Ion Temperature and Non-Thermal Velocity in a Solar Active Region: Using Emission Lines of Different Atomic Species

Details Ion Temperature and Non-Thermal Velocity in a Solar Active Region: Using Emission Lines of Different Atomic Species Ion Temperature and Non-Thermal Velocity in a Solar Active Region: Using Emission Lines of Different Atomic Species

Nov 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009apj...705l.208i&link_type=abstract

The Astrophysical Journal Letters, Volume 705, Issue 2, pp. L208-L212 (2009).

Astronomy and Astrophysics

Astronomy

5

Sun: Activity, Sun: Corona

Scientific paper

We have studied the characteristics of the ion thermal temperature and non-thermal velocity in an active region observed by the EUV Imaging Spectrometer onboard Hinode. We used two emission lines of different atomic species (Fe XVI 262.98 Å and S XIII 256.69 Å) to distinguish the ion thermal velocity from the observed full width at half-maximum. We assumed that the sources of the two emission lines are the same thermal temperature. We also assumed that they have the same non-thermal velocity. With these assumptions, we could obtain the ion thermal temperature, after noting that M sulfur ~ 0.6M iron. We have carried out the ion thermal temperature analysis in the active region where the photon counts are sufficient (>4500). What we found is as follows: (1) the common ion thermal temperatures obtained by Fe XVI and S XIII are ~2.5 MK, (2) the typical non-thermal velocities are ~13 km s-1, (3) the highest non-thermal velocities (>20 km s-1) are preferentially observed between the bright points in Fe XVI, while (4) the hottest material (>3 MK) is observed relatively inside the bright points compared with the highest non-thermal velocity region.

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