005 and investigated such planets following the suggestion of Katharina Lodders that Jupiter formed from a carbon-rich core. [2] Prior investigations of planets with high carbon-to-oxygen ratios include Fegley & Cameron 1987. [3] Carbon planets could form if protoplanetary discs are carbon-rich and oxygen-poor. They would develop differently from Earth, Mars, and Venus, which are composed mostly of silicon–oxygen compounds. Different planetary systems have different carbon-to-oxygen ratios, with the Solar System's terrestrial planets closer to being "oxygen planets" with C/O molar ratio of 0.55. [4] In 2020, survey of the 249 nearby solar analog stars found 12% of stars have C/O ratios above 0.65, making them candidates for the carbon-rich planetary systems. [5] The exoplanet 55 Cancri e, orbiting a host star with C/O molar ratio of 0.78, [6] is a possible example of a carbon planet.

Definition

Such a planet would probably have an iron-rich core like the known terrestrial planets. Surrounding that would be molten silicon carbide and titanium carbide. Above that, a layer of carbon in the form of graphite, possibly with a kilometers-thick substratum of diamond if there is sufficient pressure. During volcanic eruptions, it is possible that diamonds from the interior could come up to the surface, resulting in mountains of diamonds and silicon carbides. The surface would contain frozen or liquid hydrocarbons (e.g., tar and methane) and carbon monoxide. [7] A weather cycle is hypothetically possible on carbon planets with an atmosphere, provided that the average surface temperature is below 77 °C.

However, carbon planets will probably be devoid of water, which cannot form because any oxygen delivered by comets or asteroids will react with the carbon on the surface. The atmosphere on a relatively cool carbon planet would consist primarily of carbon dioxide or carbon monoxide with a significant amount of carbon smog. [8]

Composition

Comparison of sizes of planets with different compositions Planet sizes.svg
Comparison of sizes of planets with different compositions

Carbon planets are predicted to be of similar diameter to silicate and water planets of the same mass, potentially making them difficult to distinguish. [10] The equivalents of geologic features on Earth may also be present, but with different compositions. For instance, the rivers might consist of oils. If the temperature is low enough (below 350 K), then gasses may be able to photochemically synthesize into long-chain hydrocarbons, which could rain down onto the surface.

In 2011, NASA cancelled a mission, called TPF, which was to be an observatory much bigger than the Hubble Space Telescope that would have been able to detect such planets. The spectra of carbon planets would lack water, but show the presence of carbonaceous substances, such as carbon monoxide.

Possible candidates

Draugr, Poltergeist and Phobetor

The pulsar planets Draugr , Poltergeist and Phobetor may be carbon planets that formed from the disruption of a carbon-producing star. Carbon planets might also be located near the Galactic Center or globular clusters orbiting the galaxy, where stars have a higher carbon-to-oxygen ratio than the Sun. When old stars die, they spew out large quantities of carbon. As time passes and more and more generations of stars end, the concentration of carbon, and carbon planets, will increase. [11]

Janssen

In October 2012, it was announced that Janssen showed evidence for being a carbon planet. It has eight times the mass of Earth and twice the radius. Research indicates that the 2,150 °C (3,900 °F) planet is "covered in graphite and diamond rather than water and granite". It orbits the star Copernicus once every 18 hours. [12]

Other carbon-rich objects

In August 2011, Matthew Bailes and his team of experts from Swinburne University of Technology in Australia reported that the millisecond pulsar PSR J1719-1438 may have a binary companion star that has been crushed into a much smaller planet made largely of solid diamond. They deduced that a small companion planet must be orbiting the pulsar and causing a detectable gravitational pull. Further examination revealed that although the planet is relatively small (60,000 km diameter, or five times bigger than the Earth) its mass is slightly more than that of Jupiter. The high density of the planet gave the team a clue to its likely makeup of carbon and oxygen—and suggested the crystalline form of the elements. [13] However, this "planet" is hypothesized to be the remains of an evaporated white dwarf companion, being only the remnant inner core. According to some definitions of planet, this would not qualify because it formed as a star. [14]

At a distance of 267+1.2
−0.9 pc (approximately 870 light-years), [15] PSR J2222−0137 is a nearby intermediate-mass binary pulsar whose low-mass neutron star's companion is a white dwarf (PSR J2222−0137 B). The white dwarf has a relatively large mass of 1.319 ± 0.004  M☉ [16] and a temperature less than 3,000 K, [15] meaning it is likely crystallized, leading to this Earth-sized white dwarf being described as a "diamond-star". [17]

