|Right ascension||23h 06m 29.283s|
|Declination||−05° 02′ 28.59″|
|Evolutionary stage||Main sequence|
|Apparent magnitude (V)||±0.08218.798|
|Apparent magnitude (R)||±0.06516.466|
|Apparent magnitude (I)||±0.11514.024|
|Apparent magnitude (J)||±0.02211.354|
|Apparent magnitude (H)||±0.02110.718|
|Apparent magnitude (K)||±0.02310.296|
|V−R color index||2.332|
|R−I color index||2.442|
|J−H color index||0.636|
|J−K color index||1.058|
|Radial velocity (Rv)||±2−54 km/s|
|Proper motion (μ)|| RA: ±1.8922.1 mas/yr |
Dec.: ±1.8−471.9 mas/yr
|Parallax (π)||82.4 ± 0.8 mas|
|Distance||39.6 ± 0.4 ly |
(12.1 ± 0.1 pc)
|Absolute magnitude (MV)||±0.118.4|
|Luminosity (bolometric)||522±0.0000190.000 L☉|
|Luminosity (visual, LV)||003730.000[note 2] L☉|
|Surface gravity (log g)||≈5.227[note 3] cgs|
|Metallicity [Fe/H]||±0.080.04 dex|
|Rotation||±0.003 days 3.295|
|Rotational velocity (v sin i)||6 km/s|
2MASS J23062928-0502285, 2MASSI J2306292-050227, 2MASSW J2306292-050227, 2MUDC 12171
TRAPPIST-1, also designated as 2MASS J23062928-0502285, is an ultra-cool red dwarf star that is slightly larger, but much more massive, than the planet Jupiter; it is located 39.6 light-years (12.1 pc) from the Sun, in the direction described as the constellation Aquarius. Seven temperate terrestrial planets have been detected orbiting the star, a larger number than detected in any other planetary system. A study released in May 2017 suggests that the stability of the system is not particularly surprising if one considers how the planets migrated to their present orbits through a protoplanetary disk.
A team of Belgian astronomers first discovered three Earth-sized planets orbiting the dwarf star in 2015. A team led by Michaël Gillon at the University of Liège in Belgium detected the planets using transit photometry with the Transiting Planets and Planetesimals Small Telescope (TRAPPIST) at the La Silla Observatory in Chile and the Observatoire de l'Oukaïmeden in Morocco. On 22 February 2017, astronomers announced four additional exoplanets around TRAPPIST-1. This work used the Spitzer Space Telescope and the Very Large Telescope at Paranal, among others, and brought the total number of planets to seven, of which three are considered to be within its habitable zone. The others could also be habitable as they may possess liquid water somewhere on their surface. Depending on definition, up to six could be in the optimistic habitable zone (c, d, e, f, g, h), with estimated equilibrium temperatures of -105 to 120 Celsius.
- 1 Discovery and nomenclature
- 2 Stellar characteristics
- 3 Planetary system
- 3.1 Planetary System Data Charts
- 3.2 Orbital near-resonance
- 3.3 Formation of the planetary system
- 3.4 Tidal locking
- 3.5 Tidal heating
- 3.6 Possible effects of strong X-ray and extreme UV irradiation of the system
- 3.7 Spectroscopy of planetary atmospheres
- 3.8 Impact of stellar activity on habitability
- 3.9 Probability of interplanetary panspermia
- 3.10 Existence of undiscovered planets
- 3.11 Radio signal search
- 4 Moons
- 5 Gallery
- 6 See also
- 7 Notes
- 8 References
- 9 Further reading
- 10 External links
Discovery and nomenclature
The star at the center of the system was discovered in 1999 during the Two Micron All-Sky Survey (2MASS). It was entered in the subsequent catalog with the designation "2MASS J23062928-0502285". The numbers refer to the right ascension and declination of the star's position in the sky and the "J" refers to the Julian Epoch.
The system was later studied by a team at the University of Liège, who made their initial observations using the TRAPPIST–South telescope from September to December 2015 and published their findings in the May 2016 issue of the journal Nature. The backronym pays homage to the Catholic Christian religious order of Trappists and to the Trappist beer it produces primarily in Belgium, which the astronomers used to toast their discovery. Since the star hosted the first exoplanets discovered by this telescope, the discoverers accordingly designated it as "TRAPPIST-1".
The planets are designated in the order of their discovery, beginning with b for the first planet discovered, c for the second and so on. Three planets around TRAPPIST-1 were first discovered and designated b, c and d in order of increasing orbital periods, and the second batch of discoveries was similarly designated e to h.
Shortly after the star system was discovered, the game development studio Frontier Developments found that an almost identical system had been procedurally generated by Elite Dangerous's Stellar Forge engine, which used physics based algorithms and simulations to generate an explorable universe.
The system was in the same location with a very similar star and 7 similar planets in an arrangement very much like the system in real life. Frontier ended up simply renaming the system, originally "Core Sys Sector XU-P A5-0" and made a few minor alterations to commemorate the discovery of the system.
