Observational evidence for breakout reconnection
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- | The two observed coronal X-ray sources serve to locate the two jets above and below the indicated flare reconnection site. Radially above the active region and the X-ray sources (in projection on the plane of sky) two radio sources are located. The lower one is a counterpart of the upper X-ray source. The upper of these two sources | + | The two observed coronal X-ray sources serve to locate the two jets above and below the indicated flare reconnection site. Radially above the active region and the X-ray sources (in projection on the plane of sky) two radio sources are located. The lower one is a counterpart of the upper X-ray source. The upper of these two sources indicates the breakout reconnection together with two other sources seen at lower frequencies (here shown at NRH 236.6 MHz): these flank the upper radially oriented radio sources as nicely seen in Figure 3. |
A plausible explanation for this arrangement is that the lower radio source, like the upper X‑ray source, was associated with the upward-directed flare reconnection jet. The upper radio source above the flaring active region remained stationary in space in the next minutes of the flare thus indicating the ongoing breakout reconnection process in that height level of the corona. | A plausible explanation for this arrangement is that the lower radio source, like the upper X‑ray source, was associated with the upward-directed flare reconnection jet. The upper radio source above the flaring active region remained stationary in space in the next minutes of the flare thus indicating the ongoing breakout reconnection process in that height level of the corona. |
Revision as of 12:11, 12 March 2013
Authors: Henry Aurass and Gordon Holman
In solar eruptive events (SEE's, Holman 2012) the transition from slow to fast (eruptive) energy release leads to the interaction of a flux rope with the overlying magnetic field. If the flux rope has a field component opposite to that of the overlying field, magnetic reconnection between both fields can become observable due to the associated electron acceleration and radio emission. Such a breakout reconnection scenario is included in many numerical simulations of SEEs, but observational support for it has so far been weak.
Strong evidence for breakout reconnection has recently been identified in the combined meter-wave radio and RHESSI X-ray observations of a well-observed SEE (Aurass et al. 2013). Figure 1 shows the dynamic radio spectrum (AIP) and the RHESSI 150-300 keV flux curve. The onset of strong particle acceleration is indicated by a light-brown box in Figure 1, and the radio spectrum is enlarged and contrast-enhanced in Figure 2. It depicts the dynamic spectrum of a seemingly minute feature (the black arrow points to it) shown spatially resolved in Figure 3. Several radio sources appear instead the previous faint one above the active region: we show the radio images at two frequencies (Nançay Multifrequency Radioheliograph, NRH, courtesy: The Radioheliograph Group), as well as the RHESSI hard X-ray image.
The two observed coronal X-ray sources serve to locate the two jets above and below the indicated flare reconnection site. Radially above the active region and the X-ray sources (in projection on the plane of sky) two radio sources are located. The lower one is a counterpart of the upper X-ray source. The upper of these two sources indicates the breakout reconnection together with two other sources seen at lower frequencies (here shown at NRH 236.6 MHz): these flank the upper radially oriented radio sources as nicely seen in Figure 3.
A plausible explanation for this arrangement is that the lower radio source, like the upper X‑ray source, was associated with the upward-directed flare reconnection jet. The upper radio source above the flaring active region remained stationary in space in the next minutes of the flare thus indicating the ongoing breakout reconnection process in that height level of the corona.
![](/~tohban/wiki/images/thumb/3/3a/Fig3_neu.png/650px-Fig3_neu.png)
The configuration given by Figure 3 marks some progress in our understanding of X-ray and radio data during the very onset of eruptive energy release in SEEs: the excellent timing between the occurrence of the radially elongated radio source formation and the "above the HXR loop top source" (Sui et al. 2004) reveals that both sources belong to the same (the upper flare reconnection) hot and turbulent plasma jet. The observations described here for a near-limb event are reminiscent of the results about another SEE seen in projection on the disc where a radio source in a distance of about 0.3 solar radii from the flaring active region occurs simultaneously with the most energetic X-ray and Gamma-ray emission (see Aurass et al. 2011, 2006).
References:
H. Aurass, G. Holman, S. Braune, G. Mann, P. Zlobec: 2013, A&A submitted.
H. Aurass, G. Mann, P. Zlobec, M. Karlicky: 2011, ApJ 730, 57A
H. Aurass, G. Mann, G. Rausche, A. Warmuth: 2006, A&A 457, 681
Holman, G.D.: 2012, Physics Today 04, 56
Sui, L., Holman, G.D., Dennis, B.R.: 2004, ApJ 612, 546