The tidal deformation and atmosphere of WASP-12b from its phase curve

B. Akinsanmi; S. C. C. Barros; M. Lendl; L. Carone; P. E. Cubillos; A. Bekkelien; A. Fortier; H.-G. Florén; A. Collier Cameron; G. Boué; G. Bruno; B.-O. Demory; A. Brandeker; S. G. Sousa; T. G. Wilson; A. Deline; A. Bonfanti; G. Scandariato; M. J. Hooton; A. C. M. Correia; O. D. S. Demangeon; A. M. S. Smith; V. Singh; Y. Alibert; R. Alonso; J. Asquier; T. Bárczy; D. Barrado Navascues; W. Baumjohann; M. Beck; T. Beck; W. Benz; N. Billot; X. Bonfils; L. Borsato; C. Broeg; M. Buder; S. Charnoz; Sz. Csizmadia; M. B. Davies; M. Deleuil; L. Delrez; D. Ehrenreich; A. Erikson; J. Farinato; L. Fossati; M. Fridlund; D. Gandolfi; M. Gillon; M. Güdel; M. N. Günther; A. Heitzmann; Ch. Helling; S. Hoyer; K. G. Isaak; L. L. Kiss; K. W. F. Lam; J. Laskar; A. Lecavelier des Etangs; D. Magrin; P. F. L. Maxted; M. Mecina; C. Mordasini; V. Nascimbeni; G. Olofsson; R. Ottensamer; I. Pagano; E. Pallé; G. Peter; D. Piazza; G. Piotto; D. Pollacco; D. Queloz; R. Ragazzoni; N. Rando; H. Rauer; I. Ribas; N. C. Santos; D. Ségransan; A. E. Simon; M. Stalport; Gy. M. Szabó; N. Thomas; S. Udry; V. Van Grootel; J. Venturini; E. Villaver; N. A. Walton

doi:10.1051/0004-6361/202348502

The tidal deformation and atmosphere of WASP-12b from its phase curve

B. Akinsanmi, S. C. C. Barros, M. Lendl, L. Carone, P. E. Cubillos, A. Bekkelien, A. Fortier, H.-G. Florén, A. Collier Cameron, G. Boué, G. Bruno, B.-O. Demory, A. Brandeker, S. G. Sousa, T. G. Wilson, A. Deline, A. Bonfanti, G. Scandariato, M. J. Hooton, A. C. M. CorreiaO. D. S. Demangeon, A. M. S. Smith, V. Singh, Y. Alibert, R. Alonso, J. Asquier, T. Bárczy, D. Barrado Navascues, W. Baumjohann, M. Beck, T. Beck, W. Benz, N. Billot, X. Bonfils, L. Borsato, C. Broeg, M. Buder, S. Charnoz, Sz. Csizmadia, M. B. Davies, M. Deleuil, L. Delrez, D. Ehrenreich, A. Erikson, J. Farinato, L. Fossati, M. Fridlund, D. Gandolfi, M. Gillon, M. Güdel, M. N. Günther, A. Heitzmann, Ch. Helling, S. Hoyer, K. G. Isaak, L. L. Kiss, K. W. F. Lam, J. Laskar, A. Lecavelier des Etangs, D. Magrin, P. F. L. Maxted, M. Mecina, C. Mordasini, V. Nascimbeni, G. Olofsson, R. Ottensamer, I. Pagano, E. Pallé, G. Peter, D. Piazza, G. Piotto, D. Pollacco, D. Queloz, R. Ragazzoni, N. Rando, H. Rauer, I. Ribas, N. C. Santos, D. Ségransan, A. E. Simon, M. Stalport, Gy. M. Szabó, N. Thomas, S. Udry, V. Van Grootel, J. Venturini, E. Villaver, N. A. Walton

Research output: Contribution to journal › Article › peer-review

Abstract

Context. Ultra-hot Jupiters present a unique opportunity to understand the physics and chemistry of planets, their atmospheres, and interiors at extreme conditions. WASP-12 b stands out as an archetype of this class of exoplanets, with a close-in orbit around its star that results in intense stellar irradiation and tidal effects.

Aims. The goals are to measure the planet’s tidal deformation, atmospheric properties, and also to refine its orbital decay rate.