TRAPPIST-1 is an ultra-cool dwarf star of spectral class ±0.5 that is approximately 8% the mass of and 11% the radius of the M8.0Sun. Although it is slightly larger than Jupiter, it is about 84 times more massive. High-resolution optical spectroscopy failed to reveal the presence of lithium, suggesting it is a very low-mass main-sequence star, which is fusing hydrogen and has depleted its lithium, i.e., a red dwarf rather than a very young brown dwarf. It has a temperature of 2,511 K (2,238 °C; 4,060 °F), and its age has been estimated to be approximately ±2.2 Ga. 7.6 In comparison, the Sun has a temperature of 5,778 K (5,505 °C; 9,941 °F) and an age of about 4.6 Gyr. Observations with the Kepler K2 extension for a total of 79 days revealed starspots and infrequent weak optical flares at a rate of 0.38 per day (30-fold less frequent than for active M6–M9 dwarfs); a single strong flare appeared near the end of the observation period. The observed flaring activity possibly changes the atmospheres of the orbiting planets on a regular basis, making them less suitable for life. The star has a rotational period of 3.3 days.
High-resolution speckle images of TRAPPIST-1 were obtained and revealed that the M8 star has no companions with a luminosity equal to or brighter than a brown dwarf. This determination that the host star is single confirms that the measured transit depths for the orbiting planets provide a true value for their radii, thus proving that the planets are indeed Earth-sized.
Owing to its low luminosity, the star has the ability to live for up to 12 trillion years. It is metal-rich, with a metallicity ([Fe/H]) of 0.04, or 109% the solar amount. Its luminosity is 0.05% of that of the Sun (L☉), most of which is emitted in the infrared spectrum, and with an apparent magnitude of 18.80 it is not visible to the naked eye from the Earth.
On 22 February 2017, astronomers announced that the planetary system of this star is composed of seven temperate terrestrial planets, of which five (b, c, e, f and g) are similar in size to Earth, and two (d and h) are intermediate in size between Mars and Earth. Three of the planets (e, f and g) orbit within the habitable zone.
The system is very flat and compact. All seven of TRAPPIST-1's planets orbit much closer than Mercury orbits the Sun. Except for TRAPPIST-1b, they orbit farther than the Galilean satellites do around Jupiter, but closer than most of the other moons of Jupiter. The distance between the orbits of TRAPPIST-1b and TRAPPIST-1c is only 1.6 times the distance between the Earth and the Moon. The planets should appear prominently in each other's skies, in some cases appearing several times larger than the Moon appears from Earth. A year on the closest planet passes in only 1.5 Earth days, while the seventh planet's year passes in only 18.8 days.
The planets pass so close to one another that gravitational interactions are significant, and their orbital periods are nearly resonant. In the time the innermost planet completes eight orbits, the second, third, and fourth planets complete five, three, and two. The gravitational tugging also results in transit-timing variations (TTVs), ranging from under a minute to over 30 minutes, which allowed the investigators to calculate the masses of all but the outermost planet. The total mass of the six inner planets is approximately 0.02% the mass of TRAPPIST-1, a fraction similar to that for the Galilean satellites to Jupiter, and an observation suggestive of a similar formation history. The densities of the planets range from ~0.60 to ~1.17 times that of Earth (ρ⊕, 5.51 g/cm3), indicating predominantly rocky compositions. The uncertainties are too large to indicate whether a substantial component of volatiles is also included, except in the case of f, where the value (±0.17 ρ⊕) "favors" the presence of a layer of 0.60ice and/or an extended atmosphere. Speckle imaging excludes all possible stellar and brown dwarf companions.
Between 18 February and 27 March 2017, a team of astronomers used the Spitzer Space Telescope to observe TRAPPIST-1 to refine the orbital and physical parameters of the seven planets using updated parameters for the star. Their results were published on 9 January 2018. Although no new mass estimates were given, the team managed to refine the orbital parameters and radii of the planets within a very small error margin. In addition to updated planetary parameters, the team also found evidence for a large, hot atmosphere around the innermost planet.
On 5 February 2018, a collaborative study by an international group of scientists using the Hubble Space Telescope, the Kepler Space Telescope, the Spitzer Space Telescope, and the ESO's SPECULOOS telescope released the most accurate parameters for the TRAPPIST-1 system yet. They were able to refine the masses of the seven planets to a very small error margin, allowing the density, surface gravity, and composition of the planets to be accurately determined. The planets range in mass from about 0.3 M⊕ to 1.16 M⊕, with densities from 0.62 ρ⊕ (3.4 g/cm3) to 1.02 ρ⊕ (5.6 g/cm3). Planets c and e are almost entirely rocky, while b, d, f, g, and h have a layer of volatiles in the form of either a water shell, an ice shell, or a thick atmosphere. TRAPPIST-1d appears to have a liquid water ocean comprising about 5% of its mass—for comparison, Earth's water content is < 0.1%—while the water layers of TRAPPIST-1f and g are likely frozen. TRAPPIST-1e has a slightly higher density than Earth, indicating a terrestrial rock and iron composition. In addition, the atmospheres of the planets were further analyzed. The atmosphere of TRAPPIST-1b was found to be over the runaway greenhouse limit with an estimated 101 to 104 bar of water vapor. Planets c, d, e, and f lack hydrogen-helium atmospheres. Planet g was also observed, but there wasn't enough data to firmly rule out a hydrogen atmosphere.
