Analysis of a Solar Coronal Bright Point Extreme Ultraviolet Spectrum from the EUNIS Sounding Rocket Instrument

Details Analysis of a Solar Coronal Bright Point Extreme Ultraviolet Spectrum from the EUNIS Sounding Rocket Instrument Analysis of a Solar Coronal Bright Point Extreme Ultraviolet Spectrum from the EUNIS Sounding Rocket Instrument

Apr 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008apj...677..781b&link_type=abstract

The Astrophysical Journal, Volume 677, Issue 1, pp. 781-789.

Astronomy and Astrophysics

Astronomy

10

Sun: Corona, Sun: Magnetic Fields, Sun: Transition Region, Sun: Uv Radiation

Scientific paper

We present a well-calibrated EUV spectrum of a solar coronal bright point observed with the Extreme Ultraviolet Normal Incidence Spectrograph (EUNIS) sounding rocket instrument on 2006 April 12. The coronal bright point brightened around 06:30 UT during a period of emerging magnetic flux and remained bright at least until the rocket flight around 18:12 UT, while the magnetic flux merged and canceled. Density-sensitive line intensity ratios yield mutually consistent coronal electron densities (Ne in cm-3) of logNe~9.4. The differential emission measure (DEM, in cm-5 K-1) curve derived from the spectrum yields a peak of logDEM~20.70 at logT~6.15 and a local minimum of logDEM~20.15 at logT~5.35. Photospheric (not coronal) element abundances are required to achieve equality and consistency in the DEM derived from lines of Mg V, Mg VI, Mg VII, and Ca VII (with a low first ionization potential, or FIP) and lines from Ne IV and Ne V (with a high FIP) formed at transition region temperatures. The bright point's photospheric abundance is likely produced by reconnection-driven chromospheric evaporation, a process that is not only central to existing bright point models, but also consistent with measurements of relative Doppler velocities.

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