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TRAPPIST-1

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Plot of the radii of known rocky planets as a function of their equilibrium temperature calculated assuming zero albedo. Planets discussed in this article are color-coded by their stellar temperature. Planets circled in black have atmospheric observations planned by the James Webb Space Telescope (JWST) Guaranteed Time Observation program (Information in the Guest observer program is available here: https://www.stsci.edu/jwst/science-execution/approved-programs/cycle-1-go). Planets in the TRAPPIST-1 system are labelled b to h.
Published: 01 August 2021
Space Telescope ( JWST ) Guaranteed Time Observation program (Information in the Guest observer program is available here: https://www.stsci.edu/jwst/science-execution/approved-programs/cycle-1-go ). Planets in the TRAPPIST-1 system are labelled b to h.
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Contour lines representing the combined maximum allowable present day outgassing rates of CO2 and H2O, relative to the Earth’s present day outgassing rates, for LHS 3844 b, Trappist-1 b, and Trap-pist-1 c. Estimates based on mass loss rates from solar wind stripping only (A), and from energy-limited escape (B) are shown. Upper bounds on the maximum allowable outgassing rates are calculated using the upper limits on mass loss rates and lower limits on Earth’s present-day CO2 and H2O outgassing rates, while lower bounds use the lower limits on mass loss rates and upper limits on Earth’s outgassing rates.
Published: 01 July 2024
Figure 5. Contour lines representing the combined maximum allowable present day outgassing rates of CO 2 and H 2 O, relative to the Earth’s present day outgassing rates, for LHS 3844 b, Trappist-1 b, and Trap-pist-1 c. Estimates based on mass loss rates from solar wind stripping only
Journal Article
Published: 01 July 2024
Reviews in Mineralogy and Geochemistry (2024) 90 (1): 559–594.
...Figure 5. Contour lines representing the combined maximum allowable present day outgassing rates of CO 2 and H 2 O, relative to the Earth’s present day outgassing rates, for LHS 3844 b, Trappist-1 b, and Trap-pist-1 c. Estimates based on mass loss rates from solar wind stripping only...
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Diagram showing the habitable zone around different stars in which liquid water may be present on a planet's surface. The x-axis is the amount of starlight hitting the planet compared to that hitting present Earth; the y-axis is stellar surface temperature. Venus, Earth, and Mars are shown, along with various exoplanets identified from NASA's Kepler Space Telescope and various ground-based transit and radial velocity surveys. Only exoplanets with radii <1.6 REarth are shown. Proxima Centauri b orbits a red dwarf that is only 4 light years distant. The TRAPPIST-1 system (bottom of figure) is about 40 light years away.
Published: 01 August 2019
are shown, along with various exoplanets identified from NASA's Kepler Space Telescope and various ground-based transit and radial velocity surveys. Only exoplanets with radii <1.6 R Earth are shown. Proxima Centauri b orbits a red dwarf that is only 4 light years distant. The TRAPPIST-1 system
Journal Article
Journal: Elements
Published: 01 August 2021
Elements (2021) 17 (4): 257–263.
... Space Telescope ( JWST ) Guaranteed Time Observation program (Information in the Guest observer program is available here: https://www.stsci.edu/jwst/science-execution/approved-programs/cycle-1-go ). Planets in the TRAPPIST-1 system are labelled b to h. ...
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Journal Article
Journal: Elements
Published: 01 June 2022
Elements (2022) 18 (3): 181–186.
.... Some of the best characterized super-Earth systems may have planets holding water, although estimates come with very large error bars (e.g., Raymond et al. 2022 ). The TRAPPIST-1 is one of these iconic systems in which adjacent planets show rhythmic orbital motions and form a so-called “resonant chain...
