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論文・著書情報
| タイトル |
| 和文: | |
| 英文: | A Comprehensive Study of Short Bursts from SGR1806-20 and SGR1900+14 Detected by HETE-2 |
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| 著者 |
| 和文: |
Nakagawa, Y. E.,
Yoshida, A.,
Hurley, K.,
Atteia, J.-L.,
Maetou, M.,
Tamagawa, T.,
Suzuki, M.,
Yamazaki, T.,
Tanaka, K.,
河合 誠之,
Shirasaki, Y.,
Pelangeon, A.,
Matsuoka, M.,
Vanderspek, R.,
Crew, G. B.,
Villasenor, J. S.,
Sato, R.,
Sugita, S.,
Kotoku, J.,
有元誠,
Pizzichini, G.,
Doty, J. P.,
Ricker, G. R..
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| 英文: |
Nakagawa, Y. E.,
Yoshida, A.,
Hurley, K.,
Atteia, J.-L.,
Maetou, M.,
Tamagawa, T.,
Suzuki, M.,
Yamazaki, T.,
Tanaka, K.,
Kawai, N.,
Shirasaki, Y.,
Pelangeon, A.,
Matsuoka, M.,
Vanderspek, R.,
Crew, G. B.,
Villasenor, J. S.,
Sato, R.,
Sugita, S.,
Kotoku, J.,
Arimoto, M.,
Pizzichini, G.,
Doty, J. P.,
Ricker, G. R..
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| 言語 |
English |
| 掲載誌/書名 |
| 和文: | |
| 英文: | Publications of the Astronomical Society of Japan |
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巻, 号, ページ
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Vol. 59
pp. 653-678
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| 出版年月 |
2007年6月 |
| 出版者 |
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| 会議名称 |
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| 開催地 |
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| DOI |
https://doi.org/10.1093/pasj/59.3.653 |
| アブストラクト |
Temporal and spectral studies of short bursts (≲ a few hundred milliseconds) are presented for the soft gamma repeaters (SGRs) 1806-20 and 1900+14 using the HETE-2 samples. In five years from 2001 to 2005, HETE-2 localized 50 bursts from SGR1806-20 and 5 bursts from SGR1900+14. The cumulative number-intensity distribution of SGR1806-20 in the active year 2004 is well described by a power-law model with an index of −1.1±0.6. It is consistent with previous studies, but burst data taken in other years clearly give a steeper distribution. This may suggest that more energetic bursts could occur more frequently in periods of greater activity. From the data, the spectral evolution during bursts with a time scale of ≳ 20ms does not seem to be common in the HETE-2 sample. The spectra of all short bursts are well reproduced by a two blackbody function with temperatures of ˜ 4 and ˜ 11keV. From a timing analysis to the SGR1806-20 data, a time lag of 2.2±0.4ms is found between the 30-100keV and 2-10keV radiation bands. This may imply (1) a very rapid spectral softening and energy reinjection, (2) diffused (elongated) emission plasma along the magnetic field lines in pseudo-equilibrium with multi-temperatures, or (3) a separate (located at ≲ 700km) emission region of a softer component (say, ˜ 4keV), which could be reprocessed X-rays by higher energy (≳ 11keV) photons from an emission region near the stellar surface. |
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