The dark colors of Jupiter's North Equatorial Belt (NEB, 7–17°N) appeared to expand northward into the neighboring zone in 2015, consistent with a 3–5 year cycle. Inversions of thermal‐IR imaging from the Very Large Telescope revealed a moderate warming and reduction of aerosol opacity at the cloud tops at 17–20°N, suggesting subsidence and drying in the expanded sector. Two new thermal waves were identified during this period: (i) an upper tropospheric thermal wave (wave number 16–17, amplitude 2.5 K at 170 mbar) in the mid‐NEB that was anticorrelated with haze reflectivity; and (ii) a stratospheric wave (wave number 13–14, amplitude 7.3 K at 5 mbar) at 20–30°N. Both were quasi‐stationary, confined to regions of eastward zonal flow, and are morphologically similar to waves observed during previous expansion events.

Rotational modulations are observed on brown dwarfs and directly imaged exoplanets, but the underlying mechanism is not well understood. Here, we analyze Jupiter's rotational light curves at 12 wavelengths from the ultraviolet (UV) to the mid-infrared (mid-IR). Peak-to-peak amplitudes of Jupiter's light curves range from sub percent to 4% at most wavelengths, but the amplitude exceeds 20% at 5 µm, a wavelength sensing Jupiter's deep troposphere. Jupiter's rotational modulations are primarily caused by discrete patterns in the cloudless belts instead of the cloudy zones. The lightcurve amplitude is dominated by the sizes and brightness contrasts of the Great Red Spot (GRS), expansions of the North Equatorial Belt (NEB), patchy clouds in the North Temperate Belt (NTB) and a train of hot spots in the NEB. In reflection, the contrast is controlled by upper tropospheric and stratospheric hazes, clouds, and chromophores in the clouds. In thermal emission, the small rotational variability is caused by the spatial distribution of temperature and opacities of gas and aerosols; the large variation is caused by the NH 3 cloud holes and thin-thick clouds. The methaneband light curves exhibit opposite-shape behavior compared with the UV and visible wavelengths, caused by wavelength-dependent brightness change of the GRS. Light-curve evolution is induced by periodic events in the belts and longitudinal drifting of the GRS and patchy clouds in the NTB. This study suggests several interesting mechanisms related to distributions of temperature, gas, hazes, and clouds for understanding the observed rotational modulations on brown dwarfs and exoplanets.

Enhanced mid-infrared emission from CH 4 and other stratospheric hydrocarbons have been observed coincident with Jupiter's ultraviolet auroral emission 1-3 , which demonstrates that auroral processes and the neutral stratosphere of Jupiter are coupled. However, the exact nature of this coupling has remained an open question. Here, we present a time series of Subaru-COMICS images of Jupiter at 7.80 µm measured between January 11-14th, February 4-5th and May 17-20th (UT) 2017, which show both the morphology and magnitude of the auroral CH 4 emission to vary on daily timescales in relation to external solar-wind conditions. The southern auroral CH 4 emission increased in brightness temperature (T b) by ∆T b = 3.8 ± 0.9 K between January 11th 15:50 UT-12th 12:57 UT during a predicted solarwind compression. During the same compression, the northern auroral emission exhibited a dusk-side brightening, which mimicks the morphology observed in the ultraviolet auroral emission during periods of enhanced solar-wind pressures 4, 5. These results suggest that changes in external solar wind conditions perturb the jovian magnetosphere such that ener

To report a rare case of a patient with two recurrent episodes of Multiple Evanescent White Dot Syndrome (MEWDS) associated with the second dose and second booster of the mRNA-1273 COVID-19 vaccine (Moderna), and to perform a literature review on COVID-19-vaccine-associated MEWDS. Case Report: A 31-year-old female was evaluated for a temporal scotoma and photopsias that started two weeks after the second dose of the Moderna COVID-19 vaccine. Dilated fundus findings were remarkable for unilateral, small whitish-yellow dots scattered around posterior pole of the left eye, consistent with a diagnosis of MEWDS. The symptoms resolved three months later without treatment. Approximately one year after the first vaccine, the patient received the second Moderna COVID-19 vaccine booster and experienced a recurrence of symptoms with an enlarged scotoma and similar examination findings. The patient was treated with a course of systemic corticosteroids with subsequent clinical improvement. Conclusion: Although uveitis following COVID-19 vaccines is rare, our case highlights a need for increased awareness amongst practitioners regarding COVID-19-vaccine-associated onset or recurrence of ocular inflammatory diseases.