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Solar eclipses on Uranus occur when any of thenatural satellites of Uranus passes in front of theSun as seen fromUranus.Eclipses can occur only near a solar ring plane-crossing of Uranus (equinox), occurring approximately every 42 years, with the last crossing being in 2007/2008.^[1]

For bodies that appear smaller inangular diameter than the Sun, the proper term would be atransit and bodies that are larger than the apparent size of the Sun, the proper term would be anoccultation.

Twelve satellites of Uranus—Cressida,Desdemona,Juliet,Portia,Rosalind,Belinda,Puck,Miranda,Ariel,Umbriel,Titania andOberon—are large enough and near enough to eclipse the Sun.

All other satellites of Uranus are too small or too distant to produce anumbra.

At its distance from the Sun, the Sun's angular diameter is reduced to a tiny disk about 2 arcminutes across. The angular diameters of the moons large enough to fully eclipse the sun are: Cressida, 6–8'; Desdemona, 6–7'; Juliet, 10–12'; Portia, 9–13'; Rosalind, 4–5'; Belinda, 6–8'; Puck, 6–8'; Miranda, 10–15'; Ariel, 20–23'; Umbriel, 15–17'; Titania, 11–13'; Oberon, 8–9'.

• Brufau, Rainer. (2021). Triple shadow phenomena on Jupiter, Saturn and Uranus from 1000 CE to 3000 CE (Version 0) [Data set]. Zenodo.https://doi.org/10.5281/zenodo.5515898

• Solar eclipses by planet
• Uranus

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