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Light curve analyses of eclipsing binary system ASAS 172533-1221.4
Jatmiko A.T.P.a, Yusuf M.a, Putra M.a
a Bosscha Observatory, Institut Teknologi Bandung, Jl. Peneropongan Bintang, Lembang, West Java, Bandung, Indonesia
[vc_row][vc_column][vc_row_inner][vc_column_inner][vc_separator css=”.vc_custom_1624529070653{padding-top: 30px !important;padding-bottom: 30px !important;}”][/vc_column_inner][/vc_row_inner][vc_row_inner layout=”boxed”][vc_column_inner width=”3/4″ css=”.vc_custom_1624695412187{border-right-width: 1px !important;border-right-color: #dddddd !important;border-right-style: solid !important;border-radius: 1px !important;}”][vc_empty_space][megatron_heading title=”Abstract” size=”size-sm” text_align=”text-left”][vc_column_text]© Published under licence by IOP Publishing Ltd.Using the data taken from our 0.36 m f/7.2 robotic telescope, we performed a very first light curve (LC) analyses of eclipsing binary ASAS 172533-1221.4, one of target stars which is part of program stars in our variable star survey project. The LC of this star was constructed by using LEMON, a semi-automatic photometric pipeline written in Python. We refined a Time of Minima (ToM, T 0) and variability period of this system, P and updated its ephemerides as HJD(min I) = 2457200.255578 + 0.678861 ∗ φ. The LC modeling of the system was conducted with the PHOEBE (PHysics Of Eclipsing BinariEs) software built on top of the widely used WD program . The assorted LC modeling solutions are shown as follows: mass ratio q = 0.811 ± 0.009, inclination i = 70.62 ± 0.01°, temperature of primary and secondary component T 1 = 5559.23 ± 83.51 K and T 2 = 3871.64 ± 43.66 K, respectively, and modified Kopal potentials which are a function of primary’s and secondary’s radii Ω1 = 3.436 ± 0.018 and Ω2 = Ocr = 2.980, respectively. It is concluded that ASAS 1725533-1221.4 is found to be near-contact system with almost similar size between primary and secondary components, with its secondary component is already filling its Roche lobe.[/vc_column_text][vc_empty_space][vc_separator css=”.vc_custom_1624528584150{padding-top: 25px !important;padding-bottom: 25px !important;}”][vc_empty_space][megatron_heading title=”Author keywords” size=”size-sm” text_align=”text-left”][vc_column_text]Contact systems,Eclipsing binaries,Light curves,Robotic telescope,Secondary components,Semi-automatics,Target star,Variable stars[/vc_column_text][vc_empty_space][vc_separator css=”.vc_custom_1624528584150{padding-top: 25px !important;padding-bottom: 25px !important;}”][vc_empty_space][megatron_heading title=”Indexed keywords” size=”size-sm” text_align=”text-left”][vc_column_text][/vc_column_text][vc_empty_space][vc_separator css=”.vc_custom_1624528584150{padding-top: 25px !important;padding-bottom: 25px !important;}”][vc_empty_space][megatron_heading title=”Funding details” size=”size-sm” text_align=”text-left”][vc_column_text][/vc_column_text][vc_empty_space][vc_separator css=”.vc_custom_1624528584150{padding-top: 25px !important;padding-bottom: 25px !important;}”][vc_empty_space][megatron_heading title=”DOI” size=”size-sm” text_align=”text-left”][vc_column_text]https://doi.org/10.1088/1742-6596/1127/1/012048[/vc_column_text][/vc_column_inner][vc_column_inner width=”1/4″][vc_column_text]Widget Plumx[/vc_column_text][/vc_column_inner][/vc_row_inner][/vc_column][/vc_row][vc_row][vc_column][vc_separator css=”.vc_custom_1624528584150{padding-top: 25px !important;padding-bottom: 25px !important;}”][/vc_column][/vc_row]