Spectral signatures of dynamic plasmasSpectral signatures of dynamic plasmas Many space missions over the past 30 yrsMany space missions over the past 30 yrs A very dynamic SunA very dynamic Sun

SoHO/EITHinode/SOT

Most data interpreted using the `coronal Most data interpreted using the `coronal approximation’ . i.e. Ionization equilibrium approximation’ . i.e. Ionization equilibrium assumed, stage-to-stage ionization assumed, stage-to-stage ionization assumed .. How good is this???assumed .. How good is this???

Three examples:Three examples:

(i)(i) Electron density dependent ionizationElectron density dependent ionization

(ii) Transient ionization in the early stages of a (ii) Transient ionization in the early stages of a solar flaresolar flare

(iii) Non-thermal distributions(iii) Non-thermal distributions

..Consider two resonance lines,

N V 1238 ... from Be-like ion

O V 629 ... from Li-like ion

have over-lapping formation

temperatures

Should

give the

same

info????

SKYLAB data from mid 70’s show O V & N V have a different response,

O V QS AR 3—4

N V QS AR 8—10

WHY?

..

.. Resolved case .. Metastable included

N V intensity increases while O V decreases as Ne

increases

At Ne=1011 cm-3, N V 1238 > 60% .. O V < factor of ~2, thus the response in ARs differ by a factor of ~3

. . O V 629/N V 1238 line core ratio

At Ne = 1011 cm -3, O V 629 is reduced by almost a factor of two while N V 1238 is increased by almost a factor of two, giving a factor of ~ 3 difference .. would transient ionization make a difference??

..High UV line data from SMM/UVSP show a High UV line data from SMM/UVSP show a high correlation with hard X-ray bursts (>25 high correlation with hard X-ray bursts (>25 keV). WHY?keV). WHY?

..

..correlation of O V 1371 & HXR shows that O V correlation of O V 1371 & HXR shows that O V lacks the HXR by 0.3 to 0.7s and is flare lacks the HXR by 0.3 to 0.7s and is flare dependentdependent

. . Converting to the Line Contribution Function, we Converting to the Line Contribution Function, we have a factor of 3 enhancement at 10have a factor of 3 enhancement at 101111 cm cm-3-3 after after only 0.1s only 0.1s

Response time is prop. to NResponse time is prop. to Nee, therefore if N, therefore if Nee is is

smaller, the response time is longersmaller, the response time is longer Can explain the near simul. UV/HXR responseCan explain the near simul. UV/HXR response Need to investigate the possibility of a non-Need to investigate the possibility of a non-

GaussianGaussian

Future work: short duration EE seen in TR (105 K) lines but not in Mg X not important for coronal heating .. BUT we see them Fe XII lines .. WHY .. Transient ionization

. . Non-thermal recombination Non-thermal recombination

HXR flare date .. Cold thick target HXR flare date .. Cold thick target

(bremsstrahlung) model .. Problem (bremsstrahlung) model .. Problem

requires a large # of electronsrequires a large # of electrons

Recent work suggests nonthermal electrons by Recent work suggests nonthermal electrons by recombination is very important recombination is very important reduced the # of reduced the # of electrons by ~10 .. Problem electrons by ~10 .. Problem they used Kramers they used Kramers approx. approx.

Want to use ADAS to look at this problem using better Want to use ADAS to look at this problem using better data .. Also, what if we changed from an electron to data .. Also, what if we changed from an electron to a proton beam???a proton beam???