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  1. J-6. 理工研究域附属先端宇宙理工学研究センター
  2. j-6 10. 学術雑誌掲載論文
  3. 1. 査読済論文

The Quiescent Counterpart of the Soft Gamma-Ray Repeater SGR 0526-66

https://doi.org/10.24517/00010232
https://doi.org/10.24517/00010232
ed2f0e1a-9043-4068-91b6-5ccb97d00d50
名前 / ファイル ライセンス アクション
SC-PR-YONETOKU-D-948.pdf SC-PR-YONETOKU-D-948.pdf (180.2 kB)
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Item type 学術雑誌論文 / Journal Article(1)
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.

WEKO 15329

Kulkarni, S. R.

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Kaplan, D. L.

× Kaplan, D. L.

WEKO 15330

Kaplan, D. L.

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Marshall, H. L.

× Marshall, H. L.

WEKO 15331

Marshall, H. L.

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Frail, D. A.

× Frail, D. A.

WEKO 15332

Frail, D. A.

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Murakami, Toshio

× Murakami, Toshio

WEKO 175
e-Rad 60092350
研究者番号 60092350

Murakami, Toshio

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Yonetoku, Daisuke

× Yonetoku, Daisuke

WEKO 15034
e-Rad 40345608
金沢大学研究者情報 40345608
研究者番号 40345608

Yonetoku, Daisuke

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著者別表示 村上, 敏夫

× 村上, 敏夫

村上, 敏夫

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米德, 大輔

× 米德, 大輔

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
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
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