BO Ari Light Curve Analysis using Ground-Based and TESS Data
Atila Poro, Shiva Zamanpour, Maryam Hashemi, Yasemin Alada?, Nazim Aksaker, Samaneh Rezaei, Arif Solmaz
11 BO Ari Light Curve Analysis using Ground-Based and TESS Data
Atila Poro , Shiva Zamanpour , Maryam Hashemi , Yasemin AladaΔ , Nazim Aksaker , Samaneh Rezaei , Arif Solmaz The International Occultation Timing Association Middle East section, Iran, [email protected] Adana Organised Industrial Zones Vocational School of Technical Science, University of Γukurova, 01410, Adana, Turkey Space Science and Solar Energy Research and Application Center (UZAYMER), University of Γukurova, 01330, Adana, Turkey
ABSTRACT
We present new BVR band photometric light curves of BO Aries obtained in 2020 and combined them with the Transiting Exoplanet Survey Satellite (TESS) light curves. We obtained times of minima based on Gaussian and Cauchy distributions and then applied the Monte Carlo Markov Chain (MCMC) method to measure the amount of uncertainty from our CCD photometry and TESS data. A new ephemeris of the binary system was computed employing 204 times of minimum. The light curves were analyzed using the Wilson-Devinney binary code combined with the Monte Carlo (MC) simulation. For this light curve solution, we considered a dark spot on the primary component. We conclude that this binary is an A-type system with a mass ratio of π = 0.2074 Β±0.0001 , an orbital inclination of π = 82.18 Β± 0.02 deg, and a fillout factor of π = 75.7 Β± 0.8% . Our results for the π ( π β ) and π parameters are consistent with the results of the Xu-Dong Zhang and Sheng-Bang Qian (2020) model. The absolute parameters of the two components were calculated and the distance estimate of the binary system was found to be
142 Β± 9 pc. Keywords: Techniques: photometric; Stars: binaries: eclipsing; Stars: individual: BO Ari
1. INTRODUCTION
EW-type binaries are systems with main characteristics such as fairly equal depth eclipsing light curves, short orbital periods, less than one day, and frequently mass transfer between the two components which are in contact with each other sharing a common convective envelope. Eclipsing binaries can provide fundamental stellar properties and critical tests on the theories of stellar evolution and structure (Yuan et al. 2019). Nicholson and Varley (2006) discovered the short-period binary system BO Ari (ASAS J021208+2708.2) and determined the first orbital period of (cid:3031) . It was later observed by Acerbi et al. (2011) and classiο¬ed as an A-type W Ursae Majoris system with a mass ratio of π = 0.1889 and contact degree of π = 58.7% . GΓΌrol et al. (2015) made the first Spectroscopic observations and derived the π = 0.19024 and π = 49.8% by combining a light and radial velocity curve solution. Through the
π΅ππ observations done by Kriwattanawong et al. (2016) a mass ratio of π = 0.1754 and contact degree of π = 27.72% were obtained for the binary system. In this study, the multi-color CCD light curves in π΅ , π , and π bands along with photometric data obtained from the TESS are presented. We determined a new ephemeris for this binary system. The light curve solution with Wilson-Devinney code combined with the MC simulation was performed to obtain reliable photometric parameters. Absolute parameters and distance of the system were derived.
2. NEW PHOTOMETRIC OBSERVATION
The observation of BO Ari was carried out by a 50 cm Ritchey-Chretien RC 500/4000 Pro RC SGA OTA telescope and Apogee Aspen CG6 LN-2-G07-S58 type CCD during nine nights of observation at the UZAYMER Observatory, Γukurova University, Adana, Turkey in January 2020. The CCD has a pixel array with a pixel length of 24ΞΌ. In these observation nights, we used the
π΅ππ standard Johnson filters for the photometry. Each of the frames was binned with 40s exposure time for π filter, 60s for π filter, and 90s for π΅ filter; the average temperature of the CCD was -43 o C during the observations. TYC 1761-2002-1, TYC 1761-1358-1, WISEA J021218.9 (NED), and WISEA J021158.5 (NED) were chosen as comparison stars, and BD+26 369 was selected as a check star. All of these stars are close to BO Ari and the magnitude of the check star is appropriate. Figure 1 shows an observed field-of-view for BO Ari with the comparisons and check stars; The characteristics of these stars are shown in Table 1.
Figure 1. Observed field-of-view for BO Ari, comparison stars, and check star.