Methods. We performed comprehensive analyses of the transits, occultations, and phase curves of WASP-12b by combining new CHEOPS observations with previous TESS and Spitzer data. The planet was modeled as a triaxial ellipsoid parameterized by the second-order fluid Love number of the planet, h₂, which quantifies its radial deformation and provides insight into the interior structure.

Results. We measured the tidal deformation of WASP-12b and estimated a Love number of h₂ = 1.55_−0.49^+0.45 (at 3.2σ) from its phase curve. We measured occultation depths of 333 ± 24 ppm and 493 ± 29 ppm in the CHEOPS and TESS bands, respectively, while the nightside fluxes are consistent with zero, and also marginal eastward phase offsets. Our modeling of the dayside emission spectrum indicates that CHEOPS and TESS probe similar pressure levels in the atmosphere at a temperature of ~2900 K. We also estimated low geometric albedos of A_g = 0.086 ± 0.017 and A_g = 0.01 ± 0.023 in the CHEOPS and TESS passbands, respectively, suggesting the absence of reflective clouds in the high-temperature dayside of the planet. The CHEOPS occultations do not show strong evidence for variability in the dayside atmosphere of the planet at the median occultation depth precision of 120 ppm attained. Finally, combining the new CHEOPS timings with previous measurements refines the precision of the orbital decay rate by 12% to a value of −30.23 ± 0.82 ms yr⁻¹, resulting in a modified stellar tidal quality factor of Q′★ = 1.70 ± 0.14 × 10⁵.

Conclusions. WASP-12 b becomes the second exoplanet, after WASP-103b, for which the Love number has been measured from the effect of tidal deformation in the light curve. However, constraining the core mass fraction of the planet requires measuring h₂ with a higher precision. This can be achieved with high signal-to-noise observations with JWST since the phase curve amplitude, and consequently the induced tidal deformation effect, is higher in the infrared.

Original language	English
Article number	A63
Number of pages	24
Journal	Astronomy & Astrophysics
Volume	685
Early online date	8 May 2024
DOIs	https://doi.org/10.1051/0004-6361/202348502
Publication status	Published - May 2024

Keywords

Planets and satellites: individual: WASP-12b
Planets and satellites: interiors

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https://arxiv.org/abs/2402.10486Licence: CC BY

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REVEAL: REVEALing Signatures of Habitable Worlds Hidden by Stellar Activity
Cameron, A. C. (PI)
UKRI (EU)
1/08/24 → 31/07/30
Project: Standard
AO2 - Professor Andrew Cameron: Project AO2 - Andrew Cameron
Cameron, A. C. (PI)
Science & Technology Facilities Council
1/04/21 → 31/03/24
Project: Standard

WASP-12b CHEOPS light curves
Akinsanmi, B. (Creator), Barros, S. C. C. (Creator), Lendl, M. (Creator), Carone, L. (Creator), Cubillos, P. E. (Creator), Bekkelien, A. (Creator), Fortier, A. (Creator), Floren, H.-G. (Creator), Collier Cameron, A. (Creator), Boue, G. (Creator), Bruno, G. (Creator), Demory, B.-O. (Creator), Brandeker, A. (Creator), Sousa, S. G. (Creator), Wilson, T. G. (Creator), Deline, A. (Creator), Bonfanti, A. (Creator), Scandariato, G. (Creator), Hooton, M. J. (Creator), Correia, A. C. M. (Creator), Demangeon, O. D. S. (Creator), Smith, A. M. S. (Creator), Singh, V. (Creator), Alibert, Y. (Creator), Alonso, R. (Creator), Asquier, J. (Creator), Barczy, T. (Creator), Barrado Navascues, D. (Creator), Baumjohann, W. (Creator), Beck, M. (Creator), Beck, T. (Creator), Benz, W. (Creator), Billot, N. (Creator), Bonfils, X. (Creator), Borsato, L. (Creator), Ch, B. (Creator), Buder, M. (Creator), Charnoz, S. (Creator), Sz, C. (Creator), Davies, M. B. (Creator), Deleuil, M. (Creator), Delrez, L. (Creator), Ehrenreich, D. (Creator), Erikson, A. (Creator), Farinato, J. (Creator), Fossati, L. (Creator), Fridlund, M. (Creator), Gandolfi, D. (Creator), Gillon, M. (Creator), Guedel, M. (Creator), Guenther, M. N. (Creator), Heitzmann, A. (Creator), Helling, C. (Creator), Hoyer, S. (Creator), Isaak, K. G. (Creator), Kiss, L. L. (Creator), K.W.F., L. (Creator), Laskar, J. (Creator), Lecavelier Des Etangs, A. (Creator), Magrin, D. (Creator), Maxted, P. F. L. (Creator), Mecina, M. (Creator), Ch, M. (Creator), Nascimbeni, V. (Creator), Olofsson, G. (Creator), Ottensamer, R. (Creator), Pagano, I. (Creator), Palle, E. (Creator), Peter, G. (Creator), Piazza, D. (Creator), Piotto, G. (Creator), Pollacco, D. (Creator), Queloz, D. (Creator), Ragazzoni, R. (Creator), Rando, N. (Creator), Rauer, H. (Creator), Ribas, I. (Creator), Santos, N. C. (Creator), Segransan, D. (Creator), Simon, A. E. (Creator), Stalport, M. (Creator), GyM., S. (Creator), Thomas, N. (Creator), Udry, S. (Creator), Van Grootel, V. (Creator), Venturini, J. (Creator), Villaver, E. (Creator) & Walton, N. A. (Creator), Centre de Donnees Strasbourg (CDS), 2024
DOI: 10.26093/cds/vizier.36850063
Dataset

