IO Com: Is it a Non-secondary Minimum Star?

Abstract

Abstract. Four-color photometry of IO Com, a detached eclipsing binary with a long period (∼ 53 d), was accomplished in [2004][2005][2006][2007][2008]. The absolute astrophysical and orbital parameters of the system were determined by the analysis of the light and radial velocity curves. No secondary minima in the light curves were detected. It was revealed that IO Com is the system with a highly eccentric orbit consisting of the components of mid-F spectral types. The calculated masses and radii of the primary and secondary components are: 1.32 M ⊙ and 1.21 M ⊙ , and 2.45 R ⊙ and 1.51 R ⊙ , respectively. In the HR diagram, both components of the system are in agreement with the PARSEC isochrones for the ages between 1.5 and 2.2 Gyr and the metallicities Z between 0.01 and 0.02.

Hunt for extremely eccentric eclipsing binaries

“…The authors found the highest eccentricity for system ASAS 144242−5904.1 with e = 0.64, which was the maximum eccentricity found for eclipsing binary at that time. The rather questionable eclipsing system IO Com with its eccentric orbit e = 0.69 and P = 53 d is still quite problematic because no secondary eclipse has been detected (Taş & Evren 2014). The rich and precise data provided by the Kepler satellite (Borucki et al 2010) were analysed later and yielded a large number of detached and highly eccentric systems, one of which has an eccentricity of 0.845, but an orbital period of 265 d (Kjurkchieva et al 2017).…”

Hunt for extremely eccentric eclipsing binaries

“…The authors found the highest eccentricity for system ASAS 144242-5904.1 with e=0.64, which was the maximum eccentricity found for eclipsing binary at that time. The rather questionable eclipsing system IO Com with its eccentric orbit e=0.69 and P=53 d is still quite problematic because no secondary eclipse has been detected (Taş & Evren 2014). The rich and precise data provided by the Kepler satellite (Borucki et al 2010) were analysed later and yielded a large number of detached and highly eccentric systems, one of which has an eccentricity of 0.845, but an orbital period of 265 d (Kjurkchieva et al 2017).…”