Table 1. Characteristics of the variable, comparison and check stars (from: Vizier-APASS9).
Star type Star name RA (J2000) DEC (J2000) Magnitude ( π ) Variable BO Ari 02 12 08.7070 +27 08 18.6180 10.169 Check BD+26 369 02 12 11.1814 +27 10 19.8948 10.263 Comparison TYC 1761-2002-1 02 12 22.4090 +27 08 33.4968 11.588 Comparison TYC 1761-1358-1 02 12 01.7561 +27 07 03.1260 12.061 Comparison WISEA J021218.9 (NED) 02 12 19.0166 +27 07 52.9630 12.780 Comparison WISEA J021158.5 (NED) 02 11 58.5466 +27 07 53.1830 12.590 We reduced the raw CCD images and the basic data reduction was performed for bias, dark and flat-field according to the standard method. We aligned, reduced, and plotted raw images with AstroImageJ (AIJ) software (Collins et al. 2017). AIJ provides an astronomy-specific image display environment and tools for astronomy-specific image calibration and data reduction. This software has been determined to identify the best linear fit of a dataset (by exerting air mass) to the light curve (Davoudi et al. 2020). The study of eclipsing binaries has been advanced significantly with an increasing rate of discoveries as a result of space satellites. The Transiting Exoplanet Survey Satellite (TESS) is one of the recent missions that obtained new photometric observations data from numerous numbers of known eclipsing binaries. In this mission, the studied stars were 30 to 100 times brighter than those the Kepler mission and K2 follow-up surveyed, which enabled far easier follow-up observations with both ground-based and space-based telescopes. TESS also covered a sky area 400 times larger than that monitored by Kepler. BO Ari (TIC 5674169) was observed by the TESS mission. TESS data of this binary system is available at the Mikulski Space Telescope Archive (MAST). We extracted TESS style curves using LightKurve code from the MAST. It was observed in sector 18 by Camera 1 and CCD 3 in 120 seconds cadences. Its detrended light curves were extracted from the MAST.
3. NEW EPHEMERIS https://docs.lightkurve.org/ Four primary and five secondary minimum times were determined from our observed light curves. They were found through fitting the models to the light curves and existing minima based on Gaussian and Cauchy distributions. We then employed the Monte Carlo Markov Chain (MCMC) method to measure the amount of uncertainty related to each value (Poro et al. 2020). We also benefited from Python along with its PyMC3 package to execute the lines of code (Salvatier et al. 2016). According to this method, we also calculated all times of minima of the TESS data for this binary system. Thus, 48 new times of minima were obtained from the TESS data. Based on our observations, TESS data, and other literature we obtained 204 timings of minimum light including 98 primary and 106 secondary times of minima, given in Table 2. We used the following reference ephemeris (Acerbi et al. 2011), for calculating epoch and O-C values,
π΅π½π· (cid:3021)(cid:3005)(cid:3003) (πππ. πΌ) = 2452625.64163 + 0.3181963 Γ πΈ. (1)
We fitted all mid-transit timings with a line, using the Robust regression and determined a new ephemeris for primary minimum as,
πππ πΌ (π΅π½π· (cid:3021)(cid:3005)(cid:3003) ) = (2452625.650338 Β± 0.001993) + (0.318194081 Β± 0.000000114) Γ πΈ πππ¦π (2) where πΈ is an integer of orbital cycles after the reference epoch. Table 2. Times of minima of BO Ari.
