Observability of evaporating lava worlds

Zilinskas, Mantas; Buchem, C.P.A. van; Miguel, Yamila; Louca, Amy; Lupu, Roxana; Zieba, Sebastian; Westrenen, W. van

doi:10.1051/0004-6361/202142984

Cited by 36 publications

(43 citation statements)

References 69 publications

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“…Due to 55 Cnc e's close proximity to its host star, silicate species present in a dayside magma ocean evaporate into the atmosphere. Lava planets with silicate atmospheres are prone to temperature inversions due to UV absorption by SiO vapor (Ito et al 2015;Zilinskas et al 2022). In particular, for a stellar brightness temperature of 5172 K, the expected dayside brightness temperature at 4.5 μm is ∼3100 K due to an SiO band, which is consistent with our results.…”

Section: Interpretation Of Resultssupporting

confidence: 91%

“…We hypothesize that 55 Cnc e either has a global atmosphere covering both hemispheres of the planet (Hammond & Pierrehumbert 2017) or a local dayside atmosphere (Castan & Menou 2011;Léger et al 2011;Kite et al 2016;Zilinskas et al 2022). In either case, the short radiative timescale on 55 Cnc e ensures there is minimal heat transport, which explains the negligible phase offset and nightside flux.…”

Section: Interpretation Of Resultsmentioning

confidence: 99%

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Revisiting the Iconic Spitzer Phase Curve of 55 Cancri e: Hotter Dayside, Cooler Nightside, and Smaller Phase Offset

Mercier

Dang

Cowan

et al. 2022

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Thermal phase curves of short-period exoplanets provide the best constraints on the atmospheric dynamics and heat transport in their atmospheres. The published Spitzer Space Telescope phase curve of 55 Cancri e, an ultra-short-period super-Earth, exhibits a large phase offset suggesting significant eastward heat recirculation, unexpected on such a hot planet. We present our rereduction and analysis of these iconic observations using the open source and modular Spitzer Phase Curve Analysis pipeline. In particular, we attempt to reproduce the published analysis using the same instrument detrending scheme as the original authors. We retrieve the dayside temperature ( T day = 3771 − 520 + 669 K), nightside temperature ( T night < 1649 K at 2σ), and longitudinal offset of the planet's hot spot, and quantify how they depend on the reduction and detrending. Our reanalysis suggests that 55 Cancri e has a negligible hot spot offset of − 12 − 18 + 21 degrees east. The small phase offset and cool nightside are consistent with the poor heat transport expected on ultra-short-period planets. The high dayside 4.5 μm brightness temperature is qualitatively consistent with SiO emission from an inverted rock vapor atmosphere.

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Section: Interpretation Of Resultssupporting

confidence: 91%

Section: Interpretation Of Resultsmentioning

confidence: 99%

Revisiting the Iconic Spitzer Phase Curve of 55 Cancri e: Hotter Dayside, Cooler Nightside, and Smaller Phase Offset

Mercier

Dang

Cowan

et al. 2022

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“…Two different JWST programmes will observe 55 Cnc e's occultations in the infrared during cycle 1, using the NIRCam (PID 2084, PI A. Brandeker) and MIRI (PID 1952, PI. R. Hu) instruments, which will undoubtedly help us understand better (Zilinskas et al 2022) the nature of this iconic super-Earth.…”

Section: Discussionmentioning

confidence: 99%

55 Cancri e’s occultation captured with CHEOPS

Demory¹,

Sulis²,

Valdes³

et al. 2023

A&A

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Past occultation and phase-curve observations of the ultra-short period super-Earth 55 Cnc e obtained at visible and infrared wavelengths have been challenging to reconcile with a planetary reflection and emission model. In this study, we analyse a set of 41 occultations obtained over a two-year timespan with the CHEOPS satellite. We report the detection of 55 Cnc e's occultation with an average depth of 12 ± 3 ppm. We derive a corresponding 2-σ upper limit on the geometric albedo of A g < 0.55 once decontaminated from the thermal emission measured by Spitzer at 4.5µm. CHEOPS's photometric performance enables, for the first time, the detection of individual occultations of this super-Earth in the visible and identifies short-timescale photometric corrugations likely induced by stellar granulation. We also find a clear 47.3-day sinusoidal pattern in the time-dependent occultation depths that we are unable to relate to stellar noise, nor instrumental systematics, but whose planetary origin could be tested with upcoming JWST occultation observations of this iconic super-Earth.