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Examples of statistical comparative planetology approaches (Bean et al. 2017) to constrain planet formation and evolution processes via ensemble observations of exoplanet atmospheres. Left: Atmospheric metallicity vs. mass for solar system planets (black symbols) and for exoplanets that have detections of carbon- and/or oxygen-bearing species using JWST (red symbols). Overlaid are the predictions from population synthesis models from Fortney et al. (2013) showing a rise and then a plateau in metallicity as planetary mass decreases (gray dots). The solar system giant planets are observed to follow a very tight mass–metallicity correlation (dashed line), with the caveat that oxygen is undetected in the atmospheres of these planets, as it is sequestered in condensates below the photosphere. Figure adapted from Mansfield et al. (2018). Right: The “cosmic shoreline” (Zahnle and Catling 2017) is denoted (yellow diagonal band), which is an observed delineation in escape speed and insolation between solar system bodies that do and do not possess gaseous atmospheres (toward the upper left and toward the lower right of the plot, respectively). Transiting exoplanets that will be observed in Cycles 1 and 2 of JWST are over-plotted in this same parameter space. Symbol size denotes the expected S/N of a single transit or eclipse observation using the methods of Kempton et al. (2018). The letters b–h denote the planets in the TRAPPIST-1 system, which are all slated for JWST observations, and the terrestrial solar system planets are shown for reference. By identifying which terrestrial exoplanets possess atmospheres and whether they are bounded by the same “shoreline” as for the solar system, astronomers can constrain the processes by which planets lose or retain their atmospheres. Figure courtesy of Jegug Ih.
Published: 01 July 2024
that will be observed in Cycles 1 and 2 of JWST are over-plotted in this same parameter space. Symbol size denotes the expected S/N of a single transit or eclipse observation using the methods of Kempton et al. (2018) . The letters b–h denote the planets in the TRAPPIST-1 system, which are all slated for JWST
Journal Article
Journal: Elements
Published: 01 August 2021
Elements (2021) 17 (4): 251–256.
... as the spectrum and long-term evolution of their host stars. Many potentially habitable planets exist in planetary systems that are near an orbital resonance, for instance those in the TRAPPIST-1 system. This architecture indicates that the planets in the system formed further from the host star, where...
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Journal Article
Journal: Elements
Published: 01 December 2022
Elements (2022) 18 (6): 368–373.
... is to invoke inward movement of the snow line in the final growth phases of the satellites. A formation scenario for the extrasolar TRAPPIST-1 system that has various ice mass fractions of planets may also apply to the Galilean satellites ( Madeira et al. 2021 ). Thus, studies of the Galilean satellites...
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Journal Article
Published: 01 July 2024
Reviews in Mineralogy and Geochemistry (2024) 90 (1): 411–464.
... that will be observed in Cycles 1 and 2 of JWST are over-plotted in this same parameter space. Symbol size denotes the expected S/N of a single transit or eclipse observation using the methods of Kempton et al. (2018) . The letters b–h denote the planets in the TRAPPIST-1 system, which are all slated for JWST...
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Journal Article
Published: 01 June 2019
American Mineralogist (2019) 104 (6): 817–829.
... bulk densities of rocky exoplanets. For example, there has been much interest in the TRAPPIST-1 system because there, seven rocky, more-or-less Earth-sized, exoplanets have been discovered ( Gillon et al. 2017 ). Several studies have thus ensued, attempting to narrow their bulk densities (see Quarles...
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Journal Article
Published: 01 July 2024
Reviews in Mineralogy and Geochemistry (2024) 90 (1): 465–514.
... of O 2 or O 3 —it is nonetheless a key target in the search for life beyond Earth. Indeed, the CO 2 –CH 4 biosignature couple may be the most observable potential biosignature in the TRAPPIST-1 planetary system ( Krissansen-Totton et al. 2018a ; Mikal-Evans 2021 ; Meadows et al. 2023 ). N 2...
