Height variations of auroral hiss observed by S-310JA-11 and 12 rockets

• Main Authors: Isamu Nagano, Eiko Yamamoto, Kozo Hashimato, Iwane Kimura, Hisao Yamagishi, Hiroshi Fukunishi
• Format: Report
• Language: English
• Published: Department of Electrical and Computer Engineering, Kanazawa University/Department of Electrical and Computer Engineering, Kanazawa University/Department of Electrical Engineering, Tokyo Denki University/Department of Electrical Engineering II, Kyoto University/National Institute of Polar Research/Upper Atmosphere and Space Research Laboratory, Faculty of Science, Tohoku University 1988
• Subjects: Syowa Station; Antarc*; Antarctica
• Online Access: https://nipr.repo.nii.ac.jp/?action=repository_uri&item_id=4031; http://id.nii.ac.jp/1291/00004031/; https://nipr.repo.nii.ac.jp/?action=repository_action_common_download&item_id=4031&item_no=1&attribute_id=18&file_no=1

Electromagnetic waves constructing auroral hiss in the VLF range were observed by the S-310JA-11 and -12 rockets launched into a quiet auroral arc and into a breakup aurora respectively, from Syowa Station in Antarctica. An altitude profile of the electric field intensity, which peaked at an altitude of 90km was observed by the S-310JA-12 rocket in the frequency range less than 5kHz. An estimation of the source location of the auroral hiss was made with the altitude profile of the hiss intensity calculated by the full wave analysis so as to agree with those observed especially around the altitude of 90km. It was found that the auroral hiss is most likely to be generated at an altitude about 700km or less. On the other hand, the absolute intensity of the auroral hiss at a frequency of 4kHz observed by the rocket, which was 9.4×10^<-5> V/m/√<Hz>, was much stronger, by about 50dB, than that observed at Syowa Station. This means that the k-vector direction of the auroral hiss actually observed by the rocket lay outside the transmission cone, so that the auroral hiss could reach Syowa Station with very week intensity.