BJD
TDB (Min.) Error Epoch O-C Reference BJD
TDB (Min.) Error Epoch O-C Reference 2451479.6573 -3601.5 -0.0004 Nicholson et al. 2006 2458798.7735 0.0002 19400.5 -0.0354 TESS 2452625.6416 0 0 Acerbi et al. 2011 2458798.9341 0.0001 19401 -0.0339 TESS 2454049.4086 0.0025 4474.5 -0.0024 Martignoni 2011 2458799.0918 0.0002 19401.5 -0.0353 TESS 2454062.4588 4515.5 0.0018 Acerbi et al. 2011 2458799.2523 0.0001 19402 -0.0339 TESS 2454080.4341 4572 -0.0010 Acerbi et al. 2011 2458799.4099 0.0002 19402.5 -0.0354 TESS 2454081.3885 4575 -0.0012 Acerbi et al. 2011 2458799.5706 0.0001 19403 -0.0338 TESS 2454083.2986 4581 -0.0003 Acerbi et al. 2011 2458799.7281 0.0002 19403.5 -0.0354 TESS 2454083.4591 4581.5 0.0011 Acerbi et al. 2011 2458799.8888 0.0001 19404 -0.0338 TESS 2454084.4135 0.0003 4584.5 0.0009 Martignoni 2011 2458800.0463 0.0002 19404.5 -0.0354 TESS 2454095.3901 4619 -0.0002 Acerbi et al. 2011 2458800.2071 0.0001 19405 -0.0337 TESS 2454507.2988 0.0100 5913.5 0.0033 Paschke 2009 2458800.3645 0.0002 19405.5 -0.0354 TESS 2454808.3048 0.0100 6859.5 -0.0043 Paschke 2009 2458800.5252 0.0001 19406 -0.0338 TESS 2455080.3633 0.0003 7714.5 -0.0037 Demircan et al. 2011 2458800.6827 0.0002 19406.5 -0.0354 TESS 2455080.5190 0.0001 7715 -0.0071 Gokay et al. 2010 2458800.8435 0.0001 19407 -0.0337 TESS 2455103.4287 0.0003 7787 -0.0075 Gokay et al. 2010 2458801.1164 0.0021 19408 -0.0790 TESS 2455103.5895 0.0004 7787.5 -0.0058 Gokay et al. 2010 2458801.0023 0.0003 19407.5 -0.0340 TESS 2455144.3197 0.0008 7915.5 -0.0047 Gokay et al. 2010 2458801.6384 0.0002 19409.5 -0.0343 TESS 2455392.5079 0.0001 8695.5 -0.0097 Demircan et al. 2011 2458801.7980 0.0001 19410 -0.0338 TESS 2455487.3302 0.0002 8993.5 -0.0099 Gokay et al. 2012 2458801.9552 0.0002 19410.5 -0.0357 TESS 2455487.4897 0.0001 8994 -0.0095 Gokay et al. 2012 2458802.1158 0.0002 19411 -0.0342 TESS 2455509.2849 9062.5 -0.0107 GΓΌrol et al. 2015 2458803.5463 0.0002 19415.5 -0.0356 TESS 2455509.4448 0.0008 9063 -0.0099 Gokay et al. 2012 2458803.7071 0.0001 19416 -0.0339 TESS 2455528.3776 9122.5 -0.0098 Gokay et al. 2012 2458803.8645 0.0002 19416.5 -0.0356 TESS 2455538.2425 9153.5 -0.0090 GΓΌrol et al. 2015 2458804.0254 0.0001 19417 -0.0338 TESS 2455551.2880 0.0001 9194.5 -0.0095 Gokay et al. 2012 2458804.1827 0.0002 19417.5 -0.0356 TESS 2455553.1970 0.0001 9200.5 -0.0097 Gokay et al. 2012 2458804.3435 0.0001 19418 -0.0339 TESS 2455553.3538 9201 -0.0120 GΓΌrol et al. 2015 2458804.5009 0.0002 19418.5 -0.0356 TESS 2455887.1404 10250 -0.0133 Kriwattanawong 2016 2458804.6616 0.0001 19419 -0.0340 TESS 2455890.1630 10259.5 -0.0136 Kriwattanawong 2016 2458804.8192 0.0002 19419.5 -0.0355 TESS 2455890.3228 10260 -0.0129 Kriwattanawong 2016 2458804.9797 0.0001 19420 -0.0341 TESS 2455892.0724 10265.5 -0.0133 Kriwattanawong 2016 2458805.1373 0.0002 19420.5 -0.0356 TESS 2455892.2325 10266 -0.0123 Kriwattanawong 2016 2458805.2979 0.0001 19421 -0.0341 TESS 2456167.9468 0.0020 11132.5 -0.0151 Nelson 2013 2458805.4556 0.0002 19421.5 -0.0355 TESS 2456279.6330 0.0001 11483.5 -0.0158 Diethelm 2013 2458805.6159 0.0001 19422 -0.0343 TESS
4. PHOTOMETRIC SOLUTIONS
The BVR light curves from our ground-based observations and TESS light curve were analyzed with the Wilson & Devinney (1971) code combined with Monte Carlo (MC) simulations. This method can accurately obtain parameters and their uncertainties. So we used this method to search mass ratio. The free parameters in MC simulation and their ranges are given in Table 3.
Table 3. Free parameters and searching ranges in MC Simulations.
