The multi-color passband CCD light curves of ASAS J124343+1531.7 and LINEAR 2323566 were first obtained by the 0.84 m Ritchey–Chrtien telescope with follow up observations by the WIYN 0.90 m Cassegrain telescope. The data from the Transiting Exoplanet Survey Satellite of ASAS J124343+1531.7 was also applied for subsequent analysis. By analyzing the data through the W-D program, their mass ratios and fill-out factors were determined as 3.758, 1.438 and 31.8%, 14.9%, respectively. ASAS J124343+1531.7 is a W-subtype median contact binary, while LINEAR 2323566 is a W-subtype shallow contact binary, and the asymmetric light curves prove that they both have the O’Connell effect, which is generally explained by magnetic activity. The equivalent widths of H _α lines were calculated, which show they certainly have magnetic activity. Moreover, LINEAR 2323566 has a stronger magnetic activity. The analysis of orbital period changes shows that ASAS J124343+1531.7 has a trend of secular period increase, which is generally explained by the mass transfer from the less massive to the more massive star. According to the estimated absolute parameters, their evolutionary states are discussed. The two components of ASAS J124343+1531.7 are both main sequence stars. While for LINEAR 2323566, the more massive star is a main sequence star, the less massive star has evolved out of main sequence and is over-luminous and over-sized.

ASAS J124343+1531.7和LINEAR 2323566的多色通带CCD光变曲线首先由0.84 m Ritchey-Chrtien望远镜获得，并由WIYN 0.90 m Cassegrain望远镜进行后续观测。来自ASAS J124343+1531.7的凌日系外行星测量卫星的数据也用于后续分析。通过WD程序分析数据，确定它们的质量比和填充因子分别为3.758、1.438和31.8%、14.9%。ASAS J124343+1531.7是W亚型中位接触双星，而LINEAR 2323566是W亚型浅接触双星，不对称光变曲线证明它们都具有奥康奈尔效应，一般用磁活动来解释。H _α的等效宽度 计算出的线表明它们肯定具有磁活性。此外，LINEAR 2323566 具有更强的磁活性。对轨道周期变化的分析表明，ASAS J124343+1531.7 具有长期周期增加的趋势，这通常可以用质量从较小质量的恒星转移到较大质量的恒星来解释。根据估计的绝对参数，讨论它们的进化状态。ASAS J124343+1531.7 的两个组成部分都是主序星。而对于LINEAR 2323566，质量越大的恒星是主序星，质量越小的恒星从主序演化出来的恒星过亮、过大。