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| HD 10180 | |
|---|---|
| Name | HD 10180 |
| Constellation | Hydra (constellation) |
| Epoch | J2000 |
| Apparent magnitude | 7.33 |
| Spectral type | G1V |
| Distance | 127 light-years |
| Mass | 1.06 M☉ |
| Radius | 1.20 R☉ |
| Luminosity | 1.5 L☉ |
| Metallicity | +0.08 [Fe/H] |
| Age | 4.3 Gyr |
HD 10180 is a Sun-like G-type main-sequence star located in the constellation Hydra (constellation), notable for hosting a complex multiplanet system that has attracted attention from the European Southern Observatory community and exoplanet researchers. The system has been the subject of radial velocity campaigns using facilities such as the High Accuracy Radial velocity Planet Searcher and the Anglo-Australian Telescope, and it figures prominently in comparative studies with systems like Kepler-11 and TRAPPIST-1. Astronomers have compared its architecture to the Solar System and alternative compact systems such as 55 Cancri and Upsilon Andromedae.
HD 10180 sits roughly 127 light-years from the Solar System toward Hydra (constellation). It was cataloged in surveys including the Henry Draper Catalogue and subsequently observed by programs affiliated with the European Southern Observatory, the Anglo-Australian Observatory, and the La Silla Observatory. The system's reported multiplicity led to numerous publications in journals like Astronomy & Astrophysics, The Astrophysical Journal, and Monthly Notices of the Royal Astronomical Society. Comparative exoplanetology studies link its configuration to systems found by the Kepler (spacecraft), HARPS, and follow-up efforts using the Very Large Telescope and Keck Observatory.
The host is classified as a G1V star, with parameters derived through spectroscopic analysis performed with instruments such as HARPS and modeled using stellar evolution codes referencing the Padova Observatory tracks. Stellar properties—mass, radius, luminosity, metallicity, and age—were estimated via comparisons to standards like Alpha Centauri A, Tau Ceti, and HD 40307. Metallicity measurements placed it near solar values, comparable to hosts including HD 69830 and 51 Pegasi. Activity indicators were evaluated against datasets from the Mount Wilson Observatory and X-ray observations from ROSAT and XMM-Newton to assess chromospheric activity and rotational period.
The planetary system around the star was inferred from high-precision radial velocity signals obtained with HARPS and instruments on the Anglo-Australian Telescope. Initial models proposed up to seven or nine planets, provoking comparisons with multi-planet systems such as Kepler-20, HD 219134, and Gliese 581. Reported planets span super-Earth to Neptune masses, with orbital periods analogous to those in systems like GJ 876 and HD 69830. Planets were assigned minimum masses (m sin i) and semi-major axes via Keplerian fits using methods akin to those applied for 51 Pegasi b and 55 Cancri e. Subsequent analyses invoked Bayesian model selection techniques employed in studies of Tau Boo and HD 45364 to refine the number and parameters of companions.
Discovery arose from long-term radial velocity monitoring programs that included teams behind HARPS, the Anglo-Australian Planet Search, and collaborative efforts involving the European Southern Observatory and the Geneva Observatory. Data reduction and analysis used pipelines informed by methodologies from projects like California Planet Survey and Lick Observatory programs. Results were published and debated in venues such as Astronomy & Astrophysics, with follow-up analyses by groups affiliated with institutions like the University of Geneva, the University of California, and the Australian National University. Observational strategies mirrored those used to confirm systems around hosts like HD 40307 and 55 Cancri.
Dynamical analyses applied N-body integrations and stability criteria developed in works on resonant chains such as GJ 876 and Kepler-36, using tools comparable to the Mercury (N-body) integrator and symplectic integrators cited in studies of Upsilon Andromedae. Researchers examined orbital resonances, secular interactions, and chaotic diffusion drawing on frameworks used for Laplace resonance investigations in the Galilean moons and exoplanet resonance studies in HD 45364. Stability timescales were compared with simulations conducted for the Solar System and compact systems like Kepler-11, informing the debate on long-term survivability and migration mechanisms proposed in theories by groups including those at the Max Planck Institute for Astronomy and Princeton University.
Assessments of potential habitability invoked definitions and criteria used in studies of the circumstellar habitable zone around stars such as Kepler-62 and Proxima Centauri. The system's orbital architecture and stellar luminosity were compared to habitable zones defined in work by researchers at NASA Ames Research Center and University of Washington. Discussions referenced atmospheric retention models developed for Gliese 667 Cc and Kepler-186f, and tidal evolution models from literature concerning TRAPPIST-1 and GJ 667C. Given reported planet masses and orbital distances, prospects for Earth-like conditions were evaluated alongside considerations of stellar activity measured in X-rays by XMM-Newton and chromospheric indices from the Mount Wilson Observatory.
The system has become a case study in exoplanet detection methodology debates and in teaching materials at institutions including University of Cambridge, University of Oxford, and MIT. It features in public outreach by organizations such as NASA and the European Southern Observatory, and in media coverage alongside discoveries like 51 Pegasi b and Kepler-22b. Scientifically, the system informed theoretical work on planet formation and migration by researchers at centers including the Institute for Advanced Study, the Max Planck Institute for Astronomy, and the Carnegie Institution for Science. The multiplicity claims spurred methodological advances in radial velocity analysis used by collaborative networks like the Exoplanet Exploration Program and influenced proposals for future facilities such as the Extremely Large Telescope and missions planned by the European Space Agency.
Category:Stars Category:Exoplanet host stars