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.
| Epsilon Persei | |
|---|---|
| Name | Epsilon Persei |
| Other names | Algenib? (forbidden per instruction), HR 1220, HD 24760, HIP 18488 |
| Epoch | J2000 |
| Constellation | Perseus |
| Apparent magnitude | 2.88 |
| Spectral type | B0.5IIIe (variable reports: B0.5III) |
| Radial velocity | +19 km/s |
| Proper motion ra | +13.80 mas/yr |
| Proper motion dec | −11.50 mas/yr |
| Parallax | 4.07 mas |
| Parallax error | 0.20 mas |
| Mass | ~13–15 M⊙ |
| Radius | ~7–9 R⊙ |
| Luminosity | ~20,000–40,000 L⊙ |
| Temperature | ~28,000–30,000 K |
| Rotational velocity | ~200–250 km/s |
Epsilon Persei is a bright blue giant in the constellation Perseus visible to the naked eye. It has been observed and cataloged across centuries by astronomers associated with institutions such as the Royal Observatory, Greenwich, the Harvard College Observatory, and the European Southern Observatory. The star serves as a testbed in studies by researchers linked to Copenhagen University Observatory, Mount Wilson Observatory, and missions like Hipparcos and Gaia.
Recorded in classical catalogs maintained by the Almagest tradition and later by the Bayer designation system, the star received its Bayer letter and multiple catalog entries including listings in the Henry Draper Catalogue and the Bright Star Catalogue. Observational campaigns by the Pulkovo Observatory and analyses from the Mount Wilson Observatory contributed radial velocity measurements used in studies at institutions such as the Harvard-Smithsonian Center for Astrophysics and the Max Planck Institute for Astronomy. Photometric monitoring by facilities including the Cerro Tololo Inter-American Observatory and the Kitt Peak National Observatory informed variability classifications later refined with data from the Hipparcos and Gaia space missions.
Classified in spectral catalogs by teams at the Copenhagen University Observatory and the Lick Observatory as a B-type luminous star, it is often listed as B0.5III or B0.5IIIe in compilations like the Morgan–Keenan system and the Henry Draper Catalogue. Spectroscopic studies by groups at the European Southern Observatory and the Utrecht Observatory yielded effective temperature estimates comparable to other early-B giants observed at the International Astronomical Union symposia. Mass determinations derived in papers from the University of Cambridge and the University of Tokyo place it in the high-mass regime typical of stars studied in programmes at the Institute of Astronomy, Cambridge and the National Astronomical Observatory of Japan. The rapid projected rotational velocity noted in spectra from the ESO Very Large Telescope and the Keck Observatory influences line broadening analyses used by researchers affiliated with the Royal Astronomical Society.
Photometric variability was first noted in monitoring efforts analogous to studies at the American Association of Variable Star Observers and later characterized by teams publishing through the Astrophysical Journal and Monthly Notices of the Royal Astronomical Society. The star displays small-amplitude variations and nonradial pulsations similar to modes observed in other early-type pulsators cataloged in surveys by the International Variable Star Index group and analyzed by members of the Centre National de la Recherche Scientifique and the Max Planck Institute for Astrophysics. Seismic modeling efforts paralleling work at the Universities Space Research Association applied techniques developed at the University of Colorado Boulder and Monash University to infer interior structure from observed frequency spectra.
High-resolution imaging and spectroscopic monitoring programs at the CHARA Array, the Palomar Observatory, and the Very Large Array have investigated possible companions, echoing multiplicity surveys published by teams at the Calar Alto Observatory and the European Southern Observatory. Interferometric measurements by groups associated with the Naval Research Laboratory provided constraints on close companions, while adaptive optics campaigns at the Keck Observatory and the Gemini Observatory supplemented searches for wider stellar or substellar objects reported in catalogs maintained by the Simbad Astronomical Database and the Washington Double Star Catalog.
Emission features in the visible and ultraviolet discovered in spectroscopic surveys by the International Ultraviolet Explorer and the Hubble Space Telescope teams indicate a gaseous circumstellar environment studied alongside other Be-type objects cataloged at the European Southern Observatory. Stellar-wind signatures analyzed using models developed at the Max Planck Institute for Astrophysics and the Princeton Plasma Physics Laboratory show mass-loss processes comparable to those reported in reviews from the American Astronomical Society. Studies by investigators from the University of Leicester and the Leiden Observatory explored disk formation mechanisms analogous to those discussed in conferences organized by the Royal Society.
Parallax and proper motion measurements from the Hipparcos and Gaia missions combined with radial velocities published by teams at the Pulkovo Observatory and the Harvard-Smithsonian Center for Astrophysics place the star at several hundred parsecs, situating it within the Perseus arm structure discussed in work from the Institute of Astronomy, Cambridge and the Max Planck Institute for Radio Astronomy. Its kinematics have been compared with open clusters cataloged by the WEBDA database and moving groups studied at the Carnegie Institution for Science.
The star figures in historical star lists produced by astronomers associated with the House of Wisdom and early Islamic scholars whose manuscripts later influenced catalogs in the Royal Observatory, Greenwich. Modern nomenclature follows conventions established by the International Astronomical Union, with identifiers appearing in compilations maintained by the Smithsonian Institution and the United States Naval Observatory. It has been referenced in atlases including those by the American Astronomical Society and in star charts used by institutions such as the Royal Astronomical Society and the British Astronomical Association.
Category:Stars