Cite this

Akinsanmi, B., Barros, S. C. C., Lendl, M., Carone, L., Cubillos, P. E., Bekkelien, A., Fortier, A., Florén, H.-G., Collier Cameron, A., Boué, G., Bruno, G., Demory, B.-O., Brandeker, A., Sousa, S. G., Wilson, T. G., Deline, A., Bonfanti, A., Scandariato, G., Hooton, M. J., ... Walton, N. A. (2024). The tidal deformation and atmosphere of WASP-12b from its phase curve. Astronomy & Astrophysics, 685, Article A63. https://doi.org/10.1051/0004-6361/202348502

@article{ebf2d731811042beaeb732ee561b4cee,

title = "The tidal deformation and atmosphere of WASP-12b from its phase curve",

abstract = "Context. Ultra-hot Jupiters present a unique opportunity to understand the physics and chemistry of planets, their atmospheres, and interiors at extreme conditions. WASP-12 b stands out as an archetype of this class of exoplanets, with a close-in orbit around its star that results in intense stellar irradiation and tidal effects.Aims. The goals are to measure the planet{\textquoteright}s tidal deformation, atmospheric properties, and also to refine its orbital decay rate.Methods. We performed comprehensive analyses of the transits, occultations, and phase curves of WASP-12b by combining new CHEOPS observations with previous TESS and Spitzer data. The planet was modeled as a triaxial ellipsoid parameterized by the second-order fluid Love number of the planet, h2, which quantifies its radial deformation and provides insight into the interior structure.Results. We measured the tidal deformation of WASP-12b and estimated a Love number of h2 = 1.55−0.49+0.45 (at 3.2σ) from its phase curve. We measured occultation depths of 333 ± 24 ppm and 493 ± 29 ppm in the CHEOPS and TESS bands, respectively, while the nightside fluxes are consistent with zero, and also marginal eastward phase offsets. Our modeling of the dayside emission spectrum indicates that CHEOPS and TESS probe similar pressure levels in the atmosphere at a temperature of ~2900 K. We also estimated low geometric albedos of Ag = 0.086 ± 0.017 and Ag = 0.01 ± 0.023 in the CHEOPS and TESS passbands, respectively, suggesting the absence of reflective clouds in the high-temperature dayside of the planet. The CHEOPS occultations do not show strong evidence for variability in the dayside atmosphere of the planet at the median occultation depth precision of 120 ppm attained. Finally, combining the new CHEOPS timings with previous measurements refines the precision of the orbital decay rate by 12% to a value of −30.23 ± 0.82 ms yr−1, resulting in a modified stellar tidal quality factor of Q′★ = 1.70 ± 0.14 × 105.Conclusions. WASP-12 b becomes the second exoplanet, after WASP-103b, for which the Love number has been measured from the effect of tidal deformation in the light curve. However, constraining the core mass fraction of the planet requires measuring h2 with a higher precision. This can be achieved with high signal-to-noise observations with JWST since the phase curve amplitude, and consequently the induced tidal deformation effect, is higher in the infrared.",

