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In the early days (1972) of solar hard X-ray flare observations,  
In the early days (1972) of solar hard X-ray flare observations,  
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http://adsabs.harvard.edu/abs/1972ApJ...171..377T Fred
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[http://adsabs.harvard.edu/abs/1972ApJ...171..377T] Fred
Tomblin published theoretical arguments  
Tomblin published theoretical arguments  
that the hard X-ray spectrum of solar flares in the 5-40 keV  
that the hard X-ray spectrum of solar flares in the 5-40 keV  
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in the photosphere of those primary bremsstrahlung  
in the photosphere of those primary bremsstrahlung  
photons that are emitted downward. In a more complete  
photons that are emitted downward. In a more complete  
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analysis,  <a href="http://adsabs.harvard.edu/abs/1978ApJ...219..705B">
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analysis,  http://adsabs.harvard.edu/abs/1978ApJ...219..705B
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Taeil Bai & Reuven Ramaty</a>
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Taeil Bai & Reuven Ramaty showed that this albedo component would be polarized and  
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showed that this albedo component would be polarized and  
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its size must depend on the height of the primary source.
its size must depend on the height of the primary source.
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<h3> Why albedo has not been imaged before </h3>
<h3> Why albedo has not been imaged before </h3>
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A significant fraction (possibly as high as 40%) of the X-ray flux from solar flares  
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A significant fraction (possibly as high as 40%) of the X-ray flux from solar flares comes from X-rays that propagate back to the solar surface from coronal sources and "reflect" off the photosphere. This component of flares is called the <i>albedo</i>, and it is remarkably difficult to observe because it is very diffuse with an intensity that is one or two
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comes from X-rays
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that propagate back to the solar surface from coronal sources and "reflect" off  
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the photosphere. This component of flares is called the <i>albedo</i>, and it is remarkably  
+
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difficult to observe because it is very diffuse with an intensity that is one or two
+
orders of magnitude smaller than the primary flare sources themselves.
orders of magnitude smaller than the primary flare sources themselves.
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Its importance for flare physics is that it both distorts the spectral interpretation of X-ray  
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Its importance for flare physics is that it both distorts the spectral interpretation of X-ray emission and offers a potentially powerful diagnostic of electrons accelerated in solar flares. Our study uses the unique capabilities of the Ramaty High Energy Spectroscopic Imager (RHESSI) to isolate this albedo component, determine its properties such as size, shape and centroid location as a function of energy. We have focused on single-component flares in the 12-30 keV range that appear a within 45&deg; of disk center. Using standard techniques, we have obtained the X-ray visibilities  
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emission and offers a potentially powerful diagnostic of electrons accelerated in  
+
-
solar flares. Our study uses the unique capabilities of the Ramaty High Energy  
+
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Spectroscopic Imager (RHESSI) to isolate this albedo component, determine its  
+
-
properties such as size, shape and centroid location as a function of energy.  
+
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We have focused on single-component flares in the 12-30 keV range that appear a
+
-
within 45&deg; of disk center. Using standard techniques, we have obtained the X-ray  
+
-
visibilities  
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(<a href="http://sprg.ssl.berkeley.edu/~tohban/wiki/index.php/RHESSI_Visibilities">RHESSI Nugget # 39</a>) of a number of such flares and applied Forward-Fitting methods
(<a href="http://sprg.ssl.berkeley.edu/~tohban/wiki/index.php/RHESSI_Visibilities">RHESSI Nugget # 39</a>) of a number of such flares and applied Forward-Fitting methods
to determine the parameters of the primary component (position, flux, and size) and  
to determine the parameters of the primary component (position, flux, and size) and  

Revision as of 22:26, 12 January 2010

Contents

Solar Hard X-ray Albedo

In the early days (1972) of solar hard X-ray flare observations, [1] Fred Tomblin published theoretical arguments that the hard X-ray spectrum of solar flares in the 5-40 keV range must have an albedo component due to Compton back-scattering in the photosphere of those primary bremsstrahlung photons that are emitted downward. In a more complete analysis, http://adsabs.harvard.edu/abs/1978ApJ...219..705B Taeil Bai & Reuven Ramaty showed that this albedo component would be polarized and its size must depend on the height of the primary source.

The "reflected" photons form what is called an albedo patch. For sufficiently high primary source altitudes, the albedo would be much larger in extent than the primary source, with a size scale that increases with source height. (See Fig. 1 below.) Furthermore, the albedo source would be displaced toward disk center by a distance h sin θ, where θ is the heliocentric angle.


Why albedo has not been imaged before

A significant fraction (possibly as high as 40%) of the X-ray flux from solar flares comes from X-rays that propagate back to the solar surface from coronal sources and "reflect" off the photosphere. This component of flares is called the albedo, and it is remarkably difficult to observe because it is very diffuse with an intensity that is one or two orders of magnitude smaller than the primary flare sources themselves. Its importance for flare physics is that it both distorts the spectral interpretation of X-ray emission and offers a potentially powerful diagnostic of electrons accelerated in solar flares. Our study uses the unique capabilities of the Ramaty High Energy Spectroscopic Imager (RHESSI) to isolate this albedo component, determine its properties such as size, shape and centroid location as a function of energy. We have focused on single-component flares in the 12-30 keV range that appear a within 45° of disk center. Using standard techniques, we have obtained the X-ray visibilities (<a href="http://sprg.ssl.berkeley.edu/~tohban/wiki/index.php/RHESSI_Visibilities">RHESSI Nugget # 39</a>) of a number of such flares and applied Forward-Fitting methods to determine the parameters of the primary component (position, flux, and size) and the albedo-related parameters (primary source height and albedo flux).


Sensitivity to source size

The modulation of RHESSI's count rates depends exquisitely on the grid pitch and the source size, a fundamental property of Fourier imaging. When the source FWHM is less than the subcollimator angular resolution, the modulation amplitude falls rapidly. This is illustrated below for three subcollimators with angular resolutions of 23, 69 and 217.

Previous attempts to infer albedo properties

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