Theoretical brightness temperature profiles of atmospheric pure H 2 rotational quadrupole lines: Jupiter and Uranus

Abstract

With the advent of high-resolution instruments and their use high above most of the telluric water vapor, we can expect to observe the hydrogen pure rotational quadrupole lines at 28, 17, and 12 μm from the atmospheres of the outer planets. We have calculated the best values for the line strengths, pressure-broadening coefficients, diffusion constants, and pressure shifts for these rotational transitions. We have used the collisionally narrowed Galatry profile to calculate brightness temperature line profiles for these H 2 transitions for the outer planets Jupiter and Uranus. We have also included the effect of the H 2 rotational-translational continuum and the NH 3 ν 2 band.