Kepler-186 — LLMpedia

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Kepler-186. Kepler-186 is a main-sequence M-dwarf star in the constellation Cygnus known for hosting a compact multiplanet system including a small transiting world in the conservative habitable zone. The system's identification emerged from photometric surveys and transit validation analyses tied to missions and institutions such as Kepler, the Ames Research Center, and the SETI Institute. Studies of the star and planets have involved observatories and projects including Hubble Space Telescope, Spitzer Space Telescope, European Southern Observatory, and researchers associated with Harvard–Smithsonian Center for Astrophysics, Caltech, and the University of California, Berkeley.

Discovery and Observation

The detection was made using transit photometry by Kepler during its primary mission, with light curve analyses employing teams from NASA, Jet Propulsion Laboratory, and the Kepler Science Office. Follow-up observations and validation involved spectroscopic and adaptive optics programs at facilities such as Keck Observatory, Palomar Observatory, Gemini Observatory, Subaru Telescope, and the Very Large Telescope. The candidate list and catalogs produced by initiatives like the Exoplanet Archive and the NASA Exoplanet Science Institute contributed to peer-reviewed confirmation in papers authored by teams at SETI Institute, University of Washington, Pennsylvania State University, and the Max Planck Institute for Astronomy. Statistical validation techniques built on frameworks from groups associated with Harvard University, MIT, University of Cambridge, and University of Chicago.

The host is classified as an M-dwarf (spectral class M1V) with parameters measured and modeled by stellar astrophysicists at institutions like University of California, Santa Cruz and University of Arizona. Effective temperature determinations referenced models from groups at Kavli Institute for Theoretical Physics and data reduction pipelines from Space Telescope Science Institute. Mass and radius estimates used stellar evolution codes developed by collaborators at Institut d'Astrophysique de Paris, University of Geneva, and the Max Planck Institute for Astrophysics. Metallicity and activity indicators were compared with samples from surveys led by European Southern Observatory and the Sloan Digital Sky Survey. Photometric variability and flare assessments referenced comparative studies from Mount Wilson Observatory and long-term monitoring projects at Lick Observatory.

The compact system contains multiple small planets discovered via transit signals cataloged by the Kepler Input Catalog and analyzed using transit timing and validation methods common to teams at Princeton University, Columbia University, and University of Oxford. Dynamics and orbital architectures were modeled by researchers affiliated with NASA Ames Research Center, Cornell University, and Northwestern University using N-body codes from groups at Caltech and Institute for Advanced Study. Comparative exoplanetology placed the system alongside noted systems like TRAPPIST-1, Kepler-186f's contemporaries in the literature compared to catalogs maintained by European Space Agency and the Exoplanet Archive. Planet radius estimates relied on stellar parameters from earlier sections and transit depth analyses by teams at University of Hawaii, University of Colorado Boulder, and Monash University.

The outermost transiting planet, designated in discovery papers and simulated by climate modelers from NASA Goddard Space Flight Center, resides in the conservative habitable zone as defined in frameworks by James F. Kasting and groups at Pennsylvania State University. Habitability assessments referenced radiative-convective models from University of Exeter, global circulation models adapted from work at NCAR, and photochemical models from University of California, Los Angeles. The planet's radius places it near thresholds discussed in publications from Harvard University and University of Toronto regarding the rocky-to-gaseous transition. Studies invoking tidal locking, stellar flux, and magnetic interaction cited collaborations with researchers at University of Michigan, MIT, and Princeton Plasma Physics Laboratory.

Formation scenarios drew on protoplanetary disk theory developed by teams at Max Planck Institute for Astronomy, University of Cambridge, and University of California, Santa Cruz, and on accretion models from Caltech and ETH Zurich. Migration hypotheses referenced torque formulations from groups at Dublin Institute for Advanced Studies and resonant interaction studies from University of Bonn. N-body simulations assessing long-term stability were performed by researchers at University of Amsterdam, Universität Heidelberg, and University of Toulouse, while pebble accretion and planetesimal-driven migration frameworks incorporated results from MPIA and University of Leeds. Comparative formation work drew parallels with systems studied by teams at Observatoire de Paris, Stockholm University, and Australian National University.

Atmospheric escape, greenhouse limits, and possible compositions were modeled using tools developed at NASA Ames Research Center, University of Chicago, and University of Colorado Boulder. Observational strategies to characterize atmospheres invoked facilities such as the James Webb Space Telescope, Hubble Space Telescope, and ground-based spectrographs at European Southern Observatory and Keck Observatory. Photochemical modeling engaged researchers at University College London, University of Washington, and Imperial College London, while biosignature and false-positive frameworks cited projects at SETI Institute, NASA Astrobiology Institute, and USGS collaborators. Future prospects discussed in the literature involved mission concepts from European Space Agency, NASA, and proposals considered by teams at Blue Origin, SpaceX, and academic consortia including Harvard & Smithsonian.

Category:Exoplanet host stars