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| Kepler-36 | |
|---|---|
| Name | Kepler-36 |
| Constellation | Cygnus |
| Epoch | J2000 |
| Type | Planetary system |
Kepler-36 is a planetary system discovered by the Kepler Space Telescope mission located in the constellation Cygnus. The system attracted attention because two transiting planets exhibit unusually close orbital spacing and strong gravitational interactions revealed through transit timing variations measured by NASA teams and collaborative analyses involving institutions such as the Harvard–Smithsonian Center for Astrophysics and the SETI Institute. Observations combined photometry from Kepler with radial velocity follow-up from ground-based facilities including the W. M. Keck Observatory and the McDonald Observatory.
The system was first flagged in the Kepler Input Catalog during the primary mission of the Kepler Space Telescope and announced in peer-reviewed work led by researchers affiliated with NASA Ames Research Center, University of California, Berkeley, and Yale University. Follow-up spectroscopy used instruments on telescopes such as Keck I, the Nordic Optical Telescope, and the Hobby–Eberly Telescope to constrain stellar parameters and confirm planetary masses, complemented by high-resolution imaging from adaptive optics systems at Palomar Observatory and the Gemini Observatory. The definitive analysis combined light curves, transit timing variations, and radial velocities published in journals tied to the American Astronomical Society and peer-reviewed by editorial boards like those of Nature and The Astrophysical Journal.
The host star is a subgiant-type star catalogued with identifiers in the Kepler Input Catalog and studied by spectroscopic surveys including the LAMOST and APOGEE programs. Spectral classification relied on standards from the Henry Draper Catalogue and techniques developed at the European Southern Observatory and Max Planck Institute for Astronomy. Fundamental parameters such as effective temperature, metallicity, and surface gravity were derived using model atmospheres like those from the Kurucz grids and compared against stellar evolutionary tracks from the Yonsei–Yale and MESA models. Asteroseismic constraints, where applied, referenced methods used by missions including CoRoT and TESS to refine age and radius estimates consistent with benchmarks from the Hipparcos and Gaia astrometric catalogs.
The system hosts two confirmed transiting planets designated in discovery papers and characterized through combined analysis by teams from MIT, Princeton University, and the University of Chicago. Planetary radii and masses were determined using transit photometry from Kepler and radial velocity measurements from Keck Observatory; model comparisons used interior structure frameworks informed by studies from Jonathan Fortney's group and equations of state employed in work at the Lawrence Livermore National Laboratory. The inner planet's properties were contrasted with populations catalogued by the Exoplanet Archive and statistical studies like those by the California Planet Survey and HARPS consortium.
Kepler-36's planets display large-amplitude transit timing variations arising from strong mutual gravitational perturbations, a phenomenon analyzed using n-body integrators referenced in computational work at the Jet Propulsion Laboratory and numerical codes developed at Princeton University and Caltech. The system lies near a first-order mean-motion resonance, invoking theories from classical celestial mechanics formulated by researchers influenced by the Laplace and Lagrange formulations and modern resonant dynamics explored by groups at Cornell University and University of Cambridge. Dynamical stability studies used techniques from the N-body problem literature and chaos indicators such as the Lyapunov exponent applied in analyses akin to those conducted for systems like HD 45364 and GJ 876.
Formation scenarios invoked convergent migration within a protoplanetary disk, referencing hydrodynamic simulations developed at institutions like Princeton University and Uppsala University and planet formation theories advanced by researchers at University of Geneva and ETH Zurich. Models considered disk-driven migration, planetesimal accretion frameworks from the MMSN paradigm, and in situ assembly hypotheses informed by studies at the Institute for Advanced Study and the Max Planck Institute for Astronomy. Evolutionary trajectories integrated tidal interaction treatments derived from work at University of Cambridge and thermal evolution codes similar to those used by teams at Northwestern University to account for mass loss, envelope erosion, and potential Roche lobe effects analogous to processes invoked for systems such as Kepler-11 and 55 Cancri.
While neither planet occupies the classical habitable zone defined in studies by Kasting and collaborators, atmospheric characterization attempts referenced transmission spectroscopy methods pioneered with facilities like the Hubble Space Telescope and instruments on the Very Large Telescope. Atmospheric escape and composition models relied on ultraviolet irradiation studies from GALEX and X-ray flux assessments from Chandra X-ray Observatory and XMM-Newton to evaluate photoevaporation outcomes explored by researchers at University of California, Santa Cruz and Columbia University. Comparative exoplanetology placed Kepler-36 in context with atmospheric observations of GJ 1214 b and HD 209458 b to assess prospects for detecting signatures with next-generation observatories such as the James Webb Space Telescope and proposed missions within the European Space Agency programs.
Category:Exoplanetary systems