The Alfven Speed above a Sunspot, and Gamma-rays
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flares, i.e. that Kahler's "big flare syndrome" (where everything scales | flares, i.e. that Kahler's "big flare syndrome" (where everything scales | ||
together) does not apply in this case. | together) does not apply in this case. | ||
- | For this flare, Figure 2 shows that there was negligible [2.2 MeV | + | For this flare, Figure 2 shows that there was negligible [http://en.wikipedia.org/wiki/Solar_surface_fusion 2.2 MeV gamma-ray emission line], RHESSI's most sensitive tool for this purpose, and |
- | gamma-ray emission, RHESSI's most sensitive tool for this purpose, and | + | |
that the hard X-ray spectrum was weak above 50 keV. | that the hard X-ray spectrum was weak above 50 keV. | ||
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Many research workers will express surprise at the strength of the | Many research workers will express surprise at the strength of the | ||
[http://solarscience.msfc.nasa.gov/3dfields.shtml coronal magnetic field] | [http://solarscience.msfc.nasa.gov/3dfields.shtml coronal magnetic field] | ||
- | + | above a big spot, | |
about the [http://en.wikipedia.org/wiki/Alfvén_wave Alfvén speed], | about the [http://en.wikipedia.org/wiki/Alfvén_wave Alfvén speed], | ||
and about the [http://en.wikipedia.org/wiki/Beta_(plasma_physics) plasma beta] | and about the [http://en.wikipedia.org/wiki/Beta_(plasma_physics) plasma beta] | ||
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below a few Mm above a big spot! | below a few Mm above a big spot! | ||
Figure 3 details some of these parameters for a conservatively chosen | Figure 3 details some of these parameters for a conservatively chosen | ||
- | set of model conditions above a sunspot. | + | set of model conditions above a very large sunspot. |
- | One of the problems of | + | One of the problems of the corona above a spot umbra is so dark and non-emissive |
that ordinary astronomical techniques do not work very well, and so | that ordinary astronomical techniques do not work very well, and so | ||
in fact there are major observational uncertainties. | in fact there are major observational uncertainties. | ||
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]] | ]] | ||
- | Is this estimation, which is based on | + | Is this estimation, which is based on [http://adsabs.harvard.edu/abs/2000asqu.book.....C Allen's Astrophysical Quantities], |
- | [Allen's Astrophysical Quantities], | + | |
at all relevant to the particular flare we are discussing? | at all relevant to the particular flare we are discussing? | ||
Perhaps not directly, since the Hinode magnetographic observations suggest | Perhaps not directly, since the Hinode magnetographic observations suggest | ||
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manifestations of major flares within sunspots, with new thinking about | manifestations of major flares within sunspots, with new thinking about | ||
the theory of the processes in the corona just above them. | the theory of the processes in the corona just above them. | ||
- | A relativistic Alfvén speed means that the Poynting flux can rival | + | A relativistic Alfvén speed means that the [http://en.wikipedia.org/wiki/Flux Poynting flux] can rival |
the motions of accelerated particles, for example. | the motions of accelerated particles, for example. | ||
- | Although the theory is at its bare beginnings, it also seems likely that | + | Although the theory of these phenomena is still at its bare beginnings, it also seems likely that |
such extreme values of Alfvén speed and plasma beta will also help to | such extreme values of Alfvén speed and plasma beta will also help to | ||
accelerate the particles that RHESSI detects through hard X-rays and gamma | accelerate the particles that RHESSI detects through hard X-rays and gamma | ||
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But why, in the case of the flare we have illustrated here, were there no | But why, in the case of the flare we have illustrated here, were there no | ||
gamma rays to speak of? | gamma rays to speak of? | ||
+ | And yet, there was a | ||
+ | [http://sprg.ssl.berkeley.edu/~tohban/wiki/index.php/First_Sunquake_of_Solar_Cycle_24_Observed_by_Solar_Dynamics_Observatory sunquake]. | ||
Does the ion acceleration require a still stronger magnetic field? | Does the ion acceleration require a still stronger magnetic field? | ||
In the Alfvénic exhaust of | In the Alfvénic exhaust of |
Revision as of 11:54, 12 April 2011
Nugget | |
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Number: | 148 |
1st Author: | H. Hudson |
2nd Author: | L. Fletcher |
Published: | 12 April 2011 |
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Previous Nugget: | Slow Magnetoacoustic Waves in Two-Ribbon Flares |
List all |
Contents |
Introduction
It is common for powerful flares to occur actually within sunspots, with their H-alpha ribbons blithely crossing over these regions of very strong magnetic field. What does this association mean for flare theory, and what does it mean for the interesting differences RHESSI has discovered between flares with and without gamma-rays? We discuss these issues in the context of the X-class flare of February 15, 2011. This was only the second X-class flare of this solar maximum; it was not a gamma-ray event but it was the source of a clear sunquake.