Planetary System Data Charts
(in order from star)
|0.01154775 (1.73 million km)||87637±0.00000039 1.510||22±0.00304 0.006||±0.2389.56°||+0.031|
|0.01581512 (2.37 million km)||80746±0.00000091 2.421||54±0.00188 0.006||±0.1889.70°||+0.030|
|0.02228038 (3.33 million km)||959±0.000078 4.049||37±0.00093 0.008||+0.08
|0.02928285 (4.38 million km)||043±0.000015 6.099||10±0.00058 0.005||+0.053
|0.03853361 (5.76 million km)||585±0.000016 9.205||07±0.00068 0.010||+0.026
|0.04687692 (7.01 million km)||473±0.000018 12.354||08±0.00058 0.002||+0.019
|0.06193488 (9.27 million km)||953±0.000080 18.767||67±0.00121 0.005||±0.02389.796°||+0.026|
||Surface Gravity |
|b||3.88 ± 0.22||391.8 ± 5.5 K (118.65 ± 5.50 °C; 245.57 ± 9.90 °F) (equilibrium)
≥1,400 K (1,130 °C; 2,060 °F) (atmosphere)
750–1,500 K (477–1,227 °C; 890–2,240 °F) (surface)
|c||2.07 ± 0.12||334.8 ± 4.7 K (61.65 ± 4.70 °C; 142.97 ± 8.46 °F) (equilibrium) (for a null albedo)||0.966 +0.087|
|282.1 ± 4.0 K (8.95 ± 4.00 °C; 48.11 ± 7.20 °F) (for a null albedo)||0.483 +0.048|
|e||±0.0340.604||246.1 ± 3.5 K (−27.05 ± 3.50 °C; −16.69 ± 6.30 °F)||+0.063|
|f||0.382 (± 0.03)||219 K (−54 °C; −65 °F), ≳1,400 K (1,130 °C; 2,060 °F)||~0.62|
|g||0.258 ± 0.020||198.6 ± 3.8 K (−74.55 ± 3.80 °C; −102.19 ± 6.84 °F)||~1.06|
|h||~0.15||169 K (−104 °C; −155 °F)||~0.17|
The orbital motions of the TRAPPIST-1 planets form a complex chain with three-body Laplace-type resonances linking every member. The relative orbital periods (proceeding outward) approximate whole integer ratios of 24/24, 24/15, 24/9, 24/6, 24/4, 24/3, and 24/2, respectively, or nearest-neighbor period ratios of about 8/5, 5/3, 3/2, 3/2, 4/3, and 3/2 (1.603, 1.672, 1.506, 1.509, 1.342, and 1.519). This represents the longest known chain of near-resonant exoplanets, and is thought to have resulted from interactions between the planets as they migrated inward within the residual protoplanetary disk after forming at greater initial distances.
Most sets of orbits similar to the set found at TRAPPIST-1 are unstable, causing one planet to come within the Hill sphere of another or to be thrown out. But it has been found that there is a way for a system to migrate into a fairly stable state through damping interactions with, for example, a protoplanetary disk. After this, tidal forces can give the system a long-term stability.
The tight correspondence between whole number ratios in orbital resonances and in music theory has made it possible to convert the system's motion into music.
Formation of the planetary system
According to Ormel et al. previous models of planetary formation do not explain the formation of the highly compact TRAPPIST-1 system. Formation in place would require an unusually dense disk and would not readily account for the orbital resonances. Formation outside the frost line does not explain the planets' terrestrial nature or Earth-like masses. The authors proposed a new scenario in which planet formation starts at the frost line where pebble-size particles trigger streaming instabilities, then protoplanets quickly mature by pebble accretion. When the planets reach Earth mass they create perturbations in the gas disk that halt the inward drift of pebbles causing their growth to stall. The planets are transported by Type I migration to the inner disk, where they stall at the magnetospheric cavity and end up in mean motion resonances. Such inward migration increases the odds of substantial amounts of water being present on these worlds.
All seven planets are likely to be tidally locked (one side of each planet permanently facing the star), making the development of life there "much more challenging". A less likely possibility is that some may be trapped in a higher-order spin–orbit resonance. Tidally locked planets would typically have very large temperature differences between their permanently lit day sides and their permanently dark night sides, which could produce very strong winds circling the planets. The best places for life may be close to the mild twilight regions between the two sides, called the terminator line.
Tidal heating is predicted to be significant: all planets except f and h are expected to have a tidal heat flux greater than Earth's total heat flux. With the exception of TRAPPIST-1c, all of the planets have densities low enough to indicate the presence of significant H2O in some form. Planets b and c experience enough heating from planetary tides to maintain magma oceans in their rock mantles; planet c may have eruptions of silicate magma on its surface. Tidal heat fluxes on planets d, e, and f are lower, but are still twenty times higher than Earth's mean heat flow. Planets d and e are the most likely to be habitable. Planet d avoids the runaway greenhouse state if its albedo is ≳ 0.3.