Brown dwarfs

Planets around brown dwarfs are likely to be carbon planets depleted of water. [18]

See also

Related Research Articles

<span class="mw-page-title-main">Exoplanet</span> Planet outside the Solar System

An exoplanet or extrasolar planet is a planet outside the Solar System. The first possible evidence of an exoplanet was noted in 1917 but was not then recognized as such. The first confirmation of the detection occurred in 1992. A different planet, first detected in 1988, was confirmed in 2003. As of 1 April 2024, there are 5,653 confirmed exoplanets in 4,161 planetary systems, with 896 systems having more than one planet. The James Webb Space Telescope (JWST) is expected to discover more exoplanets, and to give more insight into their traits, such as their composition, environmental conditions, and potential for life.

<span class="mw-page-title-main">White dwarf</span> Type of stellar remnant composed mostly of electron-degenerate matter

A white dwarf is a stellar core remnant composed mostly of electron-degenerate matter. A white dwarf is very dense: its mass is comparable to the Sun's, while its volume is comparable to Earth's. A white dwarf's low luminosity comes from the emission of residual thermal energy; no fusion takes place in a white dwarf. The nearest known white dwarf is Sirius B, at 8.6 light years, the smaller component of the Sirius binary star. There are currently thought to be eight white dwarfs among the hundred star systems nearest the Sun. The unusual faintness of white dwarfs was first recognized in 1910. The name white dwarf was coined by Willem Luyten in 1922.

<span class="mw-page-title-main">Brown dwarf</span> Type of substellar object larger than a planet

Brown dwarfs are substellar objects that have more mass than the biggest gas giant planets, but less than the least massive main-sequence stars. Their mass is approximately 13 to 80 times that of Jupiter (MJ)—not big enough to sustain nuclear fusion of ordinary hydrogen (1H) into helium in their cores, but massive enough to emit some light and heat from the fusion of deuterium (2H). The most massive ones can fuse lithium (7Li).

<span class="mw-page-title-main">Rogue planet</span> Planetary object without a planetary system

A rogueplanet, also termed a free-floating planet (FFP) or an isolated planetary-mass object (iPMO), is an interstellar object of planetary mass which is not gravitationally bound to any star or brown dwarf.

PSR B1257+12, previously designated PSR 1257+12, alternatively designated PSR J1300+1240, is a millisecond pulsar located 2,300 light-years from the Sun in the constellation of Virgo, rotating at about 161 times per second. It is also named Lich, after a powerful, fictional undead creature of the same name.

<span class="mw-page-title-main">55 Cancri</span> Binary star with at least five exoplanets 41 light-years away

55 Cancri is a binary star system located 41 light-years away from the Sun in the zodiac constellation of Cancer. It has the Bayer designation Rho1 Cancri (ρ1 Cancri); 55 Cancri is the Flamsteed designation. The system consists of a K-type star and a smaller red dwarf.

<span class="mw-page-title-main">Gliese 876</span> Star in the constellation Aquarius

Gliese 876 is a red dwarf star 15.2 light-years away from Earth in the constellation of Aquarius. It is one of the closest known stars to the Sun confirmed to possess a planetary system with more than two planets, after GJ 1061, YZ Ceti, Tau Ceti, and Wolf 1061; as of 2018, four extrasolar planets have been found to orbit the star. The planetary system is also notable for the orbital properties of its planets. It is the only known system of orbital companions to exhibit a near-triple conjunction in the rare phenomenon of Laplace resonance. It is also the first extrasolar system around a normal star with measured coplanarity. While planets b and c are located in the system's habitable zone, they are giant planets believed to be analogous to Jupiter.

<span class="mw-page-title-main">Hulse–Taylor pulsar</span> Pulsar in the constellation Aquila

The Hulse–Taylor pulsar is a binary star system composed of a neutron star and a pulsar which orbit around their common center of mass. It is the first binary pulsar ever discovered.

<span class="mw-page-title-main">Exomoon</span> Moon beyond the Solar System

An exomoon or extrasolar moon is a natural satellite that orbits an exoplanet or other non-stellar extrasolar body.

<span class="mw-page-title-main">Binary pulsar</span> Two pulsars orbiting each other

A binary pulsar is a pulsar with a binary companion, often a white dwarf or neutron star. Binary pulsars are one of the few objects which allow physicists to test general relativity because of the strong gravitational fields in their vicinities. Although the binary companion to the pulsar is usually difficult or impossible to observe directly, its presence can be deduced from the timing of the pulses from the pulsar itself, which can be measured with extraordinary accuracy by radio telescopes.

