The satellite's orbit has perigee and apogee distances of 9000 km and 11000 km from the center of the Earth, respectively, when adding Earth's radius (6500 km) to their heights above the surface. The semi-major axis (a) can be computed as the average of these distances:
\[a=\frac{9000\text{ km}+11000\text{ km}}{2}=10000\text{ km}\]
The eccentricity (e) of the orbit is defined as:
\[e=\frac{\text{apogee distance}-\text{perigee distance}}{\text{apogee distance}+\text{perigee distance}}\]
Substituting the distance values:
\[e=\frac{11000-9000}{11000+9000}=\frac{2000}{20000}=0.1\]

At a particular temperature T, Planck's energy density of black body radiation in terms of frequency is \(\rho_T(\nu) = 8 \times 10^{-18} \text{ J/m}^3 \text{ Hz}^{-1}\) at \(\nu = 3 \times 10^{14}\) Hz. Then Planck's energy density \(\rho_T(\lambda)\) at the corresponding wavelength (\(\lambda\)) has the value \rule{1cm}{0.15mm} \(\times 10^2 \text{ J/m}^4\). (in integer)
[Speed of light \(c = 3 \times 10^8\) m/s]
(Note: The unit for \(\rho_T(\nu)\) in the original problem was given as J/m³, which is dimensionally incorrect for a spectral density. The correct unit J/(m³·Hz) or J·s/m³ is used here for the solution.)