V1005 Orionis
is a young flare star in the equatorial constellation of Orion
V1005 Orionis is a young flare star in the equatorial constellation of Orion. It has the identifier GJ 182 in the Gliese–Jahreiß catalogue; V1005 Ori is its variable star designation. This star is too faint to be visible to the naked eye, having a mean apparent visual magnitude of 10.1. It is located at a distance of 79.6 light years from the Sun and is drifting further away with a radial velocity of 19.2 km/s. The star is a possible member of the IC 2391 supercluster.
Flare activity was first reported for this star by N. I. Shakhovskaya in 1974. B. W. Bopp found anomalously strong lithium lines in the spectrum of GJ 182, a rarity for stars of this class and a possible indicator of a very young star. Together with F. Espenak, in 1977 Bopp demonstrated the star showed periodic variations similar to BY Draconis. In 1984, Byrne and associates found a preliminary rotation period of 4.55 days and showed the star had a normal flare rate.
The stellar classification of V1005 Ori is M0Ve, indicating this is an M-type main-sequence star (a "red dwarf") with emission lines (e) in its spectrum.
The public source identifies “V1005 Orionis” as is a young flare star in the equatorial constellation of Orion. This brief keeps that definition visible, then builds a research path around V1005, Orionis and young.
Why this record matters
A short description can identify a subject without explaining its stakes. For “V1005 Orionis”, the useful work is to connect “is a young flare star in the equatorial constellation of Orion” to the records capable of establishing context and consequence.
Named sources, stable identifiers and responsible institutions provide the strongest route from overview to verifiable evidence. The source revision retrieved here is dated Jun 23, 2026. The linked authority identifier is Q85830815. None of the 0 selected statements returned an explicit reference. The first chronological checks are 1974, 1977 and 1984.
A concise general-reference account can conceal disagreements about scope, terminology or the weight assigned to individual sources. The lead is largely declarative, so disagreement and counter-evidence require a deliberate search beyond the opening account. Authority statements aid reconciliation but still require their own references, qualifiers and ranks to be checked.
How to read it
Use the entry as an orientation point, then follow its citations and revision history. Names, dates and institutional relationships should be checked against the original record.
- Subject orientation
- Search vocabulary
- Locating named sources
The closest primary source, responsible institution and strongest cited specialist reference.
Three-step research path
- Establish the record: confirm the title “V1005 Orionis”, its source revision and the description used here.
- Expand the search: follow V1005 Orionis primary sources, V1005 Orionis archive and V1005 research across catalogues and specialist indexes.
- Test the account: compare the strongest cited source with the responsible institution’s current record and note any disagreement.
Questions for further research
- Which source most directly establishes the central claim about “V1005 Orionis”?
- What terminology or title could unlock a more precise catalogue search?
- Which institution is responsible for the underlying evidence?
Search terms from this dossier
This entry incorporates text from “V1005 Orionis” on English Wikipedia. Contributors are listed in the page history. Text is available under the Creative Commons Attribution-ShareAlike 4.0 License. Selected authority identifiers and statements are retrieved from Wikidata under CC0; their references and qualifiers remain part of the verification path.