Alight curve for IZ Velorum, plotted fromTESS data.[11] The 0.905 day period derived by Balona is marked in red.
In 1986, Balona & Laing stated that HR 3600 in fact only had a single period of 1.10 days, analias of the 9.64-day period presented by Burki et al. Citing the variable radial velocity of the star (20-30 km/s) and the low projectedrotational velocity (50 km/s), they argued that it was more likely arotating ellipsoidal variable, in which case the system would consist of a closebinary orbiting each other every 2.20 days.[12] In 1994, Balona, who continued to observe the variable, revised the period to 0.905 days (or possibly 1.81 days), which was another alias of the 9.64-day period. The 14.4-day period could not be detected. The low rotational velocity contradicts the hypotheses that the variability is caused by either binarity orrotational modulation, so the exact nature of this star has yet to be determined.[5]
^abcHøg, E.; et al. (February 2000). "The Tycho-2 Catalogue of the 2.5 Million Brightest Stars".Astronomy and Astrophysics.355 (1):L27 –L30.Bibcode:2000A&A...355L..27H.
^abcCutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E.; Fowler, John W.; Gizis, John E.; Howard, Elizabeth V.; Huchra, John P.; Jarrett, Thomas H.; Kopan, Eugene L.; Kirkpatrick, J. Davy; Light, Robert M.; Marsh, Kenneth A.; McCallon, Howard L.; Schneider, Stephen E.; Stiening, Rae; Sykes, Matthew J.; Weinberg, Martin D.; Wheaton, William A.; Wheelock, Sherry L.; Zacarias, N. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)".CDS/ADC Collection of Electronic Catalogues.2246: II/246.Bibcode:2003yCat.2246....0C.
^abcdNorth, P.; Paltani, S. (August 1994). "HD 37151: a new "slowly pulsating B star"".Astronomy & Astrophysics.288:155–164.Bibcode:1994A&A...288..155N.
