Mj. Aschwanden et al., Modeling of coronal EUV loops observed with TRACE. I. Hydrostatic solutions with nonuniform heating, ASTROPHYS J, 550(2), 2001, pp. 1036-1050
Recent observations of coronal loops in EUV wavelengths with the Transition
Region and Coronal Explorer (TRACE) and the Extreme-Ultraviolet Imaging Te
lescope (EIT) on the Solar and Heliospheric Observatory (SOHO) demonstrated
three new results that cannot be explained by most of the existing loop mo
dels: (1) EUV loops are near-isothermal along their coronal segments, (2) t
hey show an overpressure or overdensity compared with the requirements of s
teady state loops with uniform heating, and (3) the brightest EUV loops exh
ibit extended scale heights up to 4 times the hydrostatic scale height. The
se observations cannot be reconciled with the classical RTV (Rosner, Tucker
, & Vaiana) model, they do not support models with uniform heating, and the
y even partially violate the requirements of hydrostatic equilibrium. In th
is study we are fitting for the first time steady state solutions of the hy
drodynamic equations to observed intensity profiles, permitting a detailed
consistency test of the observed temperature T(s) and density profiles n(e)
(s) with steady state models, which was not possible in previous studies ba
sed on scaling laws. We calculate some 500 hydrostatic solutions, which cov
er a large parameter space of loop lengths (L approximate to 4-300 Mm), of
nonuniform heating functions (with heating scale heights in the range of la
mbda (H) approximate to 1-300 Mm), approaching also the limit of uniform he
ating (lambda (H) much greater than L). The parameter space can be subdivid
ed into three regimes, which contain (1) solutions of stably stratified loo
ps, (2) solutions of unstably stratified loops (in the case of short heatin
g scale heights, lambda (H, Mm) approximate to rootL(Mm)), and (3) a regime
in which we find no numerical solutions (when lambda (H), (Mm) less than o
r similar to rootL(Mm)). Fitting the hydrostatic solutions to 41 EUV loops
observed with TRACE (selected by the criterion of detectability over their
entire length), we find that only 30% of the loops are consistent with hydr
ostatic steady state solutions. None of the observed EUV loops is consisten
t with a uniform heating function while in quasi-steady state. Those loops
compatible with a steady state are found to be heated near the footpoints,
with a heating scale height of lambda (H) = 12 +/- 5 Mm, covering a fractio
n lambda (H)/L = 0.2 +/- 0.1 of the loop length. These results support coro
nal heating mechanisms operating in or near the chromosphere and transition
region.