The Role of Magnetic Reconnection in the 2004 August 18 Solar Eruption

Mathematics – Logic

Scientific paper

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7513 Coronal Mass Ejections (2101), 7514 Energetic Particles (2114), 7519 Flares, 7526 Magnetic Reconnection (2723, 7835), 7531 Prominence Eruptions

Scientific paper

We present a morphological study of the 2004 August 18 solar flare in which an erupting prominence is clearly visible as a bright helical structure on (E)UV images of the Transition Region and Coronal Explorer (TRACE) and H-alpha filtergrams of the Big Bear Solar Observatory (BBSO). The associated coronal mass ejection (CME) is traced with white light images of the Mouna Loa Solar Observatory (MLSO) that covers the low corona (down to 1.08 solar radii) in order to determine its causal relationship with the flare. Used as a signature of magnetic reconnection is the flare radiation at hard X-rays (HXR) and microwaves, measured by the Ramaty High Energy Solar Spectroscopic Imager (RHESSI) and the Owens Valley Solar Array (OVSA), respectively. The HXR- microwave emissions appear in multiple bursts located mostly near the surface in a complicated pattern that varies from a peak to another. It is, however, obvious that the first HXR-microwave burst precedes the magnetic flux rising and that the prominence fully erupts only after the HXR-microwave bursts. Therefore, the role of the first magnetic reconnection would be tether-cutting that allows the magnetic flux rope to rise through the overlying field. We further argue that the subsequent reconnections play a role in adding poloidal flux to the flux rope and thus rendering it unstable to eruption, based on comparison of the observed morphological evolution of the prominence with that of the kink instability model by Torok and Kleim (2005).

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