We have obtained new spectroscopy and photometry of the K0 IV, chromospherically active, single-lined spectroscopic binary HD 10909. Those observations show that the previously reported orbital and light variability periods are incorrect. HD 10909 has an orbital period of 30.1067 days and an eccentricity of 0.499. Its rotation period of 64.1 days is more than twice as long as its orbital period. The primary is situated near the base of the first-ascent red giant branch. Thus, its asynchronous rotation is likely the result of its recent evolution through the Hertzsprung gap, combined with its relatively long orbital period and high eccentricity.
Fekel, F.C.; Henry, G.W.; Brooks, K.; Hall, D.S. "Chromospherically Active Stars. XIX. A Reexamination of the Variability of HD 10909=UV Fornacis" The Astronomical Journal, Volume 122, Issue 2, pp. 991-996 (2001).