Possible effects of strong X-ray and extreme UV irradiation of the system
Bolmont et al. modelled the effects of predicted far ultraviolet (FUV) and extreme ultraviolet (EUV/XUV) irradiation of planets b and c by TRAPPIST-1. Their results suggest that the two planets may have lost as much as 15 Earth oceans of water (although the actual loss would probably be lower), depending on their initial water contents. Nonetheless, they may have retained enough water to remain habitable, and a planet orbiting further out was predicted to lose much less water.
However, a subsequent XMM-Newton X-ray study by Wheatley et al. found that the star emits X-rays at a level comparable to our own much larger Sun, and extreme ultraviolet radiation at a level 50-fold stronger than assumed by Bolmont et al. The authors predicted this would significantly alter the primary and perhaps secondary atmospheres of close-in, Earth-sized planets spanning the habitable zone of the star. The publication noted that these levels "neglected the radiation physics and hydrodynamics of the planetary atmosphere" and could be a significant overestimate. Indeed, the XUV stripping of a very thick hydrogen and helium primary atmosphere might actually be required for habitability. The high levels of XUV would also be expected to make water retention on TRAPPIST-1d less likely than predicted by Bolmont et al., though even on highly irradiated planets it might remain in cold traps at the poles or on the night sides of tidally locked planets.
If a dense atmosphere like Earth's, with a protective ozone layer, exists on planets in the habitable zone of TRAPPIST-1, UV surface environments would be similar to present-day Earth. However, an anoxic atmosphere would allow more UV to reach the surface, making surface environments hostile to even highly UV-tolerant terrestrial extremophiles. If future observations detect ozone on one of the TRAPPIST-1 planets, it would be a prime candidate to search for surface life.
Spectroscopy of planetary atmospheres
Because of the system's relative proximity, the small size of the primary and the orbital alignments that produce daily transits, the atmospheres of TRAPPIST-1's planets are favorable targets for transmission spectroscopy investigation.
The combined transmission spectrum of TRAPPIST-1b and c, obtained by the Hubble Space Telescope, rules out a cloud-free hydrogen-dominated atmosphere for each planet, so they are unlikely to harbor an extended gas envelope, unless it is cloudy out to high altitudes. Other atmospheric structures, from a cloud-free water-vapor atmosphere to a Venus-like atmosphere, remain consistent with the featureless spectrum.
Another study hinted at the presence of hydrogen exospheres around the two inner planets with an exospheric disks extending up to 7 times the planets' radii.
In a paper by an international collaboration using data from space and ground-based telescopes, it was found that TRAPPIST-1 c and TRAPPIST-1 e likely have largely rocky interiors, and that TRAPPIST-1 b is the only planet above the runaway green-house limit, with pressures of water vapour of the order of 101-104 bar.
Observations by future telescopes, such as the James Webb Space Telescope or European Extremely Large Telescope, will be able to assess the greenhouse gas content of the atmospheres, allowing better estimation of surface conditions. They may also be able to detect biosignatures like ozone or methane in the atmospheres of these planets, if life is present there.
Impact of stellar activity on habitability
The K2 observations of Kepler revealed several flares on the host star. The energy of the strongest event was comparable to the Carrington event, one of the strongest flares seen on the Sun. As the planets in TRAPPIST-1 system orbit much closer to their host star than Earth, such eruptions could cause 10–10000 times stronger magnetic storms than the most powerful geomagnetic storms on Earth. Beside the direct harm caused by the radiation associated with the eruptions, they can also pose further threats: the chemical composition of the planetary atmospheres is probably altered by the eruptions on a regular basis, and the atmospheres can be also eroded in the long term. A sufficiently strong magnetic field of the exoplanets could protect their atmosphere from the harmful effects of such eruptions, but an Earth-like exoplanet would need a magnetic field in the order of 10–1000 Gauss to be shielded from such flares (as a comparison, the Earth's magnetic field is ≈0.5 Gauss).
Probability of interplanetary panspermia
Existence of undiscovered planets
One study using the CAPSCam astrometric camera concluded that the TRAPPIST-1 system has no planets massing at least 4.6 Jupiter masses with year-long orbits and no planets massing at least 1.6 Jupiter masses with five-year orbits. The authors of the study noted, however, that their findings left areas of the TRAPPIST-1 system, most notably the zone in which planets would have intermediate-period orbits, unanalyzed.
Radio signal search
In February 2017, Seth Shostak, senior astronomer for the SETI Institute, noted: "... the SETI Institute used its Allen Telescope Array [in 2016] to observe the environs of TRAPPIST-1, scanning through 10 billion radio channels in search of signals. No transmissions were detected, although new observations are in the offing ..."
Stephen R. Kane, writing in The Astrophysical Journal Letters, notes that TRAPPIST-1 planets are unlikely to have large moons. The Earth's Moon has a radius 27% that of Earth, so its area (and its transit depth) is 7.4% that of Earth, which would likely have been noted in the transit study if present. Smaller moons of 200–300 km (120–190 mi) radius would likely not have been detected.
