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The Quiescent Counterpart of the Soft Gamma-Ray Repeater SGR 0526-66
https://doi.org/10.24517/00010232
https://doi.org/10.24517/00010232ed2f0e1a-9043-4068-91b6-5ccb97d00d50
| 名前 / ファイル | ライセンス | アクション |
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SC-PR-YONETOKU-D-948.pdf (180.2 kB)
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| Item type | 学術雑誌論文 / Journal Article(1) | |||||||||
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| 公開日 | 2017-10-03 | |||||||||
| タイトル | ||||||||||
| タイトル | The Quiescent Counterpart of the Soft Gamma-Ray Repeater SGR 0526-66 | |||||||||
| 言語 | ||||||||||
| 言語 | eng | |||||||||
| 資源タイプ | ||||||||||
| 資源タイプ識別子 | http://purl.org/coar/resource_type/c_6501 | |||||||||
| 資源タイプ | journal article | |||||||||
| ID登録 | ||||||||||
| ID登録 | 10.24517/00010232 | |||||||||
| ID登録タイプ | JaLC | |||||||||
| 著者 |
Kulkarni, S. R.
× Kulkarni, S. R.× Kaplan, D. L.× Marshall, H. L.× Frail, D. A.× Murakami, Toshio× Yonetoku, Daisuke |
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| 著者別表示 |
村上, 敏夫
× 村上, 敏夫
× 米德, 大輔
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| 提供者所属 | ||||||||||
| 内容記述タイプ | Other | |||||||||
| 内容記述 | 金沢大学大学院自然科学研究科物理学 | |||||||||
| 書誌情報 |
The Astrophysical Journal 巻 58, 号 2, p. 948-954, 発行日 2003-03-10 |
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| ISSN | ||||||||||
| 収録物識別子タイプ | ISSN | |||||||||
| 収録物識別子 | 0004-637X | |||||||||
| NCID | ||||||||||
| 収録物識別子タイプ | NCID | |||||||||
| 収録物識別子 | AA00553242 | |||||||||
| DOI | ||||||||||
| 関連タイプ | isVersionOf | |||||||||
| 識別子タイプ | DOI | |||||||||
| 関連識別子 | 10.1086/346110 | |||||||||
| 出版者 | ||||||||||
| 出版者 | American Astronomical Society | |||||||||
| 抄録 | ||||||||||
| 内容記述タイプ | Abstract | |||||||||
| 内容記述 | It is now commonly believed that soft gamma-ray repeaters (SGRs) and anomalous X-ray pulsars (AXPs) are magnetars - neutron stars powered by their magnetic fields. However, what differentiates these two seemingly dissimilar objects is, at present, unknown. We present Chandra observations of RX J052600.3-660433, the quiescent X-ray counterpart of SGR 0526-66, famous for the intense burst of 1979 March 5. The source is unresolved at the resolution of Chandra. Restricting observations to a period range around 8 s, the period noted in the afterglow of the burst of 1979 March 5, we find evidence for a similar periodicity in two epochs of data obtained 20 months apart. The secular period derivative based on these two observations is 6.6(5) × 10 -11 s s-1, similar to the period derivatives of the magnetars. As is the case with other magnetars, the spectrum is best fitted by a combination of a blackbody and a power law. However, quite surprisingly, the photon index of the power-law component is Γ ∼ 3 - intermediate to those of AXPs and SGRs. This continuum of Γ led us to suggest that the underlying physical parameter that differentiates SGRs from AXPs is manifested in the power-law component. Two decades ago, SGR 0526-66 was a classical SGR, whereas now it behaves like an AXP. Thus, it is possible that the same object cycles between the SGR and AXP states. We speculate that the main difference between AXPs and SGRs is the geometry of the B fields, and this geometry is time dependent. Finally, given the steep spectrum of RX J052600.3-660433, the total radiated energy of RX J052600.3-660433 can be much higher than traditionally estimated. If this energy is supplied by the decay of the magnetic field, then the inferred B field of RX J052600.3-660433 is in excess of 1015 G, the traditional value for magnetars. Independent of this discussion, there could well be a class of neutron stars, 1014 G ≲ B ≲ 1015 G, which are neither radio pulsars nor magnetars. | |||||||||
| 著者版フラグ | ||||||||||
| 出版タイプ | AM | |||||||||
| 出版タイプResource | http://purl.org/coar/version/c_ab4af688f83e57aa | |||||||||
