Defining the "Blind Spot" of Hinode EIS and XRT Temperature Measurements

Details Defining the "Blind Spot" of Hinode EIS and XRT Temperature Measurements Defining the "Blind Spot" of Hinode EIS and XRT Temperature Measurements

Feb 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012apj...746l..17w&link_type=abstract

The Astrophysical Journal Letters, Volume 746, Issue 2, article id. L17 (2012).

Astronomy and Astrophysics

Astronomy

Sun: Corona

Scientific paper

Observing high-temperature, low emission measure plasma is key to unlocking the coronal heating problem. With current instrumentation, a combination of EUV spectral data from Hinode Extreme-ultraviolet Imaging Spectrometer (EIS; sensitive to temperatures up to 4 MK) and broadband filter data from Hinode X-ray Telescope (XRT; sensitive to higher temperatures) is typically used to diagnose the temperature structure of the observed plasma. In this Letter, we demonstrate that a "blind spot" exists in temperature-emission measure space for combined Hinode EIS and XRT observations. For a typical active region core with significant emission at 3-4 MK, Hinode EIS and XRT are insensitive to plasma with temperatures greater than ~6 MK and emission measures less than ~1027 cm-5. We then demonstrate that the temperature and emission measure limits of this blind spot depend upon the temperature distribution of the plasma along the line of sight by considering a hypothetical emission measure distribution sharply peaked at 1 MK. For this emission measure distribution, we find that EIS and XRT are insensitive to plasma with emission measures less than ~1026 cm-5. We suggest that a spatially and spectrally resolved 6-24 Å spectrum would improve the sensitivity to these high-temperature, low emission measure plasma.

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