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The cosmic shoreline proposed by Zahnle and Catling (2017) in terms of present-day stellar flux (A), I∝vesc4, and integrated XUV flux (B), IXUV∝vesc4, with regions where planets should be airless and should retain their atmospheres labelled. The four planets interpreted to be airless based on thermal emission are plotted. Depending on the chosen formulation for the cosmic shoreline, the two Trappist planets may fall into either the regime where they would be predicted to still retain atmospheres or to be airless.
Published: 01 July 2024
Figure 1. The cosmic shoreline proposed by Zahnle and Catling (2017) in terms of present-day stellar flux (A) , I ∝ v esc 4 , and integrated XUV flux (B) , I XUV ∝ v esc 4 , with regions where planets should be airless and should retain
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Spectra of Earth-like planets showing N2O features as a function of N2O production rate. The top set of four panels shows the IR emission spectra of Earth-like planets with 21% O2, 50% cloud cover, and net N2O fluxes of 1, 10, and 100 Tmol/yr. The bottom two panels show a hypothetical transmission spectrum of TRAPPIST-1e under the same assumptions. Major absorbing species are indicated. Each scenario’s abundance is determined from the photochemical simulations shown in Figure 9. These figures were adapted from Schwieterman et al. (2022) under Creative Commons Attribution License CC-BY 4.0.
Published: 01 July 2024
Figure 10. Spectra of Earth-like planets showing N 2 O features as a function of N 2 O production rate. The top set of four panels shows the IR emission spectra of Earth-like planets with 21% O 2 , 50% cloud cover, and net N 2 O fluxes of 1, 10, and 100 Tmol/yr. The bottom two panels show
Journal Article
Published: 01 April 2025
Geochemical Perspectives (2025) 14 (1): 81–108.
... years. Third, the exoplanets shown in Figure 5.7 are all thought to be less than 1.6 Earth radii, and hence rocky. Most were discovered from the ground using the radial velocity method or from space by way of transits. The TRAPPIST-1 system at the bottom of the diagram consists of seven coplanar...
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Journal Article
Published: 01 April 2025
Geochemical Perspectives (2025) 14 (1): 102–137.
... operating James Webb Space Telescope, JWST for short, cannot do this except when the planet is bright in the infrared – meaning that it is hot – and is well separated from the star. JWST can, and will, obtain spectra from cooler exoplanet atmospheres, but only for planets like those in the TRAPPIST-1 system...
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Journal Article
Journal: Elements
Published: 01 August 2021
Elements (2021) 17 (4): 235–240.
... CT , Desch SJ , Hinkel NR , Lorenzo A ( 2018 ) Inward migration of the TRAPPIST-1 planets as inferred from their water-rich compositions . Nature Astronomy 2 : 297 - 302 , doi: 10.1038/s41550-018-0411-6 Weller MB , Lenardic A ( 2018 ) On the evolution...
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Journal Article
Published: 01 July 2024
Reviews in Mineralogy and Geochemistry (2024) 90 (1): 323–373.
... , Leconte J , Lederer SM , Luger R , Malhotra R , Meadows VS , Morris BM , Pozuelos FJ , Queloz D , Raymond SN , Selsis F , Sestovic M , Triaud AHMJ , Grootel VV ( 2021 ) Refining the transit-timing and photometric analysis of TRAPPIST-1...
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Journal Article
Published: 01 July 2024
Reviews in Mineralogy and Geochemistry (2024) 90 (1): 301–322.
... of Jupiter, where volcanism occurs absent large-scale mantle convection. Heat pipes might be restricted to planets with tidal heating and so would be a factor in exoplanets that are in close orbit to their stars ( Jackson et al. 2008 ). An example would be the Trappist-1 system ( Barr et al. 2018 ). In any...
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Journal Article
Journal: Elements
Published: 01 August 2019
Elements (2019) 15 (4): 235–240.
... are shown, along with various exoplanets identified from NASA's Kepler Space Telescope and various ground-based transit and radial velocity surveys. Only exoplanets with radii <1.6 R Earth are shown. Proxima Centauri b orbits a red dwarf that is only 4 light years distant. The TRAPPIST-1 system...
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