Science. 1986 Jul 4;233(4759):70-4. doi: 10.1126/science.233.4759.70.
The infrared interferometer spectrometer (IRIS) on Voyager 2 recorded thermal emission spectra of Uranus between 200 and 400 cm(-1) and of Miranda and Ariel between 200 and 500 cm(-1) with a spectral resolution of 4.3 cm(-1). Reflected solar radiation was also measured with a single-channel radiometer sensitive in the visible and near infrared. By combining IRIS spectra with radio science results, a mole fraction for atmospheric helium of 0.15 +/- 0.05 (mass fraction, 0.26 +/- 0.08) is found. Vertical temperature profiles between 60 and 900 millibars were derived from average polar and equatorial spectra. Temperatures averaged over a layer between 400 to 900 millibars show nearly identical values at the poles and near the equator but are 1 or 2 degrees lower at mid-latitudes in both hemispheres. The cooler zone in the southern hemisphere appears darker in reflected sunlight than the adjacent areas. An upper limit for the effective temperature of Uranus is 59.4 kelvins. Temperatures of Miranda and Ariel at the subsolar point are 86 +/- 1 and 84 +/- 1 kelvins, respectively, implying Bond albedos of 0.24 +/- 0.06 and 0.31 +/- 0.06, respectively. Estimates of phase integrals suggest that these satellites have unusual surface microstructure.
航海者 2 号上的红外干涉光谱仪（IRIS）在 200 到 400 厘米-1 之间记录了天王星的热辐射光谱，在 200 到 500 厘米-1 之间记录了 Miranda 和 Ariel 的热辐射光谱，光谱分辨率为 4.3 厘米-1。还使用一个在可见和近红外波段敏感的单通道辐射计测量了反射的太阳辐射。通过将 IRIS 光谱与射电科学结果相结合，发现大气氦的摩尔分数为 0.15 ± 0.05（质量分数为 0.26 ± 0.08）。从平均极区和赤道区光谱得出了 60 到 900 毫巴之间的垂直温度廓线。在 400 到 900 毫巴之间的层平均温度在极区和近赤道处几乎相同，但在两个半球的中纬度处低 1 或 2 度。南半球较冷的区域在反射阳光中比相邻区域显得更暗。天王星的有效温度上限为 59.4 开尔文。在太阳下点处 Miranda 和 Ariel 的温度分别为 86 ± 1 和 84 ± 1 开尔文，这意味着它们的邦德反照率分别为 0.24 ± 0.06 和 0.31 ± 0.06。相位积分的估计表明这些卫星具有不寻常的表面微观结构。
