Observational Constraints on the Origin and Acceleration of Solar Wind from Coronal Holes

UNDERSTANDING THE SOLAR WIND REQUIRES DETERMINING THE SOURCE REGIONS FOR DIFFERENT TYPES OF SOLAR WIND AND THE PHYSICAL PROCESSES THAT ACCELERATE THEM. WE PROPOSE TO INVESTIGATE THE SOLAR WIND FROM WITHIN AND NEAR CORONAL HOLES (CHS). THESE OPEN FIELD REGIONS ARE THE SOURCE OF FAST SOLAR WIND. THEIR BOUNDARIES ARE THOUGHT TO BE A SOURCE SLOW SOLAR WIND. THEORIES PROPOSE THAT AT CH BOUNDARIES RECONNECTION OCCURS BETWEEN OPEN AND CLOSED MAGNETIC FIELD RELEASING STORED PLASMA ONTO OPEN FIELD LINES TO FORM THE SLOW SOLAR WIND. MANY CHARACTERISTICS OF THIS INTERCHANGE RECONNECTION PROCESS ARE UNKNOWN.