The RHESSI satellite uses an instrument that can produce images of high-energy X-ray and gamma-ray emissions. A software algorithm automatically identifies events in the RHESSI data, and these events include solar flares as well as other events that may be of scientific interest. For the solar flares, other software automatically generates images in a number of energy bands, and these images are called "quicklook" images.
These quicklook images provide a very useful tool for easily checking that an event seen in the RHESSI light curves is a solar flare and determining from where it originated on the Sun. The location of the flare is typically associated with a group of sunspots, or active region, on the Sun. A given active region can be visible for two weeks as the Sun rotates, and can produce many flares during that time.
Above: the RHESSI Images date chooser
The RHESSI browser opens at an automatically selected time, which may not correspond to the most recent data available. You can start by selecting the day you are interested in:
Above: the RHESSI Images 24 hour time bar
Because flares can be as short as a minute, you will need to select a particular flare on that day before you can see any images. There are two ways for selecting a flare:
Above: A reconstructed RHESSI Image from the data page
The colored bar across the top indicates the intensity scale of the X-ray or gamma-ray emission in the image, with the strongest emission being yellow to white. The coordinate system is centered on the Sun, and the axes measure the angle on the sky in units of arcseconds (1 arcsecond is 1/3600 of a degree). The edge of Sun, or limb, is denoted by the white circle, and thus solar flares will occur within or just slightly outside this circle. Also listed on the image is relevant technical information such as the time range (in UT) and the energy band (in keV).
The solar flare itself will appear as the brightest spot in the image. Due to RHESSI's imaging method, there will also be red and purple concentric rings encircling the flare. If the location of the flare is very close to the location of the so-called "spin axis" of the spacecraft (denoted by a white cross), then the image may be somewhat distorted.
This full-Sun image is useful for seeing where the flare occurred in the context of the whole Sun, but it only shows the image for the energies 6-25 keV. If you click the magnifying glass to the right of "Quicklook Images" in the upper left, you will reveal a list of checkboxes that let you turn on the display of images for a variety of energy bands. Note that these types of images are zoomed in, so you may or may not see the white circle representing the solar limb.
The above tutorials compliment the downloadable Flip Charts and Data Sheets.