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Session 33 - Dynamics of Solar Magnetic Fields.
Oral session, Tuesday, June 11
Wisconsin Center,
Using best data sets of BBSO magnetograph and H\alpha observations on the quiet Sun, we carefully studied the properties and flow patterns of network and intranetwork magnetic fields and associated chromospheric jets. We have obtained the following results: (a) We studied the data for a quiet region with area of 300"\times235", more than 2500 intranetwork elements and 500 network elements are identified. Magnetic flux is measured for each magnetic element from the magnetogram taken at the best seeing. The flux of intranetwork elements falls in the range from the detection limit, 10^16 Mx, to approximate 2\times 10^18 Mx. The peak distribution locates at the flux of (6 - 8)\times 10 ^16 Mx. Using the local correlation tracking techniques, we derived the horizontal velocity fields of intranet and network magnetic fields. They consist of two components: (a) the radial divergence flows which move intranetwork fields from the network interior to the boundaries, and (b) the lateral flows which move along the network boundaries and converge toward stronger magnetic elements. Based on the number densities and flow velocities of IN fields derived, we estimate that the lower limit of total energy released from the recycling of intranetwork fields is 1.2\times 10^28 ergs/s, which is comparable to the energy required for coronal heatings. (3) Although we can not establish the correlation between spicules and magnetic dipoles, strong correlation between H\alpha-1.0Åjets and magnetic dipoles has been found. This correlation reveals reconnection nature of the jets. Based on the count rates of these jets, they may play an important role in the generation of solar wind and coronal heating.