At a theoretical level, Kane found that moons around the inner TRAPPIST-1 planets would need to be extraordinarily dense to be even theoretically possible. This is based on a comparison of the Hill sphere, which marks the outer limit of a moon's possible orbit by defining the region of space in which a planet's gravity is stronger than the tidal force of its star, and the Roche limit, which represents the smallest distance at which a moon can orbit before the planet's tides exceed its own gravity and pull it apart. These constraints do not rule out the presence of ring systems (where particles are held together by chemical rather than gravitational forces). The mathematical derivation is as follows:
is the Hill radius of the planet, calculated from the planetary semi-major axis , the mass of the planet , and the mass of the star . Note that the mass of the TRAPPIST-1 star is approximately 26,000 M⊕ (see data table above); the remaining figures are provided in the table below.
is the Roche limit of the planet, calculated from the radius of the planet , and the density of the planet .
Kane notes that moons near the edge of the Hill radius may be subject to resonant removal during planetary migration, leading to a Hill reduction factor roughly estimated as 1/3 for typical systems and 1/4 for the TRAPPIST-1 system; thus moons are not expected for the planets where is less than four. Furthermore, tidal interactions with the planet can result in a transfer of energy from the planet's rotation to the moon's orbit, causing a moon to leave the stable region over time. For these reasons, even the outer TRAPPIST-1 planets are believed to be unlikely to have moons.
TRAPPIST-1 is a smaller (11% the size), fainter and redder star than the Sun
TRAPPIST-1c landscape (artist concept)
Dimming of TRAPPIST-1 due to its seven known planets - large planets, more dimming; distant ones, longer (Spitzer Space Telescope)
This artist's impression video compares the seven planets orbiting the star at the same scale.
- HD 10180, a star with at least seven known planets
- Kepler-90, a star with eight known planets
- KIC 8462852, another star with notable transit data
- Active SETI, the attempt to transmit messages to intelligent extraterrestrial life
- Habitability of red dwarf systems
- List of potentially habitable exoplanets
- Based on photometric spectral type estimation.
- Taking the absolute visual magnitude of TRAPPIST-1 and the absolute visual magnitude of the Sun , the visual luminosity can be calculated by
- The surface gravity is calculated directly from Newton's law of universal gravitation, which gives the formula , where M is the mass of the object, r is its radius, and G is the gravitational constant. In this case, a log g of ≈5.227 indicates a surface gravity around 172 times stronger than Earth's.
- Cutri, R. M.; Skrutskie, M. F.; Van Dyk, S.; et al. (June 2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". CDS/ADC Collection of Electronic Catalogues (2246). Bibcode:2003yCat.2246....0C.
- Costa, E.; Mendez, R. A.; Jao, W.-C.; Henry, T. J.; Subasavage, J. P.; Ianna, P. A. (4 August 2006). "The Solar Neighborhood. XVI. Parallaxes from CTIOPI: Final Results from the 1.5 m Telescope Program". The Astronomical Journal. 132 (3): 1234. Bibcode:2006AJ....132.1234C. CiteSeerX . doi:10.1086/505706.
- Van Grootel, Valerie; Fernandes, Catarina S.; Gillon, Michaël; et al. (January 2018). "Stellar parameters for TRAPPIST-1". The Astrophysical Journal. 853 (1): 30. arXiv: . Bibcode:2018ApJ...853...30V. doi:10.3847/1538-4357/aaa023. More than one of
- Viti, Serena; Jones, Hugh R. A. (November 1999). "Gravity dependence at the bottom of the main sequence". Astronomy and Astrophysics. 351: 1028–1035. Bibcode:1999A&A...351.1028V. Retrieved 6 May 2016.
- Delrez, Laetitia; Gillon, Michael; H.M.J, Amaury; et al. (April 2018). "Early 2017 observations of TRAPPIST-1 with Spitzer". Monthly Notices of the Royal Astronomical Society. 475 (3): 3577–3597. arXiv: . Bibcode:2018MNRAS.475.3577D. doi:10.1093/mnras/sty051.
- Vida, Krisztián; Kővári, Zsolt; Pál, András; et al. (June 2017). "Frequent Flaring in the TRAPPIST-1 System—Unsuited for Life?". The Astrophysical Journal. 841 (2): 124. arXiv: . Bibcode:2017ApJ...841..124V. doi:10.3847/1538-4357/aa6f05. More than one of
- Barnes, J. R.; Jenkins, J. S.; Jones, H. R. A.; et al. (April 2014). "Precision radial velocities of 15 M5-M9 dwarfs". Monthly Notices of the Royal Astronomical Society. 439 (3): 3094–3113. arXiv: . Bibcode:2014MNRAS.439.3094B. doi:10.1093/mnras/stu172.
- Burgasser, Adam J.; Mamajek, Eric E. (September 2017). "On the Age of the TRAPPIST-1 System". The Astrophysical Journal. 845 (2): 110. arXiv: . Bibcode:2017ApJ...845..110B. doi:10.3847/1538-4357/aa7fea. More than one of
- "2MASS J23062928-0502285". SIMBAD. Centre de données astronomiques de Strasbourg.