Parameter Value π (deg) 60-90 π (cid:2870) (K) 5000-6500 Ξ© (cid:2869),(cid:2870) π = (π (cid:2870) /π (cid:2869) ) π π (cid:3046)(cid:3043)(cid:3042)(cid:3047) /π (cid:2869) (π΅ β π) (cid:3003)(cid:3016) (cid:3002)(cid:3045)(cid:3036) = 0 (cid:3040) . 573 . As a result, according to Eker et al. (2020), the effective temperature of the primary component was found to be K. Thus, this temperature value is close to the value as the Gaia DR2 catalog (
K). As shown in Figure 2, the obtained temperature from derived (
π΅ β π ) color for the primary component of BO Ari is also in an acceptable range with the method of Sekiguchi and Fukugita (2000).
Figure 2. BO Ariβs position (red dot) based on the Sekiguchi and Fukugita (2000) results.
The gravity-darkening coefficients π (cid:2869) = π (cid:2870) = 0.32 (Lucy 1967) and bolometric albedo values π΄ (cid:2869) = π΄ (cid:2870) = 0.5 (Rucinski 1969) were used, which correspond to the convective envelopes of both components. We assumed linear limb darkening coefficients taken from the tables published by Van Hamme (1993). The resulted parameter values obtained in the analysis of the light curves of BO Ari are given in Table 4, and the synthetic light curves based on these parameters are given in Figures 3 and 4. Table 4. Photometric solutions of BQ Ari.
Parameter Results π (cid:2869) (K) 5873 π (cid:2870) (K) 5850(35) Ξ© (cid:2869) = Ξ© (cid:2870) π (deg) 82.18(2) π π (cid:2869) /π (cid:3047)(cid:3042)(cid:3047) ( π΅ ) 0.7815(6) π (cid:2870) /π (cid:3047)(cid:3042)(cid:3047) ( π΅ ) 0.2185(4) π (cid:2869) /π (cid:3047)(cid:3042)(cid:3047) ( π ) 0.7818(6) π (cid:2870) /π (cid:3047)(cid:3042)(cid:3047) ( π ) 0.2182(4) π (cid:2869) /π (cid:3047)(cid:3042)(cid:3047) ( π ) 0.7818(6) π (cid:2870) /π (cid:3047)(cid:3042)(cid:3047) ( π ) 0.2182(4) π΄ (cid:2869) = π΄ (cid:2870) π (cid:2869) = π (cid:2870) π ( % ) 75.7(8) π (cid:2869) (back) 0.593(5) π (cid:2869) (side) 0.562(4) π (cid:2869) (pole) 0.508(4) π (cid:2870) (back) 0.353(4) π (cid:2870) (side) 0.278(3) π (cid:2870) (pole) 0.263(3) π (cid:2869) (mean) 0.553(2) π (cid:2870) (mean) 0.295(4) Colatitude spot (deg) 107(2) Longitude spot (deg) 81(1) Radius spot (deg) 21(1) π (cid:3046)(cid:3043)(cid:3042)(cid:3047) /π (cid:3046)(cid:3047)(cid:3028)(cid:3045) Figure 3. The observed light curves of BO Ari (black dots), and synthetic light curves obtained from light curve solutions in the B , V , and R filters (top to bottom respectively) and residuals are plotted; with respect to orbital phase, shifted arbitrarily in the relative flux. Figure 4. TESS observation and synthetic light curves of BO Ari.
The radial velocity of BO Ari is not available in this study, and we just can estimate the absolute parameters (Table 5). Accordingly, the mass of the primary component is derived from the Eker et al. (2020) study, and the mass of the secondary component was calculated from the equation π = (cid:3040) (cid:3118) (cid:3040) (cid:3117) . Table 5. Estimated absolute elements of BO Ari.
Parameter Primary Secondary
πππ π ( π β ) 1.095 0.227(15) π ππππ’π ( π β ) 1.190(7) 0.636(9) πΏπ’πππππ ππ‘π¦ ( πΏ β ) 1.517(15) 0.425(11) π (cid:3029)(cid:3042)(cid:3039) (mag) 4.29(28) 5.67(23) πππ π (cgs) 4.326(16) 4.187(13) π ( π β ) 2.152(18) The 3D view and the geometrical structure of BO Ari is shown in Figure 5. Figure 5. The positions of the components of BO Ari.