HD 114762 b is a small red dwarf star, in the HD 114762 system, formerly thought to be a massive gaseous extrasolar planet, approximately 126 light-years (38.6 pc) away in the constellation of Coma Berenices. This optically undetected companion to the late F-type main-sequence star HD 114762 was discovered in 1989 by Latham, et al., and confirmed in an October 1991 paper by Cochran, et al. It was thought to be the first discovered exoplanet

<span class="mw-page-title-main">Circumbinary planet</span> Planet that orbits two stars instead of one

A circumbinary planet is a planet that orbits two stars instead of one. The two stars orbit each other in a binary system, while the planet typically orbits farther from the center of the system than either of the two stars. In contrast, circumstellar planets in a binary system have stable orbits around one of the two stars, closer in than the orbital distance of the other star. Studies in 2013 showed that there is a strong hint that a circumbinary planet and its stars originate from a single disk.

<span class="mw-page-title-main">Planetary-mass object</span> Size-based definition of celestial objects

A planetary-mass object (PMO), planemo, or planetary body is, by geophysical definition of celestial objects, any celestial object massive enough to achieve hydrostatic equilibrium, but not enough to sustain core fusion like a star.

<span class="mw-page-title-main">PSR J1719−1438</span> Millisecond pulsar in the constellation Serpens

PSR J1719-1438 is a millisecond pulsar with a spin period of 5.8 ms located about 4,000 ly from Earth in the direction of Serpens Cauda, one minute from the border with Ophiuchus. Millisecond pulsars are generally thought to begin as normal pulsars and then spin up by accreting matter from a binary companion.

<span class="mw-page-title-main">Gas giant</span> Giant planet mainly composed of light elements

A gas giant is a giant planet composed mainly of hydrogen and helium. Jupiter and Saturn are the gas giants of the Solar System. The term "gas giant" was originally synonymous with "giant planet". However, in the 1990s, it became known that Uranus and Neptune are really a distinct class of giant planets, being composed mainly of heavier volatile substances. For this reason, Uranus and Neptune are now often classified in the separate category of ice giants.

<span class="mw-page-title-main">Kepler-444</span> Triple star system in the constellation of Lyra

Kepler-444 is a triple star system, estimated to be 11.2 billion years old, approximately 119 light-years (36 pc) away from Earth in the constellation Lyra. On 27 January 2015, the Kepler spacecraft is reported to have confirmed the detection of five sub-Earth-sized rocky exoplanets orbiting the main star. The star is a K-type main sequence star. All of the planets are far too close to their star to harbour life forms.

<span class="mw-page-title-main">Pulsar planet</span> Planets found orbiting pulsars, or rapidly rotating pulsars

Pulsar planets are planets that are orbiting pulsars. The first such planets to be discovered were around a millisecond pulsar in 1992 and were the first extrasolar planets to be confirmed as discovered. Pulsars are extremely precise clocks and even small planets can create detectable variations in pulsar traits; the smallest known exoplanet is a pulsar planet.

PSR J2222−0137 is a nearby intermediate-mass binary pulsar at a distance of 267+1.2
−0.9 pc, whose low-mass neutron star's companion is a white dwarf. The white dwarf has a relatively large mass of 1.319 ± 0.004 M☉ and a temperature less than 3,000 K, meaning it is likely crystallized, leading to this Earth-sized white dwarf being described as a "diamond-star".