Observations from Hinode and RHESSI
The flare was well-observed by the SOT white-light imager on Hinode, with 20-second cadence in three broad-band optical filters. This data set is quite remarkable because of the excellent resolution and brilliant image contrast achieved by the SOT telescope, the largest solar telescope ever put in space. Figure 1 shows an overlay of the patches of white-light emission extracted from the several images taken during the impulsive phase of the flare, which is when we ordinarily observe hard X-rays and gamma-rays.
At the same time as these white-light emissions, what was RHESSI seeing? Figure 2 offers a simplified view of the RHESSI counting rates, mainly to illustrate the distinct lack of a gamma-ray signature. RHESSI has shown that gamma-ray flares are quite different from ordinary flares, i.e. that Kahler's "big flare syndrome" (where everything scales together) does not apply in this case. For this flare, Figure 2 shows that there was negligible 2.2 MeV gamma-ray emission line, RHESSI's most sensitive tool for this purpose, and that the hard X-ray spectrum was weak above 50 keV.
Theory
As the images show, in this flare - as with many of the most powerful events - we are essentially looking deep into the core of the active region. In these cases the many signatures of non-thermal effects in the lower solar atmosphere (hard X-rays, H-alpha, EUV, and intense white light) all implicate the strong magnetic fields to be found in the umbra and penumbra regions of major sunspots.
In this Nugget we remind readers that the coronal volume just above a sunspot is a particularly interesting and ill-understood place. Many research workers will express surprise at the strength of the coronal magnetic field above a big spot, about the Alfvén speed, and about the plasma beta as well - all are extreme, according to the best observational estimates. The Alfvén speed, if computed naively, exceeds the speed of light below a few Mm above a big spot! Figure 3 details some of these parameters for a conservatively chosen set of model conditions above a very large sunspot. One of the problems of the corona above a spot umbra is so dark and non-emissive that ordinary astronomical techniques do not work very well, and so in fact there are major observational uncertainties. The theory behind the extrapolations in Figure 3 is very simple and safe, though. For a spot like this we could expect an Alfvén speed of c/3 at 10,000 km altitude.
Is this estimation, which is based on Allen's Astrophysical Quantities, at all relevant to the particular flare we are discussing? Perhaps not directly, since the Hinode magnetographic observations suggest field intensities about a factor of three smaller, and the spatial scales smaller as well. That means that the coronal field (intensity and scale) and Alfvén speed will be correspondingly smaller.
Speculation and Conclusion
This Nugget suggests that we begin to combine observations of the manifestations of major flares within sunspots, with new thinking about the theory of the processes in the corona just above them. A relativistic Alfvén speed means that the Poynting flux can rival the motions of accelerated particles, for example. Although the theory of these phenomena is still at its bare beginnings, it also seems likely that such extreme values of Alfvén speed and plasma beta will also help to accelerate the particles that RHESSI detects through hard X-rays and gamma rays. But why, in the case of the flare we have illustrated here, were there no gamma rays to speak of? And yet, there was a sunquake. Does the ion acceleration require a still stronger magnetic field? In the Alfvénic exhaust of magnetic reconnection one might expect the bulk motion to be in the form of relativistic particles, ie that the entire plasma would consist of high-energy particles rather than the usually assumed [Maxwellian distributions]. In any case we now have marvelous tools to study these questions observationally, and so we may expect some progress via studies of this and other flares with these tools; this Nugget and the sunquakes Nugget on the same event have only begun the work needed.
RHESSI Nugget Date | 12 April 2011 + |
RHESSI Nugget First Author | H. Hudson + |
RHESSI Nugget Index | 148 + |
RHESSI Nugget Second Author | L. Fletcher + |