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Coronal holes are seen as dark areas on the surface of the Sun in emission from the million-degree corona due to their lower electron temperature and density compared to the surrounding quiet Sun or active regions. They are the source regions of open magnetic field lines and thus the solar wind. It is recognized that fast-speed solar wind emanates from the center of large coronal holes,and the coronal hole boundary plays a crucial role in the formation of the slow-speed solar wind. Identifying and defining the coronal hole boundary is an important task for many areas of solar, heliospheric and space weather research, such as solar wind formation, heliospheric open fieldproblems and solar wind modeling and forecasting.
In the first part of this talk we present an assessment of coronal hole boundary locations from an assembly of coronal hole detection methods. In the second part of this talk we present a case study on two low-latitude coronal holes with their coronal emission and underlying photosphere magnetic field in a quest to search for the slow solar wind source region at the coronal hole boundaries.