[en] We use numerical computations of stationary solar coronal loop atmospheres to extend previous analytical work by Rosner, Tucker, and Vaiana. The two classes of loops examined include; (i) symmetric loops with a temperature maximum at the top, but now having length L greater than the pressure scale height s/sub p/, and (ii) loops which have local temperature mimimum at the top. For the first class we find new scaling laws, similar to those found by Rosner, Tucker, and Vaiana, which relate the base pressure p₀ and loop length to the base heating E₀, the heating deposition scale height s/sub H/, and the pressure scale height: Troughly-equal1.4 x 10³(p₀L)/sup 0.33/ exp[-0.04L(2/s/sub H/+1/s/sub p/)] and E₀roughly-equal10⁵p₀ /sup 1.17/L/sup -0.83/ exp [0.5L(1/s/sub H/-1/s/sub p/)]. Loop for which L is greater than approx.2 to 3 times the pressure scale height do not have stable solutions unless they have a temperature minimum at the top. Computed models with a temperature inversion at the top are allowed in a wider range of s/sub H/ values than are loops with T/sub max/ at the top. We discuss these results in relation to observations showing a dependence of prominence formation and stability on the state of evolution of magnetic structures, and we suggest a general scenario for the understanding of loop evolution from emergence in active regions through the large-scale structure phase to opening in coronal holes