Application of Three-dimensional, Time Dependent Modeling to a Survey of X-ray Bright Points C.C. Kankelborg, D.W. Longcope, and A.A. Pevtsov Montana State University We propose to study the time evolution of soft X-ray bright points (XBP) by merging complementary datasets from MDI, TRACE and EIT. By analyzing observations of the magnetic field and of the coronal and chromospheric emissions at high spatial and temporal resolution, we will determine the quantitative and morphological details of the heating process in these smallest coronal phenomena. We will test the hypothesis that this heating results from magnetic reconnection by developing a three-dimensional, time dependent, general model for the release of energy by magnetic reconnection in small-scale cancelling flux regions. Comparison of this new and sophisticated model to the unique data set anticipated from coordinated observations by TRACE and SOHO will enable us to determine whether and how much of the heating in coronal bright points can be attributed to magnetic reconnection. Plan of activities: We will use data from MDI, TRACE and EIT to infer heating rates, measure the frequency and luminosity of episodic events, and attempt to determine the degree to which XBPs are heated either continuously or episodically. We anticipate that the processes of heat deposition, conduction to the footpoints, and chromospheric evaporation can be characterized as to their temporal variation with data from TRACE, MDI and EIT. Existing observing sequences are sufficient for these purposes. A new, time-dependent model of XBP heating will be developed, based on an existing topological reconnection model. Prior to this work, XBP have been viewed predominantly as a single loop with a heating rate that is either steady or varying in time. If separator theory is correct, what appears to be a single loop evolving in time is in fact a succession of loops being heated and then cooling and disappearing. Depending on the rate of reconnection, several distinct loops may contribute simultaneously to the light curve of the XBP. Based on magnetic data alone, the model will predict the frequency and intensity of heating events, as well as observable characteristics of loop morphology evolving over time. Direct comparisons will be made with observed morphological evolution and multiwavelength light curves of XBPs. Relevance to NASA's Space Sciences programs: The proposed research uses data uniquely available from SOHO and TRACE to investigate coronal heating on small scales. The proposed observations combined with the theoretical interpretations, directly address several science themes posed in the Sun-Earth Connection Roadmap: * How is magnetic energy stored and released in the solar atmosphere? * What is the three dimensional structure of coronal magnetic fields? * How is the magnetic structure of the corona related to its thermal and dynamical evolution? Education/Public outreach: The results of an XBP study, by themselves, would not be a suitable topic for public outreach. We plan to prepare a public lecture presenting the general flavor of present space-based solar astronomy. This lecture will mention X-ray bright points as a single representative from the "zoo" of solar phenomena which are the subject of ongoing research. We will present the lecture in two or three Montana communities in collaboration with local amateur astronomy clubs.