The RHESSI Imaging Concept

By G. Hurford, E. Schmahl, Richard A. Schwartz, A. Conway, Markus J. Aschwanden, A. Csillaghy, B. Dennis, C. Johns–Krull, S. Krucker, R. Lin and 4 more. 2002

492 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering

View Paper: https://www.semanticscholar.org/paper/4a78cfa8b16781d377853ef51bb94cc99c5df925

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. M. Temmer
2. H. Hudson
3. B. Vršnak
4. Astrid Veronig
5. V. Petrosian
6. Nat Gopalswamy
7. S. Krucker
8. N. Vilmer

In Electrical and Electronic Engineering

1. Michele Piana
2. Yang Liu
3. Gianfranco Brunetti

Citations in the corpus

• An Observational Overview of Solar Flares (2011, background): “Each of the detectors has a bigrid modulation collimator with different parameters (thickness and angular resolution) (Hurford et al. 2002), giving imaging (at a basic 4-s time resolution governed by spacecraft rotation) down to the arcsec range.”
• RESPONSE OF THE PHOTOSPHERIC MAGNETIC FIELD TO THE X2.2 FLARE ON 2011 FEBRUARY 15 (2011, methodology): “PIXON images (Hurford et al. 2002) in the 35–100 keV energy range showing the flare footpoints were reconstructed using the front segments of detectors 2–8 with 16–32 s integration time throughout the event.”
• X-ray sources and magnetic reconnection in the X3.9 flare of 2003 November 3 (2006, methodology): “Note that although the angular resolution in the reconstructed RHESSI images is ∼7′′, the emission centroids can be determined with an accuracy which may be <1′′, depending on the count statistics (Hurford et al. 2002).”
• Energy partition in two solar flare/CME events (2004, methodology): “This is consistent with the area of the 50% contour of the 12–25 keV image shown in Figure 4 that was produced from the RHESSI data using the CLEAN reconstruction algorithm [Hurford et al., 2002].”
• RHESSI Microflare Statistics. I. Flare-Finding and Frequency Distributions (2008, methodology): “In order to certify that events are of solar origin all events are also imaged using back-projection (Hurford et al. 2002) and their locations found (see x 3.1).”
• RHESSI Observations of Particle Acceleration and Energy Release in an Intense Solar Gamma-Ray Line Flare (2003, background): “RHESSI (Hurford et al. 2002) is made up of nine bi-grid rotating modulation collimators (RMCs), each consisting of a pair of widely separated grids mounted on a rotating spacecraft, to provide a spatial resolution of 2 .3–3 over the full-Sun (∼1 ) field of view.”
• A Coronal Thick-Target Interpretation of Two Hard X-Ray Loop Events (2004, methodology): “Figure 2 shows a RHESSI image sequence obtained with the CLEAN algorithm (Hurford et al. 2002).”
• COMBINED STEREO/RHESSI STUDY OF CORONAL MASS EJECTION ACCELERATION AND PARTICLE ACCELERATION IN SOLAR FLARES (2010, methodology): “Figure 5 shows the RHESSI HXR image (top) reconstructed in the energy band 30–50 keV with the CLEAN algorithm (Hurford et al. 2002) together with its spectrum (bottom) integrated over 20 sec around the peak of the HXR emission.”
• Evidence for the Formation of a Large-Scale Current Sheet in a Solar Flare (2003, methodology): “…phase of the flare (before 23:09:40 UT), the spatially integrated X-ray spectrum can be fitted with an isothermal bremsstrahlung function (exponential form) with a temperature of 20–30 MK. TheRHESSI images obtained with the CLEAN imaging algorithm (Hurford et al. 2002) show a cuspshaped flare loop.”
• Double Coronal Hard and Soft X-Ray Source Observed by RHESSI: Evidence for Magnetic Reconnection and Particle Acceleration in Solar Flares (2007, methodology): “Figure 3 shows PIXON (Metcalf et al. 1996; Hurford et al. 2002) images at different energies integrated over the interval of 08:20:27– 08:20:56 UT (marked #2 in Figure 2) during the first HXR peak.”
• RHESSI Microflare Statistics. II. X-Ray Imaging, Spectroscopy, and Energy Distributions (2007, methodology): “This spatial information encoded in the time-modulation profile is normally reconstructed into an image via techniques such as back projection (Hurford et al. 2002).”
• Deducing Electron Properties from Hard X-ray Observations (2011, methodology): “These maps are produced by applying image processing algorithms (e.g., back-projection, CLEAN, Maximum Entropy or Pixon; for details see Hurford et al. 2002) to the temporally modulated fluxes from each of RHESSI’s detectors, in which spatial information on the source is encoded.”