This is a multi-period
Beta Cephei variable with a dominant oscillation period of 0.232 days.[5] It is a
proper motion member of the Upper Centaurus–Lupus sub-group in the
Scorpius–CentaurusOB association, the nearest such co-moving association of massive stars to the Sun.[6] Beta Lupi has a high
proper motion of more than 50
mas per year, suggesting a significant transverse velocity.[13]
^
abcWielen, R.; et al. (1999), "Sixth Catalogue of Fundamental Stars (FK6). Part I. Basic fundamental stars with direct solutions", Veroeffentlichungen des Astronomischen Rechen-Instituts Heidelberg, 35 (35), Astronomisches Rechen-Institut Heidelberg: 1,
Bibcode:
1999VeARI..35....1W
^
abcdde Geus, E. J.; de Zeeuw, P. T.; Lub, J. (June 1989), "Physical parameters of stars in the Scorpio-Centaurus OB association", Astronomy and Astrophysics, 216 (1–2): 44–61,
Bibcode:
1989A&A...216...44D
^Underhill, A. B.; et al. (November 1979), "Effective temperatures, angular diameters, distances and linear radii for 160 O and B stars", Monthly Notices of the Royal Astronomical Society, 189 (3): 601–605,
Bibcode:
1979MNRAS.189..601U,
doi:10.1093/mnras/189.3.601
^Sinnott, Roger W.; Perryman, Michael A. C. (1997), Millennium Star Atlas, vol. 2, Sky Publishing Corporation and the European Space Agency, p. 929,
ISBN0-933346-83-2.
^(in Chinese)中國星座神話, written by 陳久金. Published by 台灣書房出版有限公司, 2005,
ISBN978-986-7332-25-7.