Alight curve for V366 Aquarii, adapted from Jeffery (2011)[12]
Amir Ahmad and C. Simon Jeffery discovered that the star is avariable star, in 2004, and published their discovery in 2005. They detected two pulsation periods, 1950 and 2900 seconds.[13] The star's atmosphere contains 10,000 times morezirconium (per unit mass) than theSun's; it also has between 1,000 and 10,000 times the amount ofstrontium,germanium andyttrium than the Sun. The heavy metals are believed to be in cloud layers in the atmosphere where the ions of each metal have a particular opacity that allows radiational levitation to balance gravitational settling.[10]
^abZacharias, N.; Finch, C. T.; Girard, T. M.; Henden, A.;Bartlett, J. L.; Monet, D. G.; Zacharias, M. I. (2012). "VizieR Online Data Catalog: UCAC4 Catalogue (Zacharias+, 2012)".VizieR On-line Data Catalog: I/322A. Originally Published in: 2012yCat.1322....0Z; 2013AJ....145...44Z.1322.Bibcode:2012yCat.1322....0Z.
^abcDorsch, M.; Latour, M.; Heber, U.; Irrgang, A.; Charpinet, S.; Jeffery, C. S. (2020). "Heavy-metal enrichment of intermediate He-sdOB stars: The pulsators Feige 46 and LS IV-14°116 revisited".Astronomy and Astrophysics.643: A22.arXiv:2009.09032.Bibcode:2020A&A...643A..22D.doi:10.1051/0004-6361/202038859.
^abGreen, E. M.; Guvenen, B.; O'Malley, C. J.; O'Connell, C. J.; Baringer, B. P.; Villareal, A. S.; Carleton, T. M.; Fontaine, G.; Brassard, P.; Charpinet, S. (2011). "The Unusual Variable Hot B Subdwarf LS IV-14°116".The Astrophysical Journal.734 (1): 59.Bibcode:2011ApJ...734...59G.doi:10.1088/0004-637X/734/1/59.S2CID122292750.
