Burangalul: Difference between revisions
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The name " | Authors: IAU-WGSN Etymology Group, {{PAGEAUTHORS}} | ||
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[[File:Boomerang DarkSparklers+Stellarium.jpg|thumb|Buran, the Boomerang, in Musca according to Cairns and Harney (2004)<ref name=":0">Hugh Cairns and Bill Y. Harney (2004). Dark Sparklers, Cairns (Australia).</ref> and Stellarium.]] | |||
The name "Burangalul" is documented for the star α Muscae in the Wardaman culture, which is Indigenous to Australia.<ref name=":0" /> | |||
==Etymology and History== | ==Etymology and History== | ||
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==IAU Working Group on Star Names== | ==IAU Working Group on Star Names== | ||
The name was | The Wardaman name Burangalul was proposed in IAU WGSN deliberations in 2023 for α Mus, the brightest star in the constellation Musca, which had not previously had any star names adopted yet by WGSN. | ||
α Mus (HD 109668, HR 4798, HIP 61585) is a spectral type B2IV star with apparent V magnitude 2.65 ([https://simbad.cds.unistra.fr/simbad/sim-id?Ident=alf+Mus&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id SIMBAD]) situated approximately 97 parsecs away. The star is part of a multiple system, IDed in Washington Double Star catalog as WDS J12372-6908. There is a 13th magnitude companion 13 arcseconds away that shares motion with α Mus (IDed in SIMBAD as alf Mus B, HD 109668B, or Gaia DR3 5855593385874666368), however thus far this component is not yet in WDS. Stars B, C, D, E of WDS J12372-6908 do not share motion with α Mus, and hence do not appear to be physical companions. WDS also splits α Mus itself (WDS J12372-6908A) into an Aa+Ab pair reported by [https://ui.adsabs.harvard.edu/abs/2013MNRAS.436.1694R/abstract Rizzuto et al. (2013)], for which they report having resolved the system twice in 2010. [https://ui.adsabs.harvard.edu/abs/2012MNRAS.424.1925C Chini et al. (2012)] reported α Mus as a SB2 spectroscopic binary, confirming that the close companion is bright enough to be detected spectroscopically as well. Rizzuto et al. reported the companion to be ~2.7 magnitudes fainter than the primary (in a broad wavelength range of ~550-800nm), and its position angle changed by roughly 25 degrees in less than a month between July and August 2010, consistent with the orbital period being roughly a year. Given the small differences in magnitudes, the companion Ab is likely a late B-type star. The α Mus system is part of the Lower Centaurus Crux subregion of the [[wikipedia:Scorpius–Centaurus_association|Scorpius-Centaurus association]] - the nearest such large association containing numerous hot, young stars (with ages of roughly 10 million years). | |||
== Weblinks == | == Weblinks == | ||
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* [[References|References (general)]] | * [[References|References (general)]] | ||
[[Category:Asterism]] | |||
[[Category:Single star-asterism]] | [[Category:Single star-asterism]] | ||
[[Category:Star Name]] | [[Category:Star Name]] | ||
[[Category:Mus]] [[Category:Oceania]] | |||
[[Category:Australia]] | [[Category:Australia_and_New_Zealand]][[Category:Australia]] | ||
[[Category:Wardaman]] | [[Category:Wardaman]] | ||
Latest revision as of 08:29, 11 July 2026
Authors: IAU-WGSN Etymology Group, Eric Mamajek, Susanne M Hoffmann, Youla Azkarrula
The name "Burangalul" is documented for the star α Muscae in the Wardaman culture, which is Indigenous to Australia.[1]
Etymology and History
"forehead band" of the "Buran" [Boomerang = Musca] ("Dark Sparklers", Cairns & Harney 2003: p.202)
Mythology
IAU Working Group on Star Names
The Wardaman name Burangalul was proposed in IAU WGSN deliberations in 2023 for α Mus, the brightest star in the constellation Musca, which had not previously had any star names adopted yet by WGSN.
α Mus (HD 109668, HR 4798, HIP 61585) is a spectral type B2IV star with apparent V magnitude 2.65 (SIMBAD) situated approximately 97 parsecs away. The star is part of a multiple system, IDed in Washington Double Star catalog as WDS J12372-6908. There is a 13th magnitude companion 13 arcseconds away that shares motion with α Mus (IDed in SIMBAD as alf Mus B, HD 109668B, or Gaia DR3 5855593385874666368), however thus far this component is not yet in WDS. Stars B, C, D, E of WDS J12372-6908 do not share motion with α Mus, and hence do not appear to be physical companions. WDS also splits α Mus itself (WDS J12372-6908A) into an Aa+Ab pair reported by Rizzuto et al. (2013), for which they report having resolved the system twice in 2010. Chini et al. (2012) reported α Mus as a SB2 spectroscopic binary, confirming that the close companion is bright enough to be detected spectroscopically as well. Rizzuto et al. reported the companion to be ~2.7 magnitudes fainter than the primary (in a broad wavelength range of ~550-800nm), and its position angle changed by roughly 25 degrees in less than a month between July and August 2010, consistent with the orbital period being roughly a year. Given the small differences in magnitudes, the companion Ab is likely a late B-type star. The α Mus system is part of the Lower Centaurus Crux subregion of the Scorpius-Centaurus association - the nearest such large association containing numerous hot, young stars (with ages of roughly 10 million years).
