TRAPPIST-1f
{{short description|Earth-size exoplanet orbiting TRAPPIST-1}}
{{Use dmy dates|date=March 2019}}
{{Infobox planet
| name = TRAPPIST-1f
| image = TRAPPIST-1f artist impression 2018.png
| caption = Artist's impression of TRAPPIST-1f. (February 2018)
| discoverer = Michaël Gillon et al.
| discovery_site = Spitzer Space Telescope
| discovered = 22 February 2017
| discovery_method = Transit
| apsis = astron
| semimajor = {{val|0.03849|0.00033|ul=AU}}
| eccentricity = {{val|0.01007|0.00068}}
| period = {{val|9.207540|0.000032|ul=d}}
| inclination = {{val|89.740|0.019|u=deg}}
| arg_peri = {{val|368.81|3.11|u=deg}}
| star = TRAPPIST-1
| mean_radius = {{val|1.045|0.013|0.012|ul=Earth radius}}
| mass = {{val|1.039|0.031|ul=Earth mass}}
| density = {{val|5.009|0.138|0.158|ul=g/cm3}}
| surface_grav = {{val|0.951|0.024}} g
{{val|9.32|0.24|ul=m/s2}}
| single_temperature = Teq: {{val|217.7|2.1|ul=K}} ({{convert|217.7|K|C F|disp=out}})
}}
TRAPPIST-1f is an exoplanet, likely rocky, orbiting within the habitable zone{{Cite press release|title=NASA telescope reveals largest batch of Earth-size, habitable-zone planets around single star|url=https://exoplanets.nasa.gov/news/1419/nasa-telescope-reveals-largest-batch-of-earth-size-habitable-zone-planets-around-single-star/|access-date=22 February 2017|newspaper=Exoplanet Exploration: Planets Beyond our Solar System}} around the ultracool dwarf star TRAPPIST-1, located {{convert|40.7|ly|pc|lk=on|abbr=off}} 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 in 2017 using observations from the Spitzer Space Telescope.
The planet is likely tidally locked, and has been depicted as an eyeball planet in artistic impressions by NASA.
Physical characteristics
=Mass, radius, and temperature=
TRAPPIST-1f is an Earth-sized exoplanet, meaning it has a radius close to that of Earth. It has an equilibrium temperature of {{convert|218|K|C F}}. It has a radius of {{val|1.045|ul=Earth radius}} and a mass of {{val|1.039|ul=Earth mass}}. It was initially estimated to have a much lower mass, and thus a low density of {{val|3.3|0.9|u=g/cm3}} and a surface gravity around {{val|6.1|u=m/s2}} (62% of Earth's value). This suggested a large amount of volatiles, with a 2017 study suggesting that a water ocean may comprise as much as 20% of the planet's mass, increasing the temperature at the bottom of such an ocean to above {{convert|1400|K|C F}}. However, refined density estimates show that TRAPPIST-1f, like other planets in the system, is only slightly less dense than Earth, consistent with a rocky composition.
=Atmosphere=
According to simulations of magma ocean-atmosphere interaction, TRAPPIST-1f is likely to retain a fraction of primordial steam atmosphere during the initial stages of evolution, and therefore today is likely to possess a thick ocean covered by atmosphere rich in abiotic oxygen.{{citation|arxiv=2008.09599|title=Magma Ocean Evolution of the TRAPPIST-1 Planets|year=2021|doi=10.1089/ast.2020.2277 |last1=Barth |first1=Patrick |last2=Carone |first2=Ludmila |last3=Barnes |first3=Rory |last4=Noack |first4=Lena |last5=Mollière |first5=Paul |last6=Henning |first6=Thomas |journal=Astrobiology |volume=21 |issue=11 |pages=1325–1349 |pmid=34314604 |bibcode=2021AsBio..21.1325B |s2cid=221246323 }} Helium emission from TRAPPIST-1f (and planets b and e) has not been detected as of 2022.