HAT-P-36. HATNet [3, 4] SuperWASP [5, 6] CoRoT [7] Keper [8] 34 3 Vol. 34, No PROGRESS IN ASTRONOMY Aug., 2016

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1 34 3 Vol. 34, No PROGRESS IN ASTRONOMY Aug., 2016 doi: /j.issn HAT-P-36 1,2,3 ( ) m HAT-P-36 3 IRAF CCD coarse de-correlation SYSREM MCMC HAT-P-36 Mancini Bakos 20 ( ± ) d O C HAT-P-36b HAT-P-36b 1 ( ) 2 Rp F = i R [1, 2] HATNet [3, 4] SuperWASP [5, 6] CoRoT [7] Keper [8] 62.2% ➀ (u ) xupan@ynao.ac.cn ➀

2 TTV (Transit timing varitation) TDV (Transit Duration Varition) [9, 10] HAT-P HATNet (Hungarian Automated Telescope Network) [11] GSC G5 V V = mag HAT-P-36b M p = (1.832 ± 0.099) M J R p = (1.264 ± 0.071) R J P = ( ± ) d ρ p = (1.12 ± 0.19) g cm Maciejewski HAT-P-36b 0.6m Toru HAT-P-36 JKTEBOP TAP O C TTV [12] 2015 Mancini HAT-P-36 Rossiter-McLaughlin Cassini 1.52m CA 1.23m P rot = (15.3 ± 0.4) d HAT-P-36b λ = 14 ± 18 φ = degree [13] Püsküllü HAT-P-36 [14] 1 m HAT-P MCMC (Markov Chain Monte Carlo) HAT-P m HAT-P-36 1 m Andor DW436 CCD R CCD ( 1) 1 HAT-P-36 /s RMS/mag YO-1m R YO-1m R YO-1m R

3 3 HAT-P CCD CCD IRAF CCD CCD apphot mag CCD coarse de-correlation [15] SYEREM [16] Holman MCMC [17] Collier Cameron MCMC [18, 19] HAT-P-36 K 1 e ω γ T 0 P F t T b M X = {T 0, P, F, t T, b, M, K 1, e, ω} MCMC X i = X i 1 + σ X G(0, 1)f. (1) G(0, 1) 0 1 f % Metroplis-Hastings 3.1 MCMC 3 Bakos [11] R 4 T eff g [Fe/H] ξ Claret [20] Mancini P = d

4 MCMC 3.2 T = T 0 + P E T 0 E HAT-P-36b Bakos 3 [11] Mancini 3 [13] ETD ➀ 11 ( 2) 2 T = (± ) + E (± ). (2) 2 HAT-P-36 (O C) /d [11] [11] [11] [13] [13] [13] ETD ETD ETD ETD ETD ETD ETD ETD ETD ETD ETD ➀

5 3 HAT-P χ 2 = 5.11 TTV O C ( 1) HAT-P-36b Holman Murray [21] ( ) M 2 = 16 45π M t P 1 ( P2 P 1 ) 2 (1 e 2 ) 3, (3) M 2 t TTV P 1 P 2 HAT-P-36b e 2 t = d 0.0, 0.05, 0.1, 0.15, 0.2, AU 0.35 AU 0.01 AU 2 13 M J 0.1 AU HAT-P-36 O C 33.6 m/s 2

6 j + 1/j Agol 2005 [22] t = P 1 M 2, (4) 4.5j M 2 + M 1 j t = d 2 : 1 3 : 2 4 : 3 5 : 4 6 : M Bakos [11] 33.6 m/s [23] ( ) 2/3 M p sin i = P 1/3 (1 e 2 ) 1/2 M + M p K, (5) M M p (M J ) i ( ) P (d) K (m/s) M (M ) (5) HAT-P-36 [24, 25] MCMC 3 HAT-P-36b σ ( 3) ( 3) 4 3 MCMC HAT-P-36 M p = M J Mancini [13] M p = M J Bakos [11] M p = M J ( ) R p = R J Mancini R p = R J Bakos R p = R J Mancini HAT-P-36 lg R HK = ( ± 0.066) dex HAT-P-36 (1) Bakos FLWO 1.2m Mancini

7 3 HAT-P HAT-P-36 Mancini Bakos P ± ± ± d / (Rp/R ) ± ± tt ± ± d b R K ± ± ± 0.15 km s 1 γ ± ± 0.10 km s 1 e ± ω ± 63 ( ) i ± ± 1.3 ( ) ρ ± ρ M ± ± ± M R ± ± ± R a ± ± AU Rp ± ± ± RJ Mp ± ± MJ ρp ± ± 0.14 ρj Teq ± ± 55 K

