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Constrain how rapidly planets assemble in different environments and identify observations that distinguish competing formation pathways.
Explain the observed diversity of planetary masses and orbits and infer how common Solar-System-like architectures are after accounting for observational selection.
Determine which formation history accounts for the equatorial mountain ridge on Iapetus, discriminating internal evolution from deposited orbiting material.
Explain how the solar dynamo enters and recovers from prolonged low-activity intervals such as the Maunder Minimum.
Identify and quantify the processes that maintain the solar corona at temperatures far above the photosphere, and test their relative contributions against observations.