The energy balance and pressure in the solar transition zone for network and active region features

1979 ◽  
Vol 233 ◽  
pp. 741 ◽  
Author(s):  
K. R. Nicolas ◽  
J.-D. F. Bartoe ◽  
G. E. Brueckner ◽  
M. E. Vanhoosier
Keyword(s):  
Energy Balance ◽  
Active Region ◽  
Transition Zone ◽  
Solar Transition

The chromosphere-corona transition zone above an active region

1984 ◽  
Vol 4 (8) ◽  
pp. 63-66 ◽  
Author(s):  
O. Kjeldseth Moe ◽  
Ø. Andreassen ◽  
P. Maltby ◽  
J.-D.F. Bartoe ◽  
G.E. Brueckner ◽  
...  
Keyword(s):  
Active Region ◽  
Transition Zone

Heating of the solar transition zone and corona

Solar Physics ◽  
1976 ◽  
Vol 50 (1) ◽  
pp. 99-108 ◽  
Author(s):  
D. Vanbeveren ◽  
C. De Loore
Keyword(s):  
Transition Zone ◽  
Solar Transition

Solar transition zone pressures from EUV observations of O IV and N IV

1982 ◽  
Vol 259 ◽  
pp. 366 ◽  
Author(s):  
K. P. Dere ◽  
J.-D. F. Bartoe ◽  
G. E. Brueckner
Keyword(s):  
Transition Zone ◽  
Solar Transition

A search for a turbulent-free region in the solar transition zone

1977 ◽  
Vol 216 ◽  
pp. L119 ◽  
Author(s):  
U. Feldman ◽  
G. A. Doschek
Keyword(s):  
Transition Zone ◽  
Solar Transition ◽  
Free Region

scholarly journals Modelling of Solar Coronal Loops

1992 ◽  
Vol 9 ◽  
pp. 661-662
Author(s):  
C. Jordan
Keyword(s):  
Energy Balance ◽  
Active Region ◽  
Active Regions ◽  
Coronal Loops ◽  
Loop Structure ◽  
X Rays ◽  
Spectroscopic Observations ◽  
Available Information ◽  
Solar Coronal

Modelling of coronal active regions in terms of loop structures began around 1974 (see Jordan 1975) and was stimulated by images of the corona in X-rays and the uv, obtained from rocket flights. Vaiana was a pioneer in this field (see Vaiana et al. 1973). The Skylab missions provided a fuller range of imaging and spectroscopic observations, and much of the available information is still based on these data (see Orrall 1981). Since 1975 a very large number of papers have been published on the various aspects of loop structure, heating and stability (see review by Mewe 1991). Here I can mention only a few points concerning the relation between observable parameters and the energy balance and heating requirements of active region loops.

Mass motions in optically thin solar transition zone lines

1981 ◽  
Vol 195 (2) ◽  
pp. 107-113 ◽  
Author(s):  
G. A. Doschek ◽  
John T. Mariska ◽  
U. Feldman
Keyword(s):  
Transition Zone ◽  
Solar Transition

Area variation with temperature of supergranule network features in the solar transition zone

Solar Physics ◽  
1978 ◽  
Vol 58 (1) ◽  
pp. 31-36 ◽  
Author(s):  
Edward J. Eadon ◽  
Donald E. Billings
Keyword(s):  
Transition Zone ◽  
Solar Transition ◽  
Area Variation

Euv Emission Line Ratios for Si IV in the Solar Transition Region

1988 ◽  
Vol 102 ◽  
pp. 227-229
Author(s):  
F.P. Keenan ◽  
J.G. Doyle
Keyword(s):  
Active Region ◽  
Emission Line ◽  
Electron Temperature ◽  
Electron Excitation ◽  
Atomic Data ◽  
Temperature Sensitive ◽  
Excitation Rate ◽  
R Matrix ◽  
Solar Transition Region ◽  
Solar Transition

AbstractTheoretical electron temperature sensitive emission line ratios in Si IV involving the 3d2D − 3p2P and 4s2S - 3p2P multiplets at ~1125A and 816A respectively are derived using R-matrix electron excitation rate calculations. A comparison of these with observational data for a solar active region obtained with the Harvard S-055 spectrometer on board Skylab reveals that there is good agreement between theory and observation for the ratio that includes the2D3/2, 5/2 −2p3/2 transition at 1128.3A. This is in contrast to the findings of Keenan, Dufton and Kingston, and provides support for the atomic data adopted in the calculations. However the2D3/2 −2pl/2 line at 1122.5A appears to be severely blended, as it leads to electron temperature estimates that differ significantly from that expected in ionisation equilibrium. The fact that the I(1122.5A)/I(1128.3A) intensity ratios determined from several flare spectra are closer to theory than that for the active region indicates that the blending is probably due to species with relatively low ionisation potentials, such as an Fe III transition at 1122.53A, as suggested previously by Burton and Ridgeley, and Feldman and Doschek. Electron temperatures deduced for a sunspot are much lower than that predicted from ionisation balance calculations, in agreement with earlier results, and imply that a cooling flow may be present.

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