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SEA AND HISS ASSOCIATED WITH GREAT BURSTS OF SOLAR RADIO EMISSION IN NOVEMBER 1960
http://hdl.handle.net/2237/21709
http://hdl.handle.net/2237/217098df9eebd-7379-4481-97dd-65373eb3201c
| 名前 / ファイル | ライセンス | アクション |
|---|---|---|
proria_8_1.pdf (2.3 MB)
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| アイテムタイプ | 紀要論文 / Departmental Bulletin Paper(1) | |||||
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| 公開日 | 2015-04-24 | |||||
| タイトル | ||||||
| タイトル | SEA AND HISS ASSOCIATED WITH GREAT BURSTS OF SOLAR RADIO EMISSION IN NOVEMBER 1960 | |||||
| 言語 | en | |||||
| 著者 |
KAMADA, TETSUO
× KAMADA, TETSUO× OUTSU, JINSUKE× IWAI, AKIRA |
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| アクセス権 | ||||||
| アクセス権 | open access | |||||
| アクセス権URI | http://purl.org/coar/access_right/c_abf2 | |||||
| 抄録 | ||||||
| 内容記述タイプ | Abstract | |||||
| 内容記述 | On 11th, 12th, 14th and 15th November 1960, very intense outbursts of Solar radio emission occurred successively. Three of these, except the one on 12th, were observed at Toyokawa on a frequency region from 9.4 Gc/s to 1000 Mc/s. Each of these is a composed burst composed of 1st and 2nd phase of em wave burst and dm wave burst. It was found that the source of polarized component at 9.4 Gc/s moved appreciably during the 2nd phase of em wave burst, though the center of brightness was left unmoved. This phenomenon suggests the existence of two different kinds of emission mechanisms on cm wavelength region. Mode IV SEA was clearly observed at three frequencies of 10, 21 and 27 Kc/s on 11th, 14th and 15th November. It seems quite probable that SEA is closely correlated with the flare or the 1st phase of cm wave burst and not with the other parts of the burst at microwave frequencies. The type of SEA seems to be largely connected with the shape of intensity variation of cm wave burst. The duration of SEA seems to be proportional to the intensity of the flare. The lower the frequency, the later the time of maximum, which can be explained by the difference o f time necessary to reach the state of saturation of reflection coefficient in D region. The turn-over frequency of positive and negative enhancement seems to be indefinite and to lie within 14-18 Kc/s. Associated with these solar radio bursts, a generation of several series of hiss was confirmed at Wakkanai for the first time. The first series commenced at 1120 on 13th, lagging about 56 hours after the first burst. The second series, though uncertain, occurred intermittently from 1220 to 2350 on 15th. These observations indicate that the hiss is detectable at latitudes as low as about 35 degrees during a period of high sunspot activity. | |||||
| 言語 | en | |||||
| 出版者 | ||||||
| 出版者 | The Research Institute of Atmospherics, Nagoya University | |||||
| 言語 | en | |||||
| 言語 | ||||||
| 言語 | eng | |||||
| 資源タイプ | ||||||
| 資源 | http://purl.org/coar/resource_type/c_6501 | |||||
| タイプ | departmental bulletin paper | |||||
| 出版タイプ | ||||||
| 出版タイプ | VoR | |||||
| 出版タイプResource | http://purl.org/coar/version/c_970fb48d4fbd8a85 | |||||
| ISSN（print） | ||||||
| 収録物識別子タイプ | PISSN | |||||
| 収録物識別子 | 0077-264X | |||||
| 書誌情報 |
en : Proceedings of the Research Institute of Atmospherics, Nagoya University 巻 8, p. 1-16, 発行日 1961-06-15 |
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| 著者版フラグ | ||||||
| 値 | publisher | |||||
| URI | ||||||
| 識別子 | http://hdl.handle.net/2237/21709 | |||||
| 識別子タイプ | HDL | |||||
