Investigation of White Light Jets Using Mauna Loa’s K-coronograph

Coronal jets are small eruptions characterized by a narrow spire and a luminous loop base. Extensive studies using EUV and X-ray observations have significantly advanced an understanding of their formation. However, questions regarding their heating and acceleration remain. Previous Yohkoh-era white-light observations revealed that certain coronal hole jets can extend more than 5 solar radii into the heliosphere, while most terminate in the lower corona. These observations, along with subsequent ones, suggest that extended coronal hole jets could contribute to the mass in the solar wind and potentially trigger the formation of polar plumes. However, it is important to note that most coronal hole jets do not extend into the outer corona, implying the presence of additional acceleration mechanisms for extended jets. In this study, we investigate the properties of several white light jets using observations from the K-coronograph and the Atmospheric Imaging Array of the Solar Dynamics Observatory.