keywords = "Planets and satellites: individual: WASP-12b, Planets and satellites: interiors",

author = "B. Akinsanmi and Barros, {S. C. C.} and M. Lendl and L. Carone and Cubillos, {P. E.} and A. Bekkelien and A. Fortier and H.-G. Flor{\'e}n and {Collier Cameron}, A. and G. Bou{\'e} and G. Bruno and B.-O. Demory and A. Brandeker and Sousa, {S. G.} and Wilson, {T. G.} and A. Deline and A. Bonfanti and G. Scandariato and Hooton, {M. J.} and Correia, {A. C. M.} and Demangeon, {O. D. S.} and Smith, {A. M. S.} and V. Singh and Y. Alibert and R. Alonso and J. Asquier and T. B{\'a}rczy and {Barrado Navascues}, D. and W. Baumjohann and M. Beck and T. Beck and W. Benz and N. Billot and X. Bonfils and L. Borsato and C. Broeg and M. Buder and S. Charnoz and Sz. Csizmadia and Davies, {M. B.} and M. Deleuil and L. Delrez and D. Ehrenreich and A. Erikson and J. Farinato and L. Fossati and M. Fridlund and D. Gandolfi and M. Gillon and M. G{\"u}del and G{\"u}nther, {M. N.} and A. Heitzmann and Ch. Helling and S. Hoyer and Isaak, {K. G.} and Kiss, {L. L.} and Lam, {K. W. F.} and J. Laskar and {Lecavelier des Etangs}, A. and D. Magrin and Maxted, {P. F. L.} and M. Mecina and C. Mordasini and V. Nascimbeni and G. Olofsson and R. Ottensamer and I. Pagano and E. Pall{\'e} and G. Peter and D. Piazza and G. Piotto and D. Pollacco and D. Queloz and R. Ragazzoni and N. Rando and H. Rauer and I. Ribas and Santos, {N. C.} and D. S{\'e}gransan and Simon, {A. E.} and M. Stalport and Szab{\'o}, {Gy. M.} and N. Thomas and S. Udry and {Van Grootel}, V. and J. Venturini and E. Villaver and Walton, {N. A.}",

note = "Funding: LCa and CHe acknowledge support from the European Union H2020-MSCA-ITN-2019 under Grant Agreement no. 860470 (CHAMELEON). ACCa and TWi acknowledge support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant number ST/R003203/1. PM acknowledges support from STFC research grant number ST/M001040/1. NAW acknowledges UKSA grant ST/R004838/1. ",

year = "2024",

month = may,

doi = "10.1051/0004-6361/202348502",

language = "English",

volume = "685",

journal = "Astronomy & Astrophysics",

issn = "0004-6361",

publisher = "EDP SCIENCES S A",

}

Akinsanmi, B, Barros, SCC, Lendl, M, Carone, L, Cubillos, PE, Bekkelien, A, Fortier, A, Florén, H-G, Collier Cameron, A, Boué, G, Bruno, G, Demory, B-O, Brandeker, A, Sousa, SG, Wilson, TG, Deline, A, Bonfanti, A, Scandariato, G, Hooton, MJ, Correia, ACM, Demangeon, ODS, Smith, AMS, Singh, V, Alibert, Y, Alonso, R, Asquier, J, Bárczy, T, Barrado Navascues, D, Baumjohann, W, Beck, M, Beck, T, Benz, W, Billot, N, Bonfils, X, Borsato, L, Broeg, C, Buder, M, Charnoz, S, Csizmadia, S, Davies, MB, Deleuil, M, Delrez, L, Ehrenreich, D, Erikson, A, Farinato, J, Fossati, L, Fridlund, M, Gandolfi, D, Gillon, M, Güdel, M, Günther, MN, Heitzmann, A, Helling, C, Hoyer, S, Isaak, KG, Kiss, LL, Lam, KWF, Laskar, J, Lecavelier des Etangs, A, Magrin, D, Maxted, PFL, Mecina, M, Mordasini, C, Nascimbeni, V, Olofsson, G, Ottensamer, R, Pagano, I, Pallé, E, Peter, G, Piazza, D, Piotto, G, Pollacco, D, Queloz, D, Ragazzoni, R, Rando, N, Rauer, H, Ribas, I, Santos, NC, Ségransan, D, Simon, AE, Stalport, M, Szabó, GM, Thomas, N, Udry, S, Van Grootel, V, Venturini, J, Villaver, E & Walton, NA 2024, 'The tidal deformation and atmosphere of WASP-12b from its phase curve', Astronomy & Astrophysics, vol. 685, A63. https://doi.org/10.1051/0004-6361/202348502

TY - JOUR

T1 - The tidal deformation and atmosphere of WASP-12b from its phase curve

AU - Akinsanmi, B.

