Venera 11 and Venera 12 observations of e.u.v. emissions from the upper atmosphere of Venus

Far‐Ultraviolet Spectroscopy of Venus and Mars at 4 A Resolution with the Hopkins Ultraviolet Telescope on Astro‐2

“…Moreover, since the Ðrst-order spectral range of HUT extended to wavelengths as short as 830 the observations of Venus enabled the resolution of A , the identity of the emissions recorded in the narrowband photometric channels of the V enera 11 and 12 EUV instruments that had been interpreted in terms of analog terrestrial spectra (Bertaux et al 1981). This paper presents the HUT disk spectra of Venus and Mars together with the spectral identiÐcations and the disk-averaged brightnesses.…”

“…A thorough review of this subject is given by Paxton & Anderson (1992). Once the emitting species were known, narrowband polychromators were developed and Ñown on missions such as Mariner 10 (Broadfoot et al 1974) and V enera 11 and 12 (Bertaux et al 1981), although the interpretation of the data from these instruments was far from unambiguous. With Mariner 6, 7, and 9, Ñown to Mars in the early 1970s, and Pioneer V enus Orbiter, launched to Venus in 1978, ultraviolet spectrometers were included in the payloads and provided modest spectral resolution.…”

Astrophysics in 1996

“…Stem et al (1996) found emission features of N I, N n, and N 2 and CO. Furthermore, they cleared up an apparent mismatch between in situ and remote sensing measurements which previously had reported detection of Ar (Bertaux et al 1981). Interpretation of Venera 11/12 measurements implied 100 times the abundance of argon compared to predictions from the Pioneer Venus entry probe (Hoffman et al 1980).…”

EUV spectroscopy of the Venus dayglow with UVIS on Cassini

“…It was 91 R in the HUT spectrum near solar minimum when the F 10.7 cm index 203 was 82. The Venera 11 measurements (Bertaux et al, 1981) gave a maximum disc value of 204 156 R for a moderate F 10.7 index of 138, with 20% variations observed across the disc. The 205 variation of this emission across the disc and its comparison with model calculations will be 206 discussed in further details in section 5.…”