BARREL Balloon Observations and History

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Revision as of 23:13, 18 February 2014

Introduction

Solar hard X-rays and gamma-rays were discovered in the middle of the last century via balloon-borne instruments [Ref. 1] deployed by the Minnesota physicists L.E. Peterson and J.R. Winckler; the latter also discovered sprites. By modern naming convention, we'd call their flare SOL1958-03-20T13:05, but it preceded any useful soft X-ray observations and so there is no GOES classification of the event. Peterson & Winckler do report the simultaneous occurrence of a "magnetic crotchet," as also detected in the case of the Carrington flare in 1859. Such a geomagnetic effect clearly indicates the presence of strong solar soft X-ray emission along with the high-energy radiations discovered from the balloon.

In this Nugget we report recent balloon-borne observations from multiple balloons of the BARREL expedition to the Antarctic. Robyn MIllan of Dartmouth College is the lead scientist of this ambitious experiment. As with the original Peterson-Winckler experiment, BARREL wasn't designed to study solar flares, but their signals come through loud and clear anyway. BARREL's instrumentation allows it to study the precipitation of relativistic electrons from the Earth's Van Allen Belts, which indeed may share some kinds of plasma physics with what happens in a solar flare.

How BARREL Works

A stream of small balloons circles the Antarctic continent, following the vortex winds at high altitudes in the polar regions. At any one time several balloons can fly simultaneously, strung out around the Antarctic according to their time of launch. Power comes from solar cells, and full-time communication via the Iridium satellite network and an automated connection to a real-time webpage, allowing the ground-based scientists to follow along. For radiation-belt studies, multi-point measurements mean much better science. A rather fine video describes the basic program better than we can here. We do show a pretty picture here in Figure 1, though, taken at the launch of a BARREL balloon from the South African Antarctic station SANAE.

Fig. 1: A BARREL balloon shortly after launch (view from below). One can see the balloon billowing out, still far from inflated since it is just after launch; the red parachute, furled, and the payload itself. The payload itself weighs only about 20 kg, and is whisked eventually up to 30-35 km, well above 99% of the Earth's atmosphere. The balloon can maintain this altitude for the time it takes to circumnavigate the globe, albeit at very high latitude.

The instrumentation on each BARREL payload consists of a simple isotropically sensitive sodium iodide scintillation counter. This responds well to the gamma-rays and hard X-rays resulting from bremsstrahlung as the expected relativistic electrons undergo atomic collisions in the upper atmosphere. The time variations reveal the presence of interesting phenomena, and the detector records their spectra over a wide energy range The solar gamma-rays and hard X-rays result from similar physics, but with the collisions taking place in the solar atmosphere instead of the Earth's.

BARREL Solar Observations

The BARREL detectors respond to many things, since they are above the atmosphere. The full list would include many sources of cosmic X-rays, the Sun as illustrated here, the Van Allen Belts by design, and radiation from the Earth's atmosphere. For each of these components, the others would be termed "background radiation" and just reduce the quality of the observation - but that is how astrophysics usually works!

Figure 2 shows the BARREL responses to the modest M-class flare SOL2014-02-07T10:29. Note that BARREL payload "2O" missed out, but note also (the lower left panels) that it was at low altitude. This results in severe extinction of the incident solar radiation, especially since the Sun is low on the horizon even at high noon at such latitudes - if up at all.

Fig. 2: A large complicated figure! The panels on the left show, top to bottom, the GOES soft X-ray fluxes (flares); three sets of counting rates from different BARREL balloons flying on 7 February; and their heights and local times (longitudes). On the right is the clear response two of them gave to the modest flare at 10:28 UT.

The solar observations we show are only of academic interest, since not only RHESSI but also Fermi routinely produce comparable or better data for flares such as these. If a remarkable event such as the Peterson-Winckler event [Ref. 1] should be found in the accumulated BARREL database it could be a different matter.

Conclusions

BARREL reminds us of the origins of solar high-energy astrophysics (soft X-rays, hard X-rays, gamma rays, "solar cosmic rays"), where many interesting properties of solar flares at high energies were first discovered a half-century ago, mainly by Winckler and his group.

References

• [1] Gamma-Ray Burst from a Solar Flare