References

  1. ↑ Kuchner, Marc J.; Seager, S. (2005). "Extrasolar Carbon Planets". arXiv: astro-ph/0504214 .
  2. ↑ Lodders, Katharina (2004). "Jupiter Formed with More Tar than heat" (PDF). The Astrophysical Journal . 611 (1): 587–597. Bibcode:2004ApJ...611..587L. doi:10.1086/421970. S2CID   59361587.
  3. ↑ Fegley, Bruce Jr.; Cameron, A. G. W. (April 1987). "A vaporization model for iron/silicate fractionation in the Mercury protoplanet" (PDF). Earth and Planetary Science Letters . 82 (3–4): 207–222. Bibcode:1987E&PSL..82..207F. CiteSeerX   10.1.1.667.7941 . doi:10.1016/0012-821X(87)90196-8.
  4. ↑ P. E. Nissen, The carbon-to-oxygen ratio in stars with planets
  5. ↑ Stonkutė, E.; Chorniy, Y.; Tautvaišienė, G.; Drazdauskas, A.; Minkevičiūtė, R.; Mikolaitis, Š.; Kjeldsen, H.; Essen, C. von; Pakštienė, E.; Bagdonas, V. (2020). "High-resolution Spectroscopic Study of Dwarf Stars in the Northern Sky: Lithium, Carbon, and Oxygen Abundances". The Astronomical Journal. 159 (3): 90. arXiv: 2002.05555 . Bibcode:2020AJ....159...90S. doi: 10.3847/1538-3881/ab6a19 . S2CID   211096705.
  6. ↑ Teske, Johanna K.; Cunha, Katia; Schuler, Simon C.; Griffith, Caitlin A.; Smith, Verne V. (2013). "Carbon and Oxygen Abundances in Cool Metal-Rich Exoplanet Hosts: A Case Study of the C/O Ratio of 55 Cancri". The Astrophysical Journal. 778 (2): 132. arXiv: 1309.6032 . Bibcode:2013ApJ...778..132T. doi:10.1088/0004-637X/778/2/132. S2CID   119291907.
  7. ↑ Musser, George (January 2010). "Earth-Like Planets May Be Made of Carbon". Scientific American . Retrieved 3 January 2013.
  8. ↑ "Kohlenstoffplaneten", Space Magazin April 2014 (p. 35, in German)
  9. ↑ Naeye, Bob (24 September 2007). "Scientists Model a Cornucopia of Earth-sized Planets". Goddard Space Flight Center.
  10. ↑ Seager, Sara; Kuchner, Marc; Hier-Majumder, Catherine; Militzer, Burkhard (2007). "Mass-Radius Relationships for Solid Exoplanets". The Astrophysical Journal . 669 (2): 1279. arXiv: 0707.2895 . Bibcode:2007ApJ...669.1279S. doi:10.1086/521346. S2CID   8369390.
  11. ↑ "Carbon Planets - Space Art and Astronomical Illustrations". Novacelestia.com. Retrieved 3 January 2013.
  12. ↑ Wickham, Chris (15 October 2012). "A diamond bigger than Earth?". Reuters . Retrieved 3 January 2013.
  13. ↑ "Solid diamond planet found". Australian Geographic . 26 August 2011. Archived from the original on 6 October 2011.
  14. ↑ Lemonick, Michael (26 August 2011). "Scientists Discover a Diamond as Big as a Planet". Time . Archived from the original on 26 August 2011.
  15. 1 2 Kaplan, David L.; Boyles, Jason; Dunlap, Bart H.; Tendulkar, Shriharsh P.; Deller, Adam T.; Ransom, Scott M.; McLaughlin, Maura A.; Lorimer, Duncan R.; Stairs, Ingrid H. (2014). "A 1.05M☉Companion to PSR J2222–0137: The Coolest Known White Dwarf?". The Astrophysical Journal. 789 (2): 119. arXiv: 1406.0488v1 . Bibcode:2014ApJ...789..119K. doi:10.1088/0004-637X/789/2/119. ISSN   0004-637X. S2CID   19986066.
  16. ↑ Guo, Y. J.; Freire, P. C. C.; Guillemot, L.; Kramer, M.; Zhu, W. W.; Wex, N.; McKee, J. W.; Deller, A.; Ding, H.; Kaplan, D. L.; Stappers, B.; Cognard, I.; Miao, X.; Haase, L.; Keith, M.; Ransom, S. M.; Theureau, G. (2021). "PSR J2222−0137. I. Improved physical parameters for the system". Astronomy & Astrophysics. 654: A16. arXiv: 2107.09474 . Bibcode:2021A&A...654A..16G. doi:10.1051/0004-6361/202141450. S2CID   236134389.
  17. ↑ Drake, Nadia (24 June 2014). "Astronomers Find Slow-Cooked Diamond the Size of Earth". National Geographic. Archived from the original on 21 March 2021.
  18. ↑ Pascucci, Ilaria; Herczeg, Greg; Carr, John S.; Bruderer, Simon (December 2013). "The atomic and molecular content of disks around very low-mass stars and brown dwarfs" (PDF). The Astrophysical Journal . 779 (2): 178. arXiv: 1311.1228 . Bibcode:2013ApJ...779..178P. doi:10.1088/0004-637X/779/2/178. hdl:11858/00-001M-0000-0017-AAEA-0. S2CID   119001471.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.