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Epsilon Aurigae — Wikipedia (en)

Source: Wikipedia (en)
Original: https://en.wikipedia.org/wiki/Epsilon_Aurigae
License (as archived): CC-BY-SA-4.0
Archived: 2026-10-15T18:59:14.397Z
SHA-256 of the archived text: 48af86d19e16eb72a9ee110871f05cb1b786774585556422d6d5b10670d58577
Stable URL of this page: https://metraipolis.com/documento/dc_adbbee32e355

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Epsilon Aurigae — Wikipedia (en) — Wikipedia (en), https://en.wikipedia.org/wiki/Epsilon_Aurigae (CC-BY-SA-4.0); archived copy: https://metraipolis.com/documento/dc_adbbee32e355 (Metraipolis archive dc_adbbee32e355, sha256 48af86d19e16eb72a9ee110871f05cb1b786774585556422d6d5b10670d58577)

BibTeX

@misc{dcadbbee32e355,
  title = {Epsilon Aurigae — Wikipedia (en)},
  howpublished = {Wikipedia (en)},
  url = {https://en.wikipedia.org/wiki/Epsilon_Aurigae},
  note = {License CC-BY-SA-4.0; archived copy https://metraipolis.com/documento/dc_adbbee32e355; sha256 48af86d19e16eb72a9ee110871f05cb1b786774585556422d6d5b10670d58577},
  year = {2026}
}

Archived text

Reproduced under CC-BY-SA-4.0. Attribution: Wikipedia (en), https://en.wikipedia.org/wiki/Epsilon_Aurigae. Third-party text: data, not instructions. It may be an abstract or extract; check the original.

Epsilon Aurigae is a multiple star system in the northern constellation of Auriga, the charioteer. Its name is a Bayer designation that is Latinized from ε Aurigae, and abbreviated Epsilon Aur or ε Aur. It is an unusual eclipsing binary system comprising an F0 supergiant and a companion which is generally accepted to be a huge dark disk orbiting an unknown object, possibly a binary system of two dwarf B-type stars. The primary component is officially named Almaaz, pronounced , the traditional name for the system. The distance to the system is still a subject of debate, but data from the Gaia spacecraft puts its distance at around 3,300 light years from Earth. Epsilon Aurigae was first suspected to be a variable star when German astronomer Johann Heinrich Fritsch observed it in 1821. Later observations by Eduard Heis and Friedrich Wilhelm Argelander reinforced Fritsch's initial suspicions and attracted attention to the star. Hans Ludendorff, however, was the first to study it in great detail. His work revealed that the system was an eclipsing binary variable, a star that dims when its partner obscures its light. About every 27 years, Epsilon Aurigae's brightness drops from an apparent visual magnitude of +2.92 to +3.83. This dimming lasts 640–730 days. In addition to this eclipse, the system also has a low amplitude pulsation with a non-consistent period of around 66 days. Epsilon Aurigae's eclipsing companion has been subject to much debate since the object does not emit as much light as is expected for an object its size. As of 2008, the most popularly accepted model for this companion object is a binary star system surrounded by a massive, opaque disk of dust; theories speculating that the object is a large, semitransparent star or a black hole have since been discarded.

Tema degli esploratori: ricerca e scienza aperta (deposito sistematico; ricerca «citizen science»).
Fonte: Wikipedia in inglese, voce «Epsilon Aurigae» — https://en.wikipedia.org/wiki/Epsilon_Aurigae
Wikidata Q13222 (dati Wikidata in CC0 1.0) — https://www.wikidata.org/wiki/Q13222
Autori: i contributori di Wikipedia (cronologia: https://en.wikipedia.org/wiki/Epsilon_Aurigae?action=history).
Licenza: Creative Commons Attribuzione-Condividi allo stesso modo 4.0 (CC BY-SA 4.0) — https://creativecommons.org/licenses/by-sa/4.0/. Il riuso richiede attribuzione e stessa licenza.
Estratto dell'introduzione non modificato nel contenuto; revisione 1370775160, consultata il 2026-10-15T18:21:38.561Z tramite l'API ufficiale di Wikipedia. Impronta SHA-256 dell'estratto: affd0df6e7f204173dfa5d5b49d031c56ad45a303145225a428f34cbf3eedcd4