Radius, mass, and temperatureTRAPPIST-1d was detected with the transit method, allowing scientists to accurately determine its radius. The planet is about 0.784 REarth with a small error margin of about 147 km. Transit timing variations and complex computer simulations helped accurately determine the mass of the planet, which led to scientists being able to calculate its density, surface gravity, and composition. TRAPPIST-1d is a mere 0.297 MEarth, making it one of the least massive exoplanets yet found. It has 61.6% the density of Earth (3.39 g/cm3) and just under half the gravity. Both its mass, density, and surface gravity are the lowest in the entire TRAPPIST-1 system. In addition, the density of TRAPPIST-1d indicates a mainly rocky composition, with about ≤5% of its mass in the form of a volatile layer. The volatile layer of TRAPPIST-1d may consist of atmosphere, ocean, and/or ice layers. TRAPPIST-1d has an equilibrium temperature of 282.1 K (9.0 °C; 48.1 °F), assuming an albedo of 0. For an Earth-like albedo of 0.3, the planet's equilibrium temperature is around 258 K (−15 °C; 5 °F), very similar to Earth's at 255 K (−18 °C; −1 °F).
OrbitTRAPPIST-1d is a closely orbiting planet, with one full orbit taking just 4.05 days (about 97 hours) to complete. It orbits at a distance of just 0.02228 AU from the host star, or about 2.2% the distance between Earth and the Sun. For comparison, Mercury, our Solar System's innermost planet, takes 88 days to orbit at a distance of about 0.38 AU. The size of TRAPPIST-1 and the close orbit of TRAPPIST-1d around it means that the star as seen from the planet appears 5.5 times as large as the Sun from the Earth. While a planet at TRAPPIST-1d's distance from our Sun would be a scorched world, the low luminosity of TRAPPIST-1 means that the planet gets only 1.043 times the sunlight that Earth receives, placing it within the inner part of the conservative habitable zone.
Host starThe planet orbits an (M-type) ultracool dwarf star named TRAPPIST-1. The star has a mass of 0.089 M☉ (close to the boundary between brown dwarfs and hydrogen-fusing stars) and a radius of 0.121 R☉. It has a temperature of 2,516 K (2,243 °C; 4,069 °F), and is between 3 and 8 billion years old. In comparison, the Sun is 4.6 billion years old and has a temperature of 5778 K (5504.85 °C, 9940.73 °F). 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 metals than the Sun. Its luminosity (L☉) is 0.05% of that of the Sun. Stars like TRAPPIST-1 have the ability to live up to 4–5 trillion years, 400–500 times longer than the Sun will live (the Sun only has about 8 billion years of lifespan left, slightly more than half of its lifetime). 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 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 (the limit for that is 6.5). The star is not just very small and far away, it also emits comparatively little visible light, mainly shining in the invisible infrared. Even from the close in proximity of TRAPPIST-1d, about 50 times closer than Earth is from the Sun, the planet receives less than 1% the visible light Earth sees from our Sun. This would probably make the days on TRAPPIST-1d never brighter than twilight is on Earth. However, that still means that TRAPPIST-1 could easily shine at least 3000 times brighter in the sky of TRAPPIST-1d than the full moon does in Earth's night sky.
HabitabilitySee also: Habitability of red dwarf systems Models and scientists are divided on whether their convergent solutions from the data for TRAPPIST-1d indicates Earth-like habitability or a severe greenhouse effect. In some respects, this exoplanet is one of the most Earth-like found. Much smaller than Earth which may impair on its magnetosphere, it superficially receives just more than our planet's radiation. It does not have a hydrogen or helium-based atmosphere, which makes largest planets uninhabitable. The planet may also have liquid and atmospheric water, up to many times more than Earth. Likely tidally locked, a dense atmosphere could be enough to transfer heat to the much colder dark side. Most models by the University of Washington for TRAPPIST-1d strongly converge on a Venus-like planet with an uninhabitable atmosphere, due to hydrogen being stripped out of the planet's atmosphere, drying it out, as happened on Venus. It is on the inside part of the expected habitable zone of its parent star (where, with quite narrow change from Earth's magnetosphere, bombardment history, star/planetary history and gases, liquid water would be on the surface), but because it has only 0.3 Earth mass, it may have no magnetic field like Venus and Mars, leaving it vulnerable to being dehydrated by the stellar wind, and is also likely to be very geologically active due to tidal squeezing as happens to Jupiter's moon Io. Advanced, three-dimensional modeling converges on a runaway greenhouse effect; some solutions have a little water surviving beyond the early hot phase in the planet's history. Barring an excessive level of seismic activity, however, if the planet has suffered a runaway greenhouse, its atmosphere should be thinner and cooler than Venus', due to its lower mass and the fact it only gets about as much sunlight as Earth (Venus gets about twice as much). TRAPPIST-1d may resist this heating, especially if it has an Earth-like albedo of ≥0.3, according to other analyses. The same researchers point out that such proximity to the host star tends to raise geothermal activity, and tidally heat the bottom of any seas.
DiscoveryA team of astronomers headed by Michaël Gillon of the Institut d’Astrophysique et Géophysique at the University of Liège in Belgium used the TRAPPIST (Transiting Planets and Planetesimals Small Telescope) telescope at the La Silla Observatory in the Atacama desert, Chile, to observe TRAPPIST-1 and search for orbiting planets. By utilising transit photometry, they discovered three Earth-sized planets orbiting the dwarf star; the innermost two are tidally locked to their host star while the outermost appears to lie either within the system's habitable zone or just outside of it. The team made their observations from September to December 2015 and published its findings in the May 2016 issue of the journal Nature. The original claim and presumed size of the planet was revised when the full seven-planet system was revealed in 2017: "We already knew that TRAPPIST-1, a small, faint star some 40 light years away, was special. In May 2016, a team led by Michaël Gillon at Belgium’s University of Liege announced it was closely orbited by three planets that are probably rocky: TRAPPIST-1b, c and d... "As the team kept watching shadow after shadow cross the star, three planets no longer seemed like enough to explain the pattern. “At some point we could not make sense of all these transits,” Gillon says. "Now, after using the space-based Spitzer telescope to stare at the system for almost three weeks straight, Gillon and his team have solved the problem: TRAPPIST-1 has four more planets. "The planets closest to the star, TRAPPIST-1b and c, are unchanged. But there’s a new third planet, which has taken the d moniker, and what had looked like d before turned out to be glimpses of e, f and g. There’s a planet h, too, drifting farthest away and only spotted once."
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