The heating of the solar corona has been investigated during four of decades and several mechanisms able to produce heating have been proposed. It has until now not been possible to produce quantit ...

Modern solar telescope design in the EUV to x-ray range is now capable of producing large images in multiple channels at rapid cadences, with high spatial and temperature resolution. We discuss reconstruction of differential emission measures for solar coronal plasma using two state-of-the-art instruments: the X-Ray Telescope on Solar-B, and the Atmospheric Imaging Assembly on the Solar Dynamics Observatory. We discuss the relative merits of iteration and direct inversion methods for determining DEM(T ). We also consider strategies for automating and visualizing DEM maps, given the high data rates that these instruments will produce. We touch on the scientific potential of high-cadence, spatially resolved DEM data products. Solar telescope design in the EUV to x-ray range is now capable of producing large images (4096 × 4096 pixels) in multiple channels (six or more) at rapid cadences (∼ 10 seconds), with high spatial (sub-arcsecond) and temperature (order of emission kernel widths) resolution. Such instruments permit more sophisticated temperature diagnostics than the filter-ratio method used with the previous generation of coronal imaging telescopes. In this paper, we discuss the issues, capabilities, and science for DEM reconstruction in the context of two state-of-the-art instruments: the X-Ray Telescope on the Solar-B spacecraft, and the Atmospheric Imaging Assembly on the Solar Dynamics Observatory. The X-Ray Telescope (XRT) is a grazing-incidence, broadband instrument with nine diagnostic filters spanning the range 6.1 < log T< 7.5. More information on the design of XRT for DEM reconstruction can be found in Golub et al. (2004). The Atmospheric Imaging Assembly (AIA) is a normal-incidence, narrow-band instrument with four 20-cm, dual-channel telescopes operating simultaneously at a 10 second cadence (Fig. 1a). The mirrors in each telescope are subdivided into two areas (called “D”s) with different multilayer coatings, giving seven EUV channels, plus a channel used for UV and white-light observations (Fig. 1b). The AIA will be able to image coronal plasmas for 5.5 < log T< 7.5, and cooler regions of the solar atmosphere. The focal plane detector is a 4k×4k back-illuminated CCD with 0.6 arcsecond pixels and a 43 arcminute field-of-view which will be able to capture the entire solar disk— the AIA will combine the f.o.v. of SoHO/EIT with the resolution of TRACE.

https://www.cambridge.org/core/services/aop-cambridge-core/content/view/6D55172E0D320EA8C26F02C35034B83D/S1743921304006088a.pdf/div-class-title-temperature-diagnostics-with-multichannel-imaging-telescopes-div.pdf

Temperature diagnostics with multichannel imaging telescopes

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The coronal heating problem

Physics of fully ionized gases

L. Spitzer: Physics of Fully Ionized Gases, Interscience Tracts on Physics and astronomy, New york, 1956, 105頁, 13×21cm.

Physics of Fully Ionized Gases

Cosmical Magnetic Fields: Their Origin and their Activity

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The coronal heating problem

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Temperature diagnostics with multichannel imaging telescopes

References

Physics of fully ionized gases

L. Spitzer: Physics of Fully Ionized Gases, Interscience Tracts on Physics and astronomy, New york, 1956, 105頁, 13×21cm.

Physics of Fully Ionized Gases

Cosmical Magnetic Fields: Their Origin and their Activity

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