Presentation #103.02 in the session The Corona and Solar Wind Speed.
Coronal holes are areas on the solar disk with decreased intensity in EUV and X-Ray images. They are considered to be the sources of solar wind high speed streams as they have open magnetic field lines that reach out into the heliosphere. Coronal hole boundaries form the transition from open magnetic field to closed field which are field lines that bend back to the surface near the sun.In this presentation we show the results of 15 automated coronal hole detection algorithms applied to a set of SDO/AIA EUV images and magnetograms. The variation of the location of the boundary can be considerable and we discuss how this affects the physical properties of the coronal holes and the implication of these variations for solar wind modelling.