This article was accepted into the corpus but its outbound wikilinks were never NER-processed — typical at the deepest BFS hop or when the run's entity cap was reached. No expansion funnel to show.
| HD 219134 | |
|---|---|
| Name | HD 219134 |
| Epoch | J2000 |
| Constellation | Cassiopeia |
| Appmag v | 5.57 |
| Class | K3V |
| Mass | 0.78 |
| Radius | 0.778 |
| Metallicity | +0.11 |
| Names | HR 8832, HIP 114622, Gliese 892 |
HD 219134 is a nearby K-type main-sequence star located in the constellation Cassiopeia, notable for hosting a compact multi-planet system including several super-Earths and mini-Neptunes, which has attracted attention from astronomers and exoplanet missions. The star's proximity, brightness, and planetary architecture have made it a target for radial velocity programs, transit photometry, and atmospheric characterization studies involving major observatories and institutions. HD 219134's system provides comparative context for studies led by teams associated with instruments on facilities such as the European Southern Observatory, NASA, and the European Space Agency.
HD 219134 lies in the region of the sky mapped in surveys by the Hipparcos and Tycho missions and is cataloged in the Henry Draper and Gliese catalogs; it is frequently cross-referenced by research groups at the Harvard-Smithsonian Center for Astrophysics, the Max Planck Institute for Astronomy, and the Jet Propulsion Laboratory. The star's brightness has enabled follow-up by teams affiliated with the Keck Observatory, the HARPS consortium, and the Spitzer Science Center, while missions like TESS and CHEOPS have provided complementary photometric coverage used by researchers at the California Institute of Technology, the University of Geneva, and the University of Colorado. As a target of long-term monitoring by programs linked to the Carnegie Institution for Science, the system figures in comparative exoplanetology efforts supported by the National Science Foundation and the European Research Council.
The host star is classified as a K3V dwarf with parameters measured by spectroscopic campaigns at observatories such as the Anglo-Australian Telescope, the Subaru Telescope, and the Very Large Telescope, and characterized by teams at institutions including the University of Cambridge, Yale University, and Princeton University. Stellar mass and radius estimates draw on models from the Geneva stellar evolution group, isochrones developed at the University of Padua, and techniques refined by the Harvard College Observatory and the Space Telescope Science Institute; metallicity measurements link to abundance studies from the Max Planck Institute for Astrophysics and the Observatoire de Paris. HD 219134's age and rotation have been constrained using gyrochronology methods employed by researchers at the University of Arizona and the University of Bonn, while magnetic activity and chromospheric indices have been compared with data sets from Mount Wilson Observatory, the Lowell Observatory, and the National Solar Observatory.
The multi-planet system was revealed through coordinated efforts by radial velocity teams at Keck, HARPS-N, and the Automated Planet Finder, with transit detections confirmed by Spitzer and ground-based networks such as the Las Cumbres Observatory and the KELT survey; these detections were reported by collaborations including the Geneva Extrasolar Planet Search and the HARPS consortium. The architecture includes several short-period super-Earths and a longer-period Saturn-mass candidate that have been analyzed using dynamical simulations developed at institutions like MIT, Caltech, and the University of California, Berkeley, and integrated with population studies by groups at the University of Oxford and the University of Toronto. Mass and radius determinations from teams at the Massachusetts Institute of Technology, the University of Michigan, and the Australian National University support interior structure models influenced by research from the Carnegie Institution for Science, the Southwest Research Institute, and the Lunar and Planetary Institute.
Discovery and confirmation of the planets involved instruments and collaborations linked to the Keck Observatory, the European Southern Observatory, and the National Optical Astronomy Observatory, with radial velocity reduction pipelines developed by researchers at Carnegie Mellon University, the University of Geneva, and the Instituto de Astrofísica de Canarias. Transit follow-up observations were carried out by space missions and ground-based facilities such as Spitzer, TESS, CHEOPS, and the Las Cumbres network, while data analysis leveraged software and methodologies from the Space Telescope Science Institute, the Harvard-Smithsonian Center for Astrophysics, and the University of Sydney. The system has been included in target lists for future characterization by the James Webb Space Telescope, the Extremely Large Telescope, and the Thirty Meter Telescope, drawing interest from project teams at NASA, ESA, and national observatories.
Assessments of potential habitability and atmospheric composition have been pursued by research groups at institutions including the University of Chicago, the University of Exeter, and the University of California, Santa Cruz, employing transmission spectroscopy techniques used by teams working with Hubble, Spitzer, and upcoming James Webb programs. Comparative studies reference atmospheric escape models from the University of Colorado, photochemistry frameworks from UCLA, and climate models adapted by groups at the Massachusetts Institute of Technology and the Institut Pierre Simon Laplace; these efforts are coordinated with databases and analysis tools developed at the European Space Agency, the NASA Exoplanet Science Institute, and the Centre National d'Études Spatiales. While none of the confirmed planets lie squarely in classical habitable zone definitions used by the University of Arizona and the University of Washington, atmospheric characterization programs led by researchers at the University of Oxford and Leiden University continue to probe volatile inventories and surface conditions.
HD 219134 has been cited in reviews and surveys compiled by the Exoplanet Exploration Program at NASA, the ESA Science Programme, and the International Astronomical Union, and has been featured in outreach materials produced by institutions such as the American Astronomical Society, the Royal Astronomical Society, and the Planetary Society. The system serves as a benchmark in comparative exoplanetology discussed in conferences organized by the American Geophysical Union, the European Planetary Science Congress, and the International Astronomical Union's symposia, and figures in graduate curricula at universities including Stanford, Cambridge, and ETH Zurich. Its study has informed instrument design considerations at observatories such as the W. M. Keck Observatory, the European Southern Observatory, and the National Astronomical Observatory of Japan, influencing future programs at facilities supported by national science agencies and international consortia.
Category:K-type main-sequence stars Category:Exoplanet host stars