RHESSI in Cycle 24

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Revision as of 00:37, 12 September 2009

Introduction

In anticipation of Solar Cycle 24 and the hoped-for huge flares it would produce, the RHESSI germanium detectors were annealed in late 2007. This process removes radiation damage caused by the continual exposure of the detectors to the Earth's radiation belts. It is a bit of a race against time for RHESSI, because we think that only a limited number of anneals will be possible; eventually they may poison the segmentation of the detectors and effectively eliminate their gamma-ray response. But, so far so good, as shown in this Nugget with a new-cycle flare. Regular readers may be puzzled by this, since in recent Nuggets (April and July 2009) we have been fretting about the great delay in Cycle 24's onset. Nonetheless at the time of writing there have already been some new-cycle spots and flares, although it is still the case that activity has not turned up as expected. We are still worried!

The flare we have imaged

This was a GOES C1 event on July 6, 2009. Its active region was at S25, a latitude where new-cycle spots tend to appear, and had the new-cycle polarity. So, no matter how feeble this cycle may turn out to be, we have tiny flares and may hope for more energetic ones that can be observed by RHESSI at all energies, ie up into the gamma-ray range.

Figure 1 shows set of RHESSI collimator responses for this event. These (rudimentary) back-projection images all look fine, except that there are relative flux calibration issues. These do not stop us from making pretty pictures via more sophisticated algorithms.

Figure 1 Individual collimator responses for the nine RHESSI detectors, each observing a different angular scale. This is the raw material of image formation, obtained by the elementary back projection algorithm.

The July 6 flare was interesting as well because of its association with a coronal mass ejection ([CME]). Generally speaking, it appears that at solar minimum we have much weaker flare signatures with CMEs (such as this one). A future Nugget should deal with this interesting fact.

What we saw

This flare had little hard X-ray emission, which may be a characteristic of these solar-minimum events. We have made images at 5-10 keV by the standard RHESSI techniques and show a Maximum Entropy image in Figure 2. This algorithm may tend to "over-resolve" the image, ie produce untrustworthy fine structure, but to our eye it looks pretty good in comparison with the background TRACE image. The EUV and soft X-ray sources need not always match, but the details here show a strong correlation.

Figure 2 RHESSI image over 5-10 keV, made a maximum entropy algorithm, superposed on a TRACE EUV image from a slightly later time.

Conclusions

• We can make images from Cycle 24 flares that are useful for scientific purposes.
• An updated calibration would improve the imaging performance of RHESSI.
• There have been no flares yet to check the RHESSI performance at higher energies (>20 keV) in Cycle 24.