From Wikipedia, the free encyclopedia
Jump to navigation Jump to search

Exoplanet List of exoplanets
TRAPPIST-1f Artist's Impression.png
Artist's impression of TRAPPIST-1f.
Parent star
Constellation Aquarius
Right ascension (α) 23h 06m 29.283s[1]
Declination (δ) –05° 02′ 28.59″
Apparent magnitude (mV) 18.8
Distance39.5 ± 1.3 ly
(12.1 ±0.4 pc)
Spectral type M8V[2]
Mass (m) 0.08 (± 0.009) M
Radius (r) 0.117 (± 0.004) R
Temperature (T) 2550.0 (± 55.0) K
Metallicity [Fe/H] 0.04 (± 0.08)
Age >0.5 Gyr
Physical characteristics
Mass(m)0.68 (± 0.18) M
Radius(r)1.045 (± 0.038) R
Stellar flux(F)0.382 (± 0.03)[3]
Surface gravity(g)~0.62 g
Temperature (T) 219 K (−54 °C; −65 °F), ≳1,400 K (1,130 °C; 2,060 °F)[4]
Orbital elements
Semi-major axis(a) 0.037 AU
Eccentricity (e) < 0.063
Orbital period(P) 9.206690 (± 0.000015) d
Inclination (i) 89.680 (± 0.034)°
Other designations
2MASS J23062928-0502285 f, 2MASSI J2306292-050227 f, 2MASSW J2306292-050227 f, 2MUDC 12171 f
Discovery information
Discovery date 22 February 2017
Discovery method Transit
Discovery status Published
Database references
Extrasolar Planets
Exoplanet Archivedata
Open Exoplanet Cataloguedata

TRAPPIST-1f, also designated as 2MASS J23062928-0502285 f, is an exoplanet, likely rocky but under a massive water-steam gaseous envelope at very high pressure and temperature,[4] orbiting within the habitable zone[5] around the ultracool dwarf star TRAPPIST-1 39 light-years (12 parsecs) away from Earth in the constellation of Aquarius. The exoplanet was found by using the transit method, in which the dimming effect that a planet causes as it crosses in front of its star is measured.

It was one of four new exoplanets to be discovered orbiting the star using observations from the Spitzer Space Telescope.[3]


Mass, radius, and temperature[edit]

TRAPPIST-1f is an Earth-sized exoplanet, meaning it has a mass and radius close to that of Earth. It has an equilibrium temperature of 219 K (−54 °C; −65 °F), which increases to above 1,400 K (1,130 °C; 2,060 °F) if the warming of its likely very dense atmosphere is taken into account.[4] It has a radius of 1.045 ± 0.038 R and a mass of 0.68 ± 0.18 M, giving it a density of 3.3±0.9 g/cm3.[3] These values suggest surface gravity around 6.1 m/s2 (62% of Earth value).

Host star[edit]

The planet orbits an (M-type) ultracool dwarf star named TRAPPIST-1. The star has a mass of 0.08 M and a radius of 0.11 R. It has a temperature of 2550 K and is at least 500 million years old. In comparison, the Sun is 4.6 billion years old[6] and has a temperature of 5778 K.[7] The star is metal-rich, with a metallicity ([Fe/H]) of 0.04, or 109% the solar amount. This is particularly odd as such low-mass stars near the boundary between brown dwarfs and hydrogen-fusing stars should be expected to have considerably less metal content than the Sun. Its luminosity (L) is 0.05% of that of the Sun.

The star's apparent magnitude, or how bright it appears from Earth's perspective, is 18.8. Therefore, it is too dim to be seen with the naked eye.


TRAPPIST-1f orbits its host star with an orbital period of about 9.206 days and an orbital radius of about 0.037 times that of Earth's (compared to the distance of Mercury from the Sun, which is about 0.38 AU).


Artist's impression of the surface of TRAPPIST-1f, depicting a liquid water ocean on its surface. The parent star and neighbouring planets are also illustrated.

The exoplanet was announced to be either orbiting within or slightly outside of the habitable zone of its parent star, the region where, with the correct conditions and atmospheric properties, liquid water may exist on the surface of the planet. On 31 August 2017, astronomers at the Hubble Space Telescope reported the first evidence of possible water content on the TRAPPIST-1 exoplanets.[8][9]

TRAPPIST-1f has a radius about the same as Earth, at around 1.045 R, but only about two thirds of Earth's mass, at around 0.68 M. So, it is considered somewhat unlikely to be a fully rocky planet, and extremely unlikely to be an Earth-like one, that is rocky with a large iron core but without a thick hydrogen-helium atmosphere enveloping the planet. Simulations strongly suggest the planet is approximately 20% water by composition. With such a massive water envelope, the pressure and temperature will be high enough to keep the water in a gaseous state and any liquid water will only exist as clouds near the top of TRAPPIST-1f’s atmosphere. Trappist-1f is therefore likely to be no more habitable than any other gas or ice-giant with water clouds in its atmosphere.[4]