We estimated the binary system distance using the results of absolute parameters. The value of π (cid:3049) = 10.14 Β±0.005 was calculated from the observational light curve, and π (cid:3049) = 4.287 Β± 0.03 was obtained using π΅πΆ (cid:2869) =0.003 according to the Eker et al. (2020). Based on these values, we calculated the binary systemβs distance to be
142 Β± 9 pc, using π΄ (cid:3031) (cid:3049) = 0.09 Β± 0.02 (Schlafly and Finkbeiner 2011).
5. CONCLUSIONS
We obtained the temperature of the primary component as
π = 5873
K by using
π΅ β π . This value is very close to the Gaia DR2βs temperate for BO Ari which is
π = 5874 . It is found that BO Ari is a contact binary with a mass ratio of π = 0.2074 Β± 0.0001 , a fillout factor of π = 75.7 Β± 0.8% , and an inclination of π = 82.18 Β± 0.02 πππ . As indicated by the light curve solution, a cool starspot is placed on the primary component. In order to study the characteristics of W UMa contact binaries, Xu-Dong Zhang and Sheng-Bang Qian (2020) have presented π β π , and π β π relations (Equations 3 and 4) π = 10.285 Γ π + 0.00155 (3) πππ (cid:2869)(cid:2868) (1 + π) = 3πππ (cid:2869)(cid:2868) (10.285 Γ π + 0.00155) β 2πππ (cid:2869)(cid:2868)
π β πππ (cid:2869)(cid:2868) (β5198 Γ π + 2.097 β 1.481) (4) where π is the mass ratio, π is the separation between two components, and π is the orbital period in year unit. The boundaries of these relations were given as, π (cid:3048) = 11.587 Γ π + 0.00132 (5) π (cid:3039) = 9.972 Γ π + 0.00132 (6) πππ (cid:2869)(cid:2868) (1 + π) (cid:3048) = 3πππ (cid:2869)(cid:2868) (11.587 Γ π + 0.00132) β 2πππ (cid:2869)(cid:2868) π β πππ (cid:2869)(cid:2868) (β4021 Γ π + 1.868 β 1.300) (7) πππ (cid:2869)(cid:2868) (1 + π) (cid:3039) = 3πππ (cid:2869)(cid:2868) (9.972 Γ π + 0.00132) β 2πππ (cid:2869)(cid:2868)
π β πππ (cid:2869)(cid:2868) (β2701 Γ π β 0.967 + 0.104) (8) We have derived π and π by using the above equations for BO Ari. The results of calculations the Xu-Dong Zhang and Sheng-Bang Qian (2020) relations show that the value of π(π Κ ) = 2.256 and its lower and upper limit are 2.149-2.451; Also, for the π parameter, the value 0.3983 was obtained and the lower and upper limit of 0.0309-0.9389 was estimated; For both of these parameters, our results from this study ( π(π Κ ) = 2.152 , π = 0.2074 ) are in consistent with them. We have shown our system in Figure 6 according to these relations. Figure 6. BO Ariβs position based on the πππ (π + π) β π· relation (blue dot). The suggested value for π (solid line) and the lower and upper limits for it (dotted line) are shown in the diagram. We estimated the absolute parameters related to both components of BO Ari. Mass, radius, bolometric magnitude, and luminosity of the system were obtained. According to the estimated absolute parameters, we measured the distance as
142 Β± 9 pc. The Gaia EDR3 parallax gives a distance value of pc. Therefore, our estimated distance for this binary system seems to be consistent with the Gaia EDR3 distance considering our estimated uncertainty. The componentsβ positions of BO Ari are plotted in the Hertzsprung-Russell (H-R) diagram and are shown in Figure 7, in which it seems the primary component is in the main-sequence, and the secondary component is placed near the ZAMS.
Figure 7. Position of both components of BO Ari on the H-R diagram, in which the theoretical ZAMS and TAMS curves are indicated. According to the low mass ratio, a large of fillout factor, high inclination, and the very small temperature difference between components, we can conclude that BO Ari is an overcontact binary and A-type W UMa binary system. Given that the amount of evidence for a low mass ratio has increased from previous studies, we expect it will become deeper overcontact based on system evolution.
ACKNOWLEDGEMENTS
This manuscript was prepared by a joint cooperation between the International Occultation Timing Association Middle East section (IOTA/ME) and Γukurova University, Adana, Turkey. We thank TΓBΔ°TAK National Observatory for its support in providing the CCD to UZAYMER.
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