- Gillon, M.; Jehin, E.; Lederer, S. M.; Delrez, L.; De Wit, J.; Burdanov, A.; Van Grootel, V.; Burgasser, A. J.; Triaud, A. H. M. J.; Opitom, C.; Demory, B.-O.; Sahu, D. K.; Bardalez Gagliuffi, D.; Magain, P.; Queloz, D. (2016). "Temperate Earth-sized planets transiting a nearby ultracool dwarf star" (PDF). Nature. 533 (7602): 221–224. arXiv: . Bibcode:2016Natur.533..221G. doi:10.1038/nature17448. PMID 27135924.
- "Three Potentially Habitable Worlds Found Around Nearby Ultracool Dwarf Star – Currently the best place to search for life beyond the Solar System". European Southern Observatory.
- Chang, Kenneth (22 February 2017). "7 Earth-Size Planets Identified in Orbit Around a Dwarf Star". The New York Times. Retrieved 22 February 2017.
- "Twinkle, Twinkle Little Trappist". The New York Times. 24 February 2017. Retrieved 27 February 2017.
- Witze, A. (22 February 2017). "These seven alien worlds could help explain how planets form". Nature. doi:10.1038/nature.2017.21512.
- Marchis, Franck (22 February 2017). "Wonderful potentially habitable worlds around TRAPPIST-1". The Planetary Society. Retrieved 25 February 2017.
- Tamayo, Daniel; Rein, Hanno; Petrovich, Cristobal; Murray, Norman (10 May 2017). "Convergent Migration Renders TRAPPIST-1 Long-lived". The Astrophysical Journal Letters. 840 (2): L19. arXiv: . Bibcode:2017ApJ...840L..19T. doi:10.3847/2041-8213/aa70ea. More than one of
- Chang, Kenneth (10 May 2017). "The Harmony That Keeps Trappist-1's 7 Earth-size Worlds From Colliding". The New York Times. Retrieved 11 May 2017.
- Sample, Ian (2 May 2016). "Could these newly-discovered planets orbiting an ultracool dwarf host life?". The Guardian. Retrieved 2 May 2016.
- Bennett, Jay (2 May 2016). "Three New Planets Are the Best Bets for Life". Popular Mechanics. Retrieved 2 May 2016.
- Shostak, Seth (22 February 2017). "This Weird Planetary System Seems Like Something From Science Fiction". NBC News. Retrieved 1 March 2017.
- Gillon, Michaël; Triaud, Amaury; Jehin, Emmanuël; et al. (22 February 2017). "Ultracool Dwarf and the Seven Planets". European Southern Observatory. eso1706. Retrieved 1 May 2017.
- Landau, Elizabeth; Chou, Felicia; Potter, Sean (21 February 2017). "NASA telescope reveals largest batch of Earth-size, habitable-zone planets around single star". Exoplanet Exploration. NASA. Retrieved 22 February 2017.
- Bolmont, E.; Selsis, F.; Owen, J. E.; Ribas, I.; Raymond, S. N.; Leconte, J.; Gillon, M. (2017). "Water loss from terrestrial planets orbiting ultracool dwarfs: implications for the planets of TRAPPIST-1". Monthly Notices of the Royal Astronomical Society. 464 (3): 3728–3741. arXiv: . Bibcode:2017MNRAS.464.3728B. doi:10.1093/mnras/stw2578.
- "Early 2017 observations of TRAPPIST-1 with Spitzer" Derez, L. et al. Available at https://arxiv.org/pdf/1801.02554.pdf. Accessed 4 February 2018
- Bryant, Tracey (22 February 2017). "Celestial Connection". University of Delaware.
- Gizis, John E.; Monet, David G.; Reid, I. Neill; Kirkpatrick, J. Davy; Liebert, James; Williams, Rik J. (2000). "New Neighbors from 2MASS: Activity and Kinematics at the Bottom of the Main Sequence". The Astronomical Journal. 120 (2): 1085–1095. arXiv: . Bibcode:2000AJ....120.1085G. doi:10.1086/301456.
- Gramer, Robbie (22 February 2017). "News So Foreign It's Out of This World: Scientists Discover Seven New Potentially Habitable Planets". Foreign Policy.
Scientists named the system TRAPPIST-1 after the telescope that first found the system. (For all those Belgian beer lovers out there, the telescope’s name is an homage to the trappist religious orders in Belgium, known for brewing some of the world’s best beers.)
- Jehin, Emmanuël; Queloz, Didier; Boffin, Henri; et al. (8 June 2010). "New National Telescope at La Silla". European Southern Observatory. eso1023. Retrieved 4 January 2015.
- Hessman, F. V.; Dhillon, V. S.; Winget, D. E.; et al. (3 December 2010). "On the naming convention used for multiple star systems and extrasolar planets". arXiv: [astro-ph.SR].
- "Elite: Dangerous 'predicted' the discovery of the Trappist-1 system". Polygon. Retrieved 2018-07-29.
