A search for the tritium hyperfine line from nearby stars |
| |
| Institution: | 1. National Institute for Fusion Science, 322-6 Oroshi-cho, Toki, Gifu, 509-5292, Japan;2. JGC CORPORATION, 2-3-1, Minato Mirai, Nishi-ku, Yokohama, Kanagawa 220-0012, Japan;3. SOKENDAI (The Graduate University for Advanced Studies), 322-6 Oroshi-cho, Toki, Gifu 509-5292, Japan;1. Physical Chemistry Division, CSIR-National Chemical Laboratory, Pune 411008, India;2. Departmento de Química, CINVESTAV, Avenida Instituto Politécnico Nacional, 2508 A. P. 14-740, México, DF 07000, Mexico;1. National Institute for Fusion Science, National Institutes for Natural Sciences, Toki 509-5292, Japan;2. SOKENDAI (The Graduate University for Advanced Studies), 322-6 Oroshi-cho, Toki 509-5292, Japan;3. Kyushu University, Kasuga 816-8580, Japan;4. Kindai University, Osaka 577-8502, Japan;5. Shizuoka University, Shizuoka 422-8529, Japan;6. Ibaraki University, Mito 310-8512, Japan |
| |
| Abstract: | A search for the tritium hyperfine line at 1516 MHz from 108 assorted astronomical objects, with emphasis on 53 nearby stars, was conducted in June 1983. All stars within 20 light-years visible from the 26-m telescope at Hat Creek Radio Observatory were examined using 256 4883-Hz channels. Twelve stars were also examined using 1024 76-Hz channels. The wideband- and narrowband-channel observations achieved sensitivities of 5–14 × 10−24 W/m2/channel and 0.7–2 × 10−24 W/m2/channel, respectively. No detections were made. The tritium frequency is highly attractive for SETI work because the isotope is cosmically rare and the tritium hyperfine line is centered in the SETI waterhole region of the terrestrial microwave window. In addition to beacon signals, tritium hyperfine emission may occur as a byproduct of extensive nuclear fusion energy production by extraterrestrial civilizations. |
| |
| Keywords: | |
| 本文献已被 ScienceDirect 等数据库收录！ |
|