{{citation|arxiv=2106.11444|year=2021|title=Nondetection of Helium in the Upper Atmospheres of TRAPPIST-1b, e, and F|doi=10.3847/1538-3881/ac0d57 |last1=Krishnamurthy |first1=Vigneshwaran |last2=Hirano |first2=Teruyuki |last3=Stefánsson |first3=Gumundur |last4=Ninan |first4=Joe P. |last5=Mahadevan |first5=Suvrath |last6=Gaidos |first6=Eric |last7=Kopparapu |first7=Ravi |last8=Sato |first8=Bunei |last9=Hori |first9=Yasunori |last10=Bender |first10=Chad F. |last11=Cañas |first11=Caleb I. |last12=Diddams |first12=Scott A. |last13=Halverson |first13=Samuel |last14=Harakawa |first14=Hiroki |last15=Hawley |first15=Suzanne |last16=Hearty |first16=Fred |last17=Hebb |first17=Leslie |last18=Hodapp |first18=Klaus |last19=Jacobson |first19=Shane |last20=Kanodia |first20=Shubham |last21=Konishi |first21=Mihoko |last22=Kotani |first22=Takayuki |last23=Kowalski |first23=Adam |last24=Kudo |first24=Tomoyuki |last25=Kurokawa |first25=Takashi |last26=Kuzuhara |first26=Masayuki |last27=Lin |first27=Andrea |last28=Maney |first28=Marissa |last29=Metcalf |first29=Andrew J. |last30=Morris |first30=Brett |journal=The Astronomical Journal |volume=162 |issue=3 |page=82 |bibcode=2021AJ....162...82K |display-authors=1 |doi-access=free }}
=Host star=
The planet orbits an (M-type) ultracool dwarf star named TRAPPIST-1. The star has a mass of 0.08 {{solar mass}} and a radius of 0.11 {{solar radius}}. It has a temperature of 2550 K and is at least 7-8 billion years old. In comparison, the Sun is 4.6 billion years old{{cite web |url=http://www.universetoday.com/18237/how-old-is-the-sun/ |title=How Old is the Sun? |author=Fraser Cain |date=16 September 2008 |publisher=Universe Today |access-date=19 February 2011}} and has a temperature of 5778 K.{{cite web |url=http://www.universetoday.com/18092/temperature-of-the-sun/ |title=Temperature of the Sun |author=Fraser Cain |date=15 September 2008 |publisher=Universe Today |access-date=19 February 2011}} 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; on the other hand, metal-rich stars are also more likely to have planets than metal-poor ones. Its luminosity ({{solar luminosity|link=y}}) 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.
=Orbit=
Habitability
{{see also|Habitability of red dwarf systems}}
File:PIA21423 - Surface of TRAPPIST-1f.jpg
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.
TRAPPIST-1f has a radius about the same as Earth, at around 1.045 {{Earth radius}}, but was initially thought to have only about two thirds of Earth's mass, at around 0.68 {{Earth mass|sym=y}}. So, it was 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 in 2017 suggested the planet is approximately 20% water by composition, much higher than that of Earth. 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. Based on this study, TRAPPIST-1f is therefore likely to be no more habitable than any other ice giant with water clouds in its atmosphere. However, refined estimates show that TRAPPIST-1f has about the same mass as Earth, and like other planets in the system, is only slightly less dense than Earth, consistent with a rocky composition.
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. 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 moderate temperature – called the terminator line, where the temperatures may be suitable (about {{convert|273|K|C F|disp=or}}) for liquid water to exist. 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.
See also
References
{{reflist|30em|refs=
| last=Adams | first=Fred C.
| author2=Laughlin, Gregory|author3= Graves, Genevieve J. M.
| title=Red Dwarfs and the End of the Main Sequence
| book-title=Gravitational Collapse: From Massive Stars to Planets
| pages=46–49
| publisher=Revista Mexicana de Astronomía y Astrofísica
| bibcode=2004RMxAC..22...46A
}}
{{cite news |author=PTI |title=First evidence of water found on TRAPPIST-1 planets] |url=http://indianexpress.com/article/technology/science/first-evidence-of-water-found-on-trappist-1-planets-4827977/ |date=4 September 2017 |work=The Indian Express |access-date=4 September 2017 }}
}}
External links
- [https://www.youtube.com/watch?v=ieJIht3fnVM NASA Briefing on the Discovery of TRAPPIST-1's 7 Planets]
{{TRAPPIST-1}}
{{Exoplanet}}
{{2017 in space}}
{{Aquarius (constellation)}}
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Category:Exoplanets discovered in 2017
Category:Near-Earth-sized exoplanets
Category:Near-Earth-sized exoplanets in the habitable zone
Category:Transiting exoplanets