- Koberlein, Brian (22 February 2017). "Here's How Astronomers Found Seven Earth-Sized Planets Around A Dwarf Star". Forbes. Retrieved 26 February 2017.
- Reiners, A.; Basri, G. (February 2010). "A Volume-Limited Sample of 63 M7-M9.5 Dwarfs. II. Activity, Magnetism, and the Fade of the Rotation-Dominated Dynamo". The Astrophysical Journal. 710 (2): 924–935. arXiv: . Bibcode:2010ApJ...710..924R. doi:10.1088/0004-637X/710/2/924.
- Cain, Fraser (23 December 2015). "Temperature of the Sun". Universe Today. Retrieved 19 February 2017.
- Williams, Matt (24 September 2016). "What is the Life Cycle of the Sun?". Universe Today. Retrieved 19 February 2011.
- Luger, Rodrigo; Sestovic, Marko; Kruse, Ethan; Grimm, Simon L.; Demory, Brice-Oliver; et al. (12 March 2017). "A terrestrial-sized exoplanet at the snow line of TRAPPIST-1". Nature Astronomy. 1 (6): 0129. arXiv: [astro-ph.EP]. Bibcode:2017NatAs...1E.129L. doi:10.1038/s41550-017-0129.
- Howell, S.; Everett, M.; Horch, E. (September 2016). "Speckle Imaging Excludes Low-mass Companions Orbiting the Exoplanet Host Star TRAPPIST-1". The Astrophysical Journal Letters. 829 (1): 2–9. arXiv: . Bibcode:2016ApJ...829L...2H. doi:10.3847/2041-8205/829/1/L2.
- Adams, Fred C.; Laughlin, Gregory; Graves, Genevieve J. M. (December 2004). "Red Dwarfs and the End of the Main Sequence". Gravitational Collapse: From Massive Stars to Planets. Revista Mexicana de Astronomía y Astrofísica Conference Series. 22. National Autonomous University of Mexico. pp. 46–49. Bibcode:2004RMxAC..22...46A. ISBN 978-970-32-1160-9.
- "TRAPPIST-1 Planets Probably Rich in Water – First glimpse of what Earth-sized exoplanets are made of". www.eso.org. Retrieved 7 February 2018.
- Gillon, M.; Triaud, A. H. M. J.; Demory, B.-O.; et al. (February 2017). "Seven temperate terrestrial planets around the nearby ultracool dwarf star TRAPPIST-1" (PDF). Nature. 542 (7642): 456–460. arXiv: . Bibcode:2017Natur.542..456G. doi:10.1038/nature21360. PMC . PMID 28230125.
- Chou, Felicia; Potter, Sean; Landau, Elizabeth (22 February 2017). "NASA Telescope Reveals Largest Batch of Earth-Size, Habitable-Zone Planets Around Single Star". NASA. Release 17-015.
- "TRAPPIST-1 Planet Lineup". NASA / Jet Propulsion Laboratory. 22 February 2017.
- Wall, Mike (22 February 2017). "Major Discovery! 7 Earth-Size Alien Planets Circle Nearby Star". Space.com.
- Redd, Nola Taylor (24 February 2017). "TRAPPIST-1: System with 7 Earth-Size Exoplanets". Space.com.
- Snellen, Ignas A. G. (23 February 2017). "Astronomy: Earth's seven sisters". Nature. 542 (7642): 421–423. Bibcode:2017Natur.542..421S. doi:10.1038/542421a.
- Howell, Steve B.; Everett, Mark E.; Horch, Elliott P.; et al. (September 2016). "Speckle Imaging Excludes Low-mass Companions Orbiting the Exoplanet Host Star TRAPPIST-1". The Astrophysical Journal Letters. 829 (1): L2. arXiv: . Bibcode:2016ApJ...829L...2H. doi:10.3847/2041-8205/829/1/L2. More than one of
- Bourrier, Vincent; de Wit, Julien; Jäger, Mathias (31 August 2017). "Hubble delivers first hints of possible water content of TRAPPIST-1 planets". SpaceTelescope.org. Retrieved 4 September 2017.
- "First evidence of water found on TRAPPIST-1 planets". The Indian Express. Press Trust of India. 4 September 2017. Retrieved 4 September 2017.
- Grimm, Simon L.; Demory, Brice-Olivier; Gillon, Michaël; et al. (21 January 2018). "The nature of the TRAPPIST-1 exoplanets". Astronomy & Astrophysics. 613: A68. arXiv: . Bibcode:2018A&A...613A..68G. doi:10.1051/0004-6361/201732233.
- de Wit, Julien; Wakeford, Hannah R.; Lewis, Nikole K.; et al. (March 2018). "Atmospheric reconnaissance of the habitable-zone Earth-sized planets orbiting TRAPPIST-1". Nature Astronomy. 2 (3): 214–219. arXiv: . Bibcode:2018NatAs...2..214D. doi:10.1038/s41550-017-0374-z.
- 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: . Bibcode:2017ApJ...842L...5Q. doi:10.3847/2041-8213/aa74bf.
- "Planet TRAPPIST-h". Exoplanet.eu. Retrieved 24 April 2018.