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“…Our choice of komatiite is based on early Earth (Miguel et al 2011). Different melt compositions or evaporated atmospheres may result in chemistry and thermal structure changes (Zilinskas et al 2022).…”

Section: Pseudo-2d Rock Vapor Modelmentioning

confidence: 99%

K2 and Spitzer phase curves of the rocky ultra-short-period planet K2-141 b hint at a tenuous rock vapor atmosphere

Zieba

Zilinskas

Kreidberg

et al. 2022

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K2-141 b is a transiting, small (1.5 R⊕) ultra-short-period (USP) planet discovered by the Kepler space telescope orbiting a K-dwarf host star every 6.7 h. The planet's high surface temperature of more than 2000 K makes it an excellent target for thermal emission observations. Here we present 65 h of continuous photometric observations of K2-141 b collected with Spitzer's Infrared Array Camera (IRAC) Channel 2 at 4.5 μm spanning ten full orbits of the planet. We measured an infrared eclipse depth of ${f_{{{\rm{p}} \mathord{\left/ {\vphantom {{\rm{p}} {{{\rm{f}}_{\rm{*}}}}}} \right. \kern-\nulldelimiterspace} {{{\rm{f}}_{\rm{*}}}}}}} = 142.9_{ - 39.0}^{38.5}$ ppm and a peak to trough amplitude variation of $A = 120.6_{ - 43.0}^{42.3}$ ppm. The best fit model to the Spitzer data shows no significant thermal hotspot offset, in contrast to the previously observed offset for the well-studied USP planet 55 Cnc e. We also jointly analyzed the new Spitzer observations with the photometry collected by Kepler during two separate K2 campaigns. We modeled the planetary emission with a range of toy models that include a reflective and a thermal contribution. With a two-temperature model, we measured a dayside temperature of ${T_{{\rm{p,d}}}} = 2049_{ - 359}^{362}$ K and a night-side temperature that is consistent with zero (Tp,n < 1712 K at 2σ). Models with a steep dayside temperature gradient provide a better fit to the data than a uniform dayside temperature (ΔBIC = 22.2). We also found evidence for a nonzero geometric albedo ${A_{\rm{g}}} = 0.282_{ - 0.078}^{0.070}$. We also compared the data to a physically motivated, pseudo-2D rock vapor model and a 1D turbulent boundary layer model. Both models fit the data well. Notably, we found that the optical eclipse depth can be explained by thermal emission from a hot inversion layer, rather than reflected light. A thermal inversion may also be responsible for the deep optical eclipse observed for another USP, Kepler-10 b. Finally, we significantly improved the ephemerides for K2-141 b and c, which will facilitate further follow-up observations of this interesting system with state-of-the-art observatories such as James Webb Space Telescope.

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Observability of evaporating lava worlds

Cited by 36 publications

References 69 publications

Revisiting the Iconic Spitzer Phase Curve of 55 Cancri e: Hotter Dayside, Cooler Nightside, and Smaller Phase Offset

Revisiting the Iconic Spitzer Phase Curve of 55 Cancri e: Hotter Dayside, Cooler Nightside, and Smaller Phase Offset

55 Cancri e’s occultation captured with CHEOPS

K2 and Spitzer phase curves of the rocky ultra-short-period planet K2-141 b hint at a tenuous rock vapor atmosphere

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