Photometric Studies of Two Neglected Eclipsing Binaries AX Cassiopeia and V1107 Cassiopeia with Possibly Additional Companions

Abstract

New photometry for two eclipsing binaries, AX Cas and V1107 Cas, was carried out during the 2014-2015 observing season. With an updated version of the W-D program, photometric solutions were simultaneously derived from BV light curves. Results indicate that AX Cas is a semi-detached binary with a mass ratio of q 0.400 0.003for V1107 Cas, respectively. From 26 EB/EW binaries with only cyclic variations, we derived the relation between periods and total masses, indicating that mass loss from the system occurs from the semi-detached configuration to the contact case. The cyclic oscillations for 22 sample stars (including AX Cas and V1107 Cas) may be attributed to third bodies. Additional companions could remove angular momentum from the central systems, which may play a key role in the evolutionary process.

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“…where i is the inclination of the orbital plane of the third body, m 1 is the mass of primary [m ⊙ ], q = m 2 /m 1 is the dimensionless mass ratio of secondary and primary, m 3 is the mass of the third body [m ⊙ ], a = A/2 is half of the peak the peak amplitude of O-C modulation caused by the third body [d], and p 3 is the period of the modulations caused by the third body [y] (Borkovits and Hegedues, 1996;Tanrıver, 2015;Yang et al, 2016). We use the masses m 1 = 3.2m ⊙ and m 2 = 1.3m ⊙ (Demircan et al, 1995, A4 IV + G5 IV).…”