TESS unveils the phase curve of WASP-33b: Characterization of the planetary atmosphere and the pulsations from the star

被引：34

作者：

von Essen, C. ^{[1
,2
]}

Mallonn, M. ^{[3
]}

Borre, C. C. ^{[1
]}

Antoci, V. ^{[1
,4
]}

Stassun, K. G. ^{[5
]}

Khalafinejad, S. ^{[6
]}

Tautvaisiene, G. ^{[2
]}

机构：

[1] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, Ny Munkegade 120, DK-8000 Aarhus C, Denmark

[2] Vilnius Univ, Inst Theoret Phys & Astron, Astron Observ, Sauletekio Av 3, LT-10257 Vilnius, Lithuania

[3] Leibniz Inst Astrophys Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany

[4] Tech Univ Denmark, Natl Space Inst, DTU Space, Elektrovej 328, DK-2800 Lyngby, Denmark

[5] Vanderbilt Univ, Dept Phys & Astron, 6301 Stevenson Ctr Ln, Nashville, TN 37235 USA

[6] Heidelberg Univ, Landessternwarte, Zentrum Astron, Konigstuhl 12, D-69117 Heidelberg, Germany

来源：

ASTRONOMY & ASTROPHYSICS | 2020年 / 639卷

基金：

新加坡国家研究基金会;

关键词：

planets and satellites: atmospheres; planets and satellites: fundamental parameters; stars: individual: WASP-33; methods: observational; HOST STARS; EMISSION; TEMPERATURES; MASSES; OFFSET; RADII; MAP;

D O I：

10.1051/0004-6361/202037905

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present the detection and characterization of the full-orbit phase curve and secondary eclipse of the ultra-hot Jupiter WASP-33b at optical wavelengths, along with the pulsation spectrum of the host star. We analyzed data collected by the Transiting Exoplanet Survey Satellite (TESS) in sector 18. WASP-33b belongs to a very short list of highly irradiated exoplanets that were discovered from the ground and were later visited by TESS. The host star of WASP-33b is of delta Scuti-type and shows nonradial pulsations in the millimagnitude regime, with periods comparable to the period of the primary transit. These completely deform the photometric light curve, which hinders our interpretations. By carrying out a detailed determination of the pulsation spectrum of the host star, we find 29 pulsation frequencies with a signal-to-noise ratio higher than 4. After cleaning the light curve from the stellar pulsations, we confidently report a secondary eclipse depth of 305.8 +/- 35.5 parts-per-million (ppm), along with an amplitude of the phase curve of 100.4 +/- 13.1 ppm and a corresponding westward offset between the region of maximum brightness and the substellar point of 28.7 +/- 7.1 degrees, making WASP-33b one of the few planets with such an offset found so far. Our derived Bond albedo, A(B) = 0.369 +/- 0.050, and heat recirculation efficiency, = 0.189 +/- 0.014, confirm again that he behavior of WASP-33b is similar to that of other hot Jupiters, despite the high irradiation received from its host star. By connecting the amplitude of the phase curve to the primary transit and depths of the secondary eclipse, we determine that the day- and nightside brightness temperatures of WASP-33b are 3014 +/- 60 K and 1605 +/- 45 K, respectively. From the detection of photometric variations due to gravitational interactions, we estimate a planet mass of M-P = 2.81 +/- 0.53 M-J. Based on analyzing the stellar pulsations in the frame of the planetary orbit, we find no signals of star-planet interactions.

引用

页数：19

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