AU - Barros, S. C. C.

AU - Lendl, M.

AU - Carone, L.

AU - Cubillos, P. E.

AU - Bekkelien, A.

AU - Fortier, A.

AU - Florén, H.-G.

AU - Collier Cameron, A.

AU - Boué, G.

AU - Bruno, G.

AU - Demory, B.-O.

AU - Brandeker, A.

AU - Sousa, S. G.

AU - Wilson, T. G.

AU - Deline, A.

AU - Bonfanti, A.

AU - Scandariato, G.

AU - Hooton, M. J.

AU - Correia, A. C. M.

AU - Demangeon, O. D. S.

AU - Smith, A. M. S.

AU - Singh, V.

AU - Alibert, Y.

AU - Alonso, R.

AU - Asquier, J.

AU - Bárczy, T.

AU - Barrado Navascues, D.

AU - Baumjohann, W.

AU - Beck, M.

AU - Beck, T.

AU - Benz, W.

AU - Billot, N.

AU - Bonfils, X.

AU - Borsato, L.

AU - Broeg, C.

AU - Buder, M.

AU - Charnoz, S.

AU - Csizmadia, Sz.

AU - Davies, M. B.

AU - Deleuil, M.

AU - Delrez, L.

AU - Ehrenreich, D.

AU - Erikson, A.

AU - Farinato, J.

AU - Fossati, L.

AU - Fridlund, M.

AU - Gandolfi, D.

AU - Gillon, M.

AU - Güdel, M.

AU - Günther, M. N.

AU - Heitzmann, A.

AU - Helling, Ch.

AU - Hoyer, S.

AU - Isaak, K. G.

AU - Kiss, L. L.

AU - Lam, K. W. F.

AU - Laskar, J.

AU - Lecavelier des Etangs, A.

AU - Magrin, D.

AU - Maxted, P. F. L.

AU - Mecina, M.

AU - Mordasini, C.

AU - Nascimbeni, V.

AU - Olofsson, G.

AU - Ottensamer, R.

AU - Pagano, I.

AU - Pallé, E.

AU - Peter, G.

AU - Piazza, D.

AU - Piotto, G.

AU - Pollacco, D.

AU - Queloz, D.

AU - Ragazzoni, R.

AU - Rando, N.

AU - Rauer, H.

AU - Ribas, I.

AU - Santos, N. C.

AU - Ségransan, D.

AU - Simon, A. E.

AU - Stalport, M.

AU - Szabó, Gy. M.

AU - Thomas, N.

AU - Udry, S.

AU - Van Grootel, V.

AU - Venturini, J.

AU - Villaver, E.

AU - Walton, N. A.

N1 - Funding: LCa and CHe acknowledge support from the European Union H2020-MSCA-ITN-2019 under Grant Agreement no. 860470 (CHAMELEON). ACCa and TWi acknowledge support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant number ST/R003203/1. PM acknowledges support from STFC research grant number ST/M001040/1. NAW acknowledges UKSA grant ST/R004838/1.