Its host star is a red ultracool dwarf, with only about 8% of the mass of the Sun (close to the boundary between brown dwarfs and hydrogen-fusing stars). As a result, stars like TRAPPIST-1 have the ability to live up to 4–5 trillion years, 400–500 times longer than the Sun will live.[10] Because of this ability to live for long periods of time, it is likely TRAPPIST-1 will be one of the last remaining stars when the Universe is much older than it is now, when the gas needed to form new stars will be exhausted, and the remaining ones begin to die off.

The planet is very likely tidally locked, with one hemisphere permanently facing towards the star, while the opposite side shrouded in eternal darkness. However, between these two intense areas, there would be a sliver of habitability – called the terminator line, where the temperatures may be suitable (about 273 K or 0 °C or 32 °F) for liquid water to exist.[citation needed] Additionally, a much larger portion of the planet may be habitable if it supports a thick enough atmosphere to transfer heat to the side facing away from the star.[citation needed]

See also[edit]


  1. ^ Cutri, R.M.; Skrutskie, M.F.; Van Dyk, S.; Beichman, C.A.; Carpenter, J.M.; Chester, T.; Cambresy, L.; Evans, T.; Fowler, J.; Gizis, J.; Howard, E.; Huchra, J.; Jarrett, T.; Kopan, E.L.; Kirkpatrick, J.D.; Light, R.M.; Marsh, K.A.; McCallon, H.; Schneider, S.; Stiening, R.; Sykes, M.; Weinberg, M.; Wheaton, W.A.; Wheelock, S.; Zacarias, N. (June 2003). "2MASS All Sky Catalog of point sources". VizieR Online Data Catalog. European Southern Observatory with data provided by the SAO/NASA Astrophysics Data System. 2246. Bibcode:2003yCat.2246....0C. 
  2. ^ Costa, E.; Mendez, R.A.; Jao, W.-C.; Henry, T.J.; Subasavage, J.P.; Ianna, P.A. (August 4, 2006). "The Solar Neighborhood. XVI. Parallaxes from CTIOPI: Final Results from the 1.5 m Telescope Program" (PDF). The Astronomical Journal. The American Astronomical Society. 132 (3): 1234. Bibcode:2006AJ....132.1234C. CiteSeerX accessible. doi:10.1086/505706. 
  3. ^ a b c Gillon, Michaël; Triaud, Amaury H. M. J.; Demory, Brice-Olivier; Jehin, Emmanuël; Agol, Eric; Deck, Katherine M.; Lederer, Susan M.; Wit, Julien de; Burdanov, Artem (2017). "Seven temperate terrestrial planets around the nearby ultracool dwarf star TRAPPIST-1". Nature. 542 (7642): 456–460. arXiv:1703.01424Freely accessible. Bibcode:2017Natur.542..456G. doi:10.1038/nature21360. PMID 28230125. 
  4. ^ a b c d Quarles, Billy; Quintana, Elisa V.; Lopez, Eric D.; Schlieder, Joshua E.; Barclay, Thomas (2017). "Plausible Compositions of the Seven TRAPPIST-1 Planets Using Long-term Dynamical Simulations". The Astrophysical Journal. 842: L5. arXiv:1704.02261Freely accessible. Bibcode:2017ApJ...842L...5Q. doi:10.3847/2041-8213/aa74bf. 
  5. ^ "NASA telescope reveals largest batch of Earth-size, habitable-zone planets around single star". Exoplanet Exploration: Planets Beyond our Solar System (Press release). Retrieved 22 February 2017. 
  6. ^ Fraser Cain (16 September 2008). "How Old is the Sun?". Universe Today. Retrieved 19 February 2011. 
  7. ^ Fraser Cain (15 September 2008). "Temperature of the Sun". Universe Today. Retrieved 19 February 2011. 
  8. ^ Bourrier, Vincent; de Wit, Julien; Jäger, Mathias (31 August 2017). "Hubble delivers first hints of possible water content of TRAPPIST-1 planets". Retrieved 4 September 2017. 
  9. ^ PTI (4 September 2017). "First evidence of water found on TRAPPIST-1 planets]". The Indian Express. Retrieved 4 September 2017. 
  10. ^ Adams, Fred C.; Laughlin, Gregory; Graves, Genevieve J. M. "Red Dwarfs and the End of the Main Sequence". Gravitational Collapse: From Massive Stars to Planets. Revista Mexicana de Astronomía y Astrofísica. pp. 46–49. Bibcode:2004RMxAC..22...46A. 

External links[edit]