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JWST reveals a rapid and strong day side variability of 55 Cancri e

Authors :
Patel, J. A.
Brandeker, A.
Kitzmann, D.
de la Roche, D. J. M. Petit dit
Bello-Arufe, A.
Heng, K.
Valdés, E. Meier
Persson, C. M.
Zhang, M.
Demory, B. -O.
Bourrier, V.
Deline, A.
Ehrenreich, D.
Fridlund, M.
Hu, R.
Lendl, M.
Oza, A. V.
Alibert, Y.
Hooton, M. J.
Source :
A&A 690, A159 (2024)
Publication Year :
2024

Abstract

The nature of the close-in rocky planet 55 Cnc e is puzzling despite having been observed extensively. Its optical and infrared occultation depths show temporal variability, in addition to a phase curve variability observed in the optical. We wish to explore the possibility that the variability originates from the planet being in a 3:2 spin-orbit resonance, thus showing different sides during occultations. We proposed and were awarded Cycle 1 time at the James Webb Space Telescope (JWST) to test this hypothesis. JWST/NIRCam observed five occultations (secondary eclipses), of which four were observed within a week, of the planet simultaneously at 2.1 and 4.5 {\mu}m. While the former gives band-integrated photometry, the latter provides a spectrum between 3.9-5.0 {\mu}m. We find that the occultation depths in both bandpasses are highly variable and change between a non-detection (-5 +/- 6 ppm and 7 +/- 9 ppm) to 96 +/- 8 ppm and 119 (+34) (-19) ppm at 2.1 {\mu}m and 4.5 {\mu}m, respectively. Interestingly, the variations in both bandpasses are not correlated and do not support the 3:2 spin-orbit resonance explanation. The measured brightness temperature at 4.5 {\mu}m varies between 873-2256 K and is lower than the expected dayside temperature of bare rock with no heat re-distribution (2500 K) which is indicative of an atmosphere. Our atmospheric retrieval analysis of occultation depth spectra at 4.5 {\mu}m finds that different visits statistically favour various atmospheric scenarios including a thin outgassed CO/CO2 atmosphere and a silicate rock vapour atmosphere. Some visits even support a flat line model. The observed variability could be explained by stochastic outgassing of CO/CO2, which is also hinted by retrievals. Alternatively, the variability, observed at both 2.1 and 4.5 {\mu}m, could be the result of a circumstellar patchy dust torus generated by volcanism on the planet.<br />Comment: 32 pages, 10 + 15 figures, 3+2 tables, accepted for publication in A&A

Details

Database :
arXiv
Journal :
A&A 690, A159 (2024)
Publication Type :
Report
Accession number :
edsarx.2407.12898
Document Type :
Working Paper
Full Text :
https://doi.org/10.1051/0004-6361/202450748