Preliminary Study of Upper Transition Region Network Reconnection Events

Details Preliminary Study of Upper Transition Region Network Reconnection Events Preliminary Study of Upper Transition Region Network Reconnection Events

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spd....37.2505o&link_type=abstract

American Astronomical Society, SPD meeting #37, #25.05; Bulletin of the American Astronomical Society, Vol. 38, p.252

Physics

Scientific paper

We have conducted a preliminary study of network reconnection events that generate bright points in the Sun's upper transition region, which we have dubbed "upper transition region bright points", or UBPs. Using archived EIT and SUMER data covering the transition region and corona we measured the surface densities, sizes, radiative output, and magnetic structure of UBPs at each of two temperatures (Te 0.20 MK and Te 0.63 MK) in the quiet sun and in a coronal hole. Surface densities ranged from 5.07 ± 0.12 × 10-4 Mm-2 to 1.92 ± 0.50 × 10-3 Mm-2. The mean UBP size ranged from 9.36 ± 2.81 Mm to 12.21 ± 3.66 Mm. The mean irradiance measurements ranged from 5.50 ± 0.72 × 103 ergs cm-2 s-1 to 5.96 ± 0.78 ×10-4 ergs cm-2 s-1. We further determined the total UBP contribution to upper TR quiet sun and coronal hole emission at each temperature and the magnitudes of the average magnetic flux elements underlying the UBPs. Comparison to the theoretical model of Longcope & Kankelborg (1999), which applies the physics of randomly moving photospheric magnetic flux elements that collide and generate coronal x-ray bright points through reconnection, was performed. We modified the model for application to the upper TR and found it sufficient to post-predict our UBP observations if the magnetic reconnection efficiency parameter, θ, varied between 0.1 and 1.0 across the TR and if the background magnetic field, B0 = 6 Gauss. We discuss the implications of this study for the overall structure and energy balance of the sun's upper TR and our plans for future work.

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