8 mag 0.08 mag 3 HAT-P-36 Cassini 1.52m CA 1.23m FLWO 1.2m YO 1m YO 1m (2) % HAT-P-36b TrES-3b [26] WASP-77Ab [27] WASP-46b [28] HAT-P-23b [29] WASP-135b [30] P = ( ± ) d Mancini Bakos Bakos Mancini [1] Baraffe I, Chabrier G, Barman T. A&A, 2008, 482: 315 [2] Fortney J J, Marley M S, Barnes J W, ApJ, 2007, 659: 1661 [3] Bakos G A, Lazar J, Papp I, et al. PASP, 2002, 114: 974 [4] Bakos G A, Noyes R W, Kovacs G, et al. Transiting Planets. Cambridge: Cambridge Universtity Press, 2009: 21 [5] Christian D J, Pollacco D L, Skillen I, et al. MNRAS, 2006, 372: 1117 [6] Pollacco D L, Skillen I, Cameron A C, et al. PASP, 2006, 118: 1407 [7] Fridlund C V M, Team CoRoT. Physica Scripta, 2008, T130: [8] Borucki W J, Koch D, Basri G, et al. Science, 2010, 327: 977 [9] Fulton B J, Shporer A, Winn J N, et al. AJ, 2011, 142: 84 [10] Kipping D M. MNRAS, 2009, 392: 181 [11] Bakos G Á, Hartman J D, Torres G, et al. AJ, 2012, 144: 19

9 3 HAT-P [12] Maciejewski G, Puchalski D, Saral G, et al. Information Bulletin on Variable Stars, 2013, 6082: 1 [13] Mancini L, Esposito M, Covino E, et al. A&A, 2015, 579: A136 [14] Püsküllü Ç, Soydugan F, Erdem A, et al. ASPC, 2015, 496: 356 [15] Collier C A, Pollacco D, Street R A, et al. MNRAS, 2006, 373: 799 [16] Tamuz O, Mazeh T, Zucker S, MNRAS, 2005, 356: 1466 [17] Holman M J, Winn J N, Latham D W, et al. ApJ, 2006, 652: 1715 [18] Collier C A, Wilson D M, West R G, et al. MNRAS, 2007, 380: 1230 [19] Pollacco D, Skillen I, Collier C A, et al. MNRAS, 2008, 385: 1576 [20] Claret A. A&A, 2000, 363: 1081 [21] Holman M J, Murray N M. Science, 2005, 307: 1288 [22] Agol E, Steffen J, Sari R, et al. MNRAS, 2005, 359: 567 [23] Torres G, Winn J N, Holman M J, ApJ, 2008, 677: 1324 [24] Sun L L, Gu S H, Wang X B, et al. RAA, 2015, 15: 117 [25] Wang X B, Gu S H, Collier C A., et al. RAA, 2013, 13: 593 [26] O Donovan F T, Charbonneau D, Bakos G Á, et al. ApJL, 2007, 663: L37 [27] Maxted P F L, Anderson D R, Collier C A, et al. PASP, 2013, 125: 48 [28] Anderson D R, Collier C A, Gillon M, et al. MNRAS, 2012, 422: 1988 [29] Bakos G Á, Hartman J, Torres G, et al. ApJ, 2011, 742: 116 [30] Spake J J, Brown D J A, Doyle A P, et al. PASP, 2016, 128: Photometric Observations and Study for the Transiting Exoplanetary System HAT-P-36 PAN Xu 1,2,3 (1. Yunnan Observatories, Chinese Academy of Sciences, Kunming , China; 2. Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming , China; 3. University of Chinese Academy of Sciences, Beijing , China) Abstract: We use the 1-meter telescope of Yunnan Observatories and observed three transit events of HAT-P-36 from 2012 to We correct the data for systematic errors based on coarse de-correlation and SYSREM algorithms. Three new transit light curves are analyzed by means of the Markov chain Monte Carlo technique. The value of planet mass acquired in this paper is slightly larger than the results of Mancini and Bakos. Through the analysis of all available mid-transit times of symmetric and complete light curves, I refine the ephemeris of HAT-P-36b, which is better than former ones. Via the O C analysis, I find that this system exists significant transit timing variations. But the Lomb-Scargle periodogram generated for timing residuals show no significant signal. Therefore, I speculate that there is an external perturbing planet and hence this paper also gives some physical parameters range of this perturbing planet. Key words: exoplanet; HAT-P-36; transit event