The First Light Curve Solutions of GW Leo and Period Study of Two Contact Binary Systems. (arXiv:2011.02903v3 [astro-ph.SR] UPDATED)

<a href="http://arxiv.org/find/astro-ph/1/au:+Poro_A/0/1/0/all/0/1">Atila Poro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Halavati_A/0/1/0/all/0/1">Afshin Halavati</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lashgari_E/0/1/0/all/0/1">Elahe Lashgari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gardi_A/0/1/0/all/0/1">Ali Gardi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+GholizadehSoghar_K/0/1/0/all/0/1">Keyvan GholizadehSoghar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dashti_Y/0/1/0/all/0/1">Yasaman Dashti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mohammadizadeh_F/0/1/0/all/0/1">Fatemeh Mohammadizadeh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hedayatjoo_M/0/1/0/all/0/1">Mahya Hedayatjoo</a>

We performed the first light curve analysis of GW Leo and a new ephemeris is

obtained for QT Boo. In the present photometric study of two contact binary

systems, we found that the period of these binary systems is decreasing at a

rate of dp/dt=-6.21*10^(-3) days yr^(-1) for GW Leo, and dp/dt=-4.72*10^(-3)

days yr^(-1) for QT Boo, respectively. The light curve investigation also

yields that the system GW Leo is a contact W UMa eclipsing binary with a

photometric mass ratio of q=0.881+-0.030, a fillout factor of f=3%, and an

inclination of 54.060+-0.066 deg. Due to the O’Connell effect which is known as

asymmetries in the light curves’ maxima, a cold spot is employed along with the

solution. We also calculate the distance of GW Leo from the distance modulus

formula as 465.58+-23 pc, which is relatively close to the quantity measured by

the Gaia DR2 using the binary systems’ parallax. Moreover, the positions of

their components on the H-R diagram are represented.

We performed the first light curve analysis of GW Leo and a new ephemeris is

obtained for QT Boo. In the present photometric study of two contact binary

systems, we found that the period of these binary systems is decreasing at a

rate of dp/dt=-6.21*10^(-3) days yr^(-1) for GW Leo, and dp/dt=-4.72*10^(-3)

days yr^(-1) for QT Boo, respectively. The light curve investigation also

yields that the system GW Leo is a contact W UMa eclipsing binary with a

photometric mass ratio of q=0.881+-0.030, a fillout factor of f=3%, and an

inclination of 54.060+-0.066 deg. Due to the O’Connell effect which is known as

asymmetries in the light curves’ maxima, a cold spot is employed along with the

solution. We also calculate the distance of GW Leo from the distance modulus

formula as 465.58+-23 pc, which is relatively close to the quantity measured by

the Gaia DR2 using the binary systems’ parallax. Moreover, the positions of

their components on the H-R diagram are represented.

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