| Article ID | Journal | Published Year | Pages | File Type |
|---|---|---|---|---|
| 1779021 | New Astronomy | 2014 | 6 Pages |
•The photometric elements for the system show that the primary star is more massive and hotter.•The spectral types of the primary and secondary star are K1 and K3 respectively.•The positions of both components on the mass–radius relation show that they above the ZAMS track by about 0.2 magnitudes.
A total of 311 BVRI observations were carried out on 4 May 2013 for the new short period W UMa system 1SWASP J133105.91 + 121538.0 using the 1.88 m reflector telescope of Kottamia Astronomical Observatory (KAO) at NRIAG. A photometric solution of these light curves was obtained by means of Wilson–Devinney (WD) code. A spotted model was applied to treat the asymmetry of the light curve. The results show that the more massive component is hotter than the less massive one with about ΔT ∼ 300 K. The system is at a distance of 89 ± 3.6 pc. Based on the physical parameters of the system, we investigate the evolutionary state of the components. Both components are above the zero age main sequence (ZAMS) track by about 0.2 magnitudes.
