2025A&A...693A.128S

Query : 2025A&A...693A.128S

2025A&A...693A.128S - Astronomy and Astrophysics, volume 693A128 (2025/1-1)

CHEOPS observations confirm nodal precession in the WASP-33 system.

SMITH A.M.S., CSIZMADIA S., VAN GROOTEL V., LENDL M., PERSSON C.M., OLOFSSON G., EHRENREICH D., GUNTHER M.N., HEITZMANN A., BARROS S.C.C., BONFANTI A., BRANDEKER A., CABRERA J., DEMANGEON O.D.S., FOSSATI L., HARRE J.-V., HOOTON M.J., HOYER S., KALMAN S., SALMON S., SOUSA S.G., SZABO G.M., WILSON T.G., ALIBERT Y., ALONSO R., ASQUIER J., BARCZY T., BARRADO D., BAUMJOHANN W., BENZ W., BILLOT N., BORSATO L., BROEG C., COLLIER CAMERON A., CORREIA A.C.M., CUBILLOS P.E., DAVIES M.B., DELEUIL M., DELINE A., DEMORY B.-O., DEREKAS A., EDWARDS B., EGGER J.A., ERIKSON A., FORTIER A., FRIDLUND M., GANDOLFI D., GAZEAS K., GILLON M., GUDEL M., HASIBA J., HELLING C., ISAAK K.G., KISS L.L., KORTH J., LAM K.W.F., LASKAR J., LECAVELIER DES ETANGS A., MAGRIN D., MAXTED P.F.L., MERIN B., MORDASINI C., NASCIMBENI V., OTTENSAMER R., PAGANO I., PALLE E., PETER G., PIAZZA D., PIOTTO G., POLLACCO D., QUELOZ D., RAGAZZONI R., RANDO N., RAUER H., RIBAS I., SANTOS N.C., SCANDARIATO G., SEGRANSAN D., SIMON A.E., STALPORT M., SULIS S., UDRY S., ULMER-MOLL S., VENTURINI J., VILLAVER E., VIOTTO V., WALTER I., WALTON N.A. and WOLF S.

Abstract (from CDS):

Aims. We aim to observe the transits and occultations of WASP-33 b, which orbits a rapidly rotating δ Scuti pulsator, with the goal of measuring the orbital obliquity via the gravity-darkening effect, and constraining the geometric albedo via the occultation depth.
Methods. We observed four transits and four occultations with CHEOPS, and employ a variety of techniques to remove the effects of the stellar pulsations from the light curves, as well as the usual CHEOPS systematic effects. We also performed a comprehensive analysis of low-resolution spectral and Gaia data to re-determine the stellar properties of WASP-33.
Results. We measure an orbital obliquity 111.3–0.7+0.2 degrees, which is consistent with previous measurements made via Doppler tomography. We also measure the planetary impact parameter, and confirm that this parameter is undergoing rapid secular evolution as a result of nodal precession of the planetary orbit. This precession allows us to determine the second-order fluid Love number of the star, which we find agrees well with the predictions of theoretical stellar models. We are unable to robustly measure a unique value of the occultation depth, and emphasise the need for long-baseline observations to better measure the pulsation periods.

Abstract Copyright: © The Authors 2025

Journal keyword(s): planets and satellites: dynamical evolution and stability - planets and satellites: fundamental parameters - planets and satellites: gaseous planets - planets and satellites: individual: WASP-33 b - stars: oscillations - stars: individual: WASP-33

VizieR on-line data: <Available at CDS (J/A+A/693/A128): w33_drp.dat w33_pipe.dat detrend.dat>

Simbad objects: 12

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Number of rows : 12
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 HD 15082b Pl 02 26 51.0582618096 +37 33 01.736482032           ~ 403 1
2 HD 15082 EB* 02 26 51.0582618096 +37 33 01.736482032   8.41 8.14     kA5hA8mF4 229 1
3 HD 31221b Pl? 04 54 49.3851496008 +22 08 47.363855892           ~ 4 0
4 HD 133112b Pl 15 02 44.8678907928 -03 01 52.986571896           ~ 144 0
5 BD+46 2629 ** 19 07 53.104944 +46 52 06.00420   10.12 9.70 9.80   kA2hA5mA7(IV)m: 173 0
6 BD+46 2629A * 19 07 53.1397066992 +46 52 05.922122844           ~ 48 1
7 HD 185603 * 19 38 38.7352230144 +31 13 09.217127532   7.67 7.58     A0 80 0
8 HD 185603b Pl 19 38 38.7352230144 +31 13 09.217127532           ~ 184 0
9 HD 195689b Pl 20 31 26.3534153736 +39 56 19.773037500           ~ 358 0
10 HD 201585b Pl 21 10 12.3723073896 +10 44 19.949472816           ~ 83 0
11 HD 201585 * 21 10 12.3723073896 +10 44 19.949472816   8.51 8.27     A8 53 0
12 BD+66 1610b Pl 23 29 04.2251836392 +67 02 05.378578800           ~ 27 0

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