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Context. The Sun's complex corona is the source of the solar wind andinterplanetary magnetic field. While the large scale morphology is wellunderstood, the impact of variations in coronal properties on the scale of afew degrees on properties of the interplanetary medium is not known. SolarOrbiter, carrying both remote sensing and in situ instruments into the innersolar system, is intended to make these connections better than ever before.Aims. We combine remote sensing and in situ measurements from Solar Orbiter'sfirst perihelion at 0.5 AU to study the fine scale structure of the solar windfrom the equatorward edge of a polar coronal hole with the aim of identifyingcharacteristics of the corona which can explain the in situ variations.Methods. We use in situ measurements of the magnetic field, density and solarwind speed to identify structures on scales of hours at the spacecraft. UsingPotential Field Source Surface mapping we estimate the source locations of themeasured solar wind as a function of time and use EUI images to characterisethese solar sources. Results. We identify small scale stream interactions inthe solar wind with compressed magnetic field and density along with speedvariations which are associated with corrugations in the edge of the coronalhole on scales of several degrees, demonstrating that fine scale coronalstructure can directly influence solar wind properties and drive variationswithin individual streams. Conclusions. This early analysis alreadydemonstrates the power of Solar Orbiter's combined remote sensing and in situpayload and shows that with future, closer perihelia it will be possibledramatically to improve our knowledge of the coronal sources of fine scalesolar wind structure, which is important both for understanding the phenomenadriving the solar wind and predicting its impacts at the Earth and elsewhere.

Signatures of coronal hole substructure in the solar wind: combined Solar Orbiter remote sensing and in situ measurements