- "Hubble delivers first hints of possible water content of TRAPPIST-1 planets". www.spacetelescope.org. Retrieved 1 September 2017.
- Ormel, Chris; Liu, Beibei; Schoonenberg, Djoeke (20 March 2017). "Formation of TRAPPIST-1 and other compact systems". Astronomy & Astrophysics. 604: A1. arXiv: [astro-ph.EP]. Bibcode:2017A&A...604A...1O. doi:10.1051/0004-6361/201730826.
- https://arxiv.org/abs/1712.05641 Interior Structures and Tidal Heating in the TRAPPIST-1 Planets
- Wheatley, Peter J.; Louden, Tom; Bourrier, Vincent; Ehrenreich, David; Gillon, Michaël (February 2017). "Strong XUV irradiation of the Earth-sized exoplanets orbiting the ultracool dwarf TRAPPIST-1". Monthly Notices of the Royal Astronomical Society: Letters. 465 (1): L74–L78. arXiv: . Bibcode:2017MNRAS.465L..74W. doi:10.1093/mnrasl/slw192.
- O'Malley-James, J. T.; Kaltenegger, L. (28 March 2017). "UV Surface Habitability of the TRAPPIST-1 System". Monthly Notices of the Royal Astronomical Society: Letters. 469: L26–L30. arXiv: [astro-ph.EP]. Bibcode:2017MNRAS.469L..26O. doi:10.1093/mnrasl/slx047.
- Kaplan, Sarah (22 February 2017). "Here's what you should know about the newfound TRAPPIST-1 solar system". The Washington Post.
- Gleiser, M. (23 February 2017). "Trappist-1 Planet Discovery Ignites Enthusiasm in Search For Alien Life". NPR. Retrieved 25 February 2017.
- de Wit, Julien; Wakeford, Hannah R.; Gillon, Michaël; et al. (1 September 2016). "A combined transmission spectrum of the Earth-sized exoplanets TRAPPIST-1 b and c". Nature. 537 (7618): 69–72. arXiv: . Bibcode:2016Natur.537...69D. doi:10.1038/nature18641. PMID 27437572.
- Bourrier, V.; Ehrenreich, D.; Wheatley, P. J.; et al. (February 2017). "Reconnaissance of the TRAPPIST-1 exoplanet system in the Lyman-α line". Astronomy & Astrophysics. 599: L3. arXiv: . Bibcode:2017A&A...599L...3B. doi:10.1051/0004-6361/201630238. More than one of
- Swain, M. (2008). "Probing the Atmospheres of Exoplanets" (PDF). Hubble 2008: Science Year in Review. NASA. Retrieved 25 February 2017.
- Osgood, M. (22 February 2017). "Sagan Institute director explains what life could be like near Trappist-1". Cornell University. Retrieved 25 February 2017.
- Barstow, J. K.; Irwin, P. G. J. (September 2016). "Habitable worlds with JWST: Transit spectroscopy of the TRAPPIST-1 system?". Monthly Notices of the Royal Astronomical Society: Letters. 461 (1): L92–L96. arXiv: . Bibcode:2016MNRAS.461L..92B. doi:10.1093/mnrasl/slw109.
- Lingam, Manasvi; Loeb, Abraham (15 March 2017). "Enhanced interplanetary panspermia in the TRAPPIST-1 system". Proceedings of the National Academy of Sciences: 201703517. arXiv: [astro-ph.EP]. Bibcode:2017PNAS..114.6689L. doi:10.1073/pnas.1703517114.
- Boss, Alan; Weinberger, Alycia; Keiser, Sandra; Astraatmadja, Tri; Anglada-Escude, Guillem; Thompson, Ian (2017). "Astrometric Constraints on the Masses of Long-Period Gas Giant Planets in the TRAPPIST-1 Planetary System". The Astronomical Journal. 154 (3): 1–16. arXiv: . Bibcode:2017AJ....154..103B. doi:10.3847/1538-3881/aa84b5.
- Howell, Elizabeth (5 May 2017). "TRAPPIST-1 Planets Have No Large Moons, Raising Questions about Habitability". Seeker. Retrieved 17 June 2017.
- Kane, Stephen R. (April 2017). "Worlds without Moons: Exomoon Constraints for Compact Planetary Systems". The Astrophysical Journal Letters. 839 (2): L19. arXiv: . Bibcode:2017ApJ...839L..19K. doi:10.3847/2041-8213/aa6bf2. More than one of
- "Artist's view of planets transiting red dwarf star in TRAPPIST-1 system". SpaceTelescope.org. 20 July 2016. Retrieved 21 July 2016.
- Levenson, Thomas (2 May 2016). "Astronomers Have Found Planets in the Habitable Zone of a Nearby Star". The Atlantic. Retrieved 31 July 2016.
|Wikimedia Commons has media related to TRAPPIST-1.|
- TRAPPIST.one, the discovery team's official website
- on YouTube by NASA
- on YouTube by NASA's Jet Propulsion Laboratory
- ESOcast 83: "Ultracool Dwarf with Planets" by the European Southern Observatory