PY - 2024/5

Y1 - 2024/5

N2 - Context. Ultra-hot Jupiters present a unique opportunity to understand the physics and chemistry of planets, their atmospheres, and interiors at extreme conditions. WASP-12 b stands out as an archetype of this class of exoplanets, with a close-in orbit around its star that results in intense stellar irradiation and tidal effects.Aims. The goals are to measure the planet’s tidal deformation, atmospheric properties, and also to refine its orbital decay rate.Methods. We performed comprehensive analyses of the transits, occultations, and phase curves of WASP-12b by combining new CHEOPS observations with previous TESS and Spitzer data. The planet was modeled as a triaxial ellipsoid parameterized by the second-order fluid Love number of the planet, h2, which quantifies its radial deformation and provides insight into the interior structure.Results. We measured the tidal deformation of WASP-12b and estimated a Love number of h2 = 1.55−0.49+0.45 (at 3.2σ) from its phase curve. We measured occultation depths of 333 ± 24 ppm and 493 ± 29 ppm in the CHEOPS and TESS bands, respectively, while the nightside fluxes are consistent with zero, and also marginal eastward phase offsets. Our modeling of the dayside emission spectrum indicates that CHEOPS and TESS probe similar pressure levels in the atmosphere at a temperature of ~2900 K. We also estimated low geometric albedos of Ag = 0.086 ± 0.017 and Ag = 0.01 ± 0.023 in the CHEOPS and TESS passbands, respectively, suggesting the absence of reflective clouds in the high-temperature dayside of the planet. The CHEOPS occultations do not show strong evidence for variability in the dayside atmosphere of the planet at the median occultation depth precision of 120 ppm attained. Finally, combining the new CHEOPS timings with previous measurements refines the precision of the orbital decay rate by 12% to a value of −30.23 ± 0.82 ms yr−1, resulting in a modified stellar tidal quality factor of Q′★ = 1.70 ± 0.14 × 105.Conclusions. WASP-12 b becomes the second exoplanet, after WASP-103b, for which the Love number has been measured from the effect of tidal deformation in the light curve. However, constraining the core mass fraction of the planet requires measuring h2 with a higher precision. This can be achieved with high signal-to-noise observations with JWST since the phase curve amplitude, and consequently the induced tidal deformation effect, is higher in the infrared.

AB - Context. Ultra-hot Jupiters present a unique opportunity to understand the physics and chemistry of planets, their atmospheres, and interiors at extreme conditions. WASP-12 b stands out as an archetype of this class of exoplanets, with a close-in orbit around its star that results in intense stellar irradiation and tidal effects.Aims. The goals are to measure the planet’s tidal deformation, atmospheric properties, and also to refine its orbital decay rate.Methods. We performed comprehensive analyses of the transits, occultations, and phase curves of WASP-12b by combining new CHEOPS observations with previous TESS and Spitzer data. The planet was modeled as a triaxial ellipsoid parameterized by the second-order fluid Love number of the planet, h2, which quantifies its radial deformation and provides insight into the interior structure.Results. We measured the tidal deformation of WASP-12b and estimated a Love number of h2 = 1.55−0.49+0.45 (at 3.2σ) from its phase curve. We measured occultation depths of 333 ± 24 ppm and 493 ± 29 ppm in the CHEOPS and TESS bands, respectively, while the nightside fluxes are consistent with zero, and also marginal eastward phase offsets. Our modeling of the dayside emission spectrum indicates that CHEOPS and TESS probe similar pressure levels in the atmosphere at a temperature of ~2900 K. We also estimated low geometric albedos of Ag = 0.086 ± 0.017 and Ag = 0.01 ± 0.023 in the CHEOPS and TESS passbands, respectively, suggesting the absence of reflective clouds in the high-temperature dayside of the planet. The CHEOPS occultations do not show strong evidence for variability in the dayside atmosphere of the planet at the median occultation depth precision of 120 ppm attained. Finally, combining the new CHEOPS timings with previous measurements refines the precision of the orbital decay rate by 12% to a value of −30.23 ± 0.82 ms yr−1, resulting in a modified stellar tidal quality factor of Q′★ = 1.70 ± 0.14 × 105.Conclusions. WASP-12 b becomes the second exoplanet, after WASP-103b, for which the Love number has been measured from the effect of tidal deformation in the light curve. However, constraining the core mass fraction of the planet requires measuring h2 with a higher precision. This can be achieved with high signal-to-noise observations with JWST since the phase curve amplitude, and consequently the induced tidal deformation effect, is higher in the infrared.

KW - Planets and satellites: individual: WASP-12b

KW - Planets and satellites: interiors

U2 - 10.1051/0004-6361/202348502

DO - 10.1051/0004-6361/202348502

M3 - Article

SN - 0004-6361

VL - 685

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

M1 - A63

ER -

The tidal deformation and atmosphere of WASP-12b from its phase curve

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REVEAL: REVEALing Signatures of Habitable Worlds Hidden by Stellar Activity

AO2 - Professor Andrew Cameron: Project AO2 - Andrew Cameron

Datasets

WASP-12b CHEOPS light curves

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