| アイテムタイプ |
itemtype_ver1(1) |
| 公開日 |
2025-08-28 |
| タイトル |
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タイトル |
Comparison of Polar Magnetic Fields Derived from MILOS and MERLIN Inversions with Hinode/SOT-SP Data |
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言語 |
en |
| 著者 |
Kubo, Masahito
Shiota, Daikou
Katsukawa, Yukio
Shimojo, Masumi
Orozco Suárez, David
Nitta, Nariaki
DeRosa, Marc
Centeno, Rebecca
Iijima, Haruhisa
Matsumoto, Takuma
Masuda, Satoshi
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| アクセス権 |
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アクセス権 |
embargoed access |
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アクセス権URI |
http://purl.org/coar/access_right/c_f1cf |
| 権利 |
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|
権利情報 |
This version of the article has been accepted for publication, after peer review (when applicable) and is subject to Springer Nature’s AM terms of use, but is not the Version of Record and does not reflect post-acceptance improvements, or any corrections. The Version of Record is available online at: http://dx.doi.org/10.1007/s11207-025-02487-z |
|
言語 |
en |
| 内容記述 |
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内容記述タイプ |
Abstract |
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内容記述 |
The detailed investigation of the polar magnetic field and its time evolution is one of the major achievements of Hinode. Precise measurements of the polar magnetic field are essential for understanding the solar cycle, as they provide important constraints for identifying the source regions of the solar wind. The Spectropolarimeter (SP) of the Solar Optical Telescope (SOT) on board Hinode has been the instrument best suited to make such measurements. In this study, we compare the SOT-SP data for the polar regions, processed using two representative Milne-Eddington inversion codes, MILOS and MERLIN. These codes are applied to the same level-1 SOT-SP data, and the same disambiguation algorithm is used on the maps that go through the two inversions. We find that the radial magnetic-flux density (the magnetic-flux density with respect to the local vertical) provided by the MERLIN inversion tends to be approximately 7% – 10% larger than that obtained from the MILOS inversion. The slightly higher radial magnetic-flux density from MERLIN appears to be common to the polar magnetic fields observed at different phases of the solar cycle. When MILOS is run with the same scattered-light profile and the same magnetic filling factor that are derived with the MERLIN inversion, the radial magnetic-flux density derived from the two inversions is almost the same. We attribute the difference in the radial magnetic-flux density to different filling factors adopted by the two inversions, based on whether the scattered-light profiles are assumed to be the Stokes I profiles averaged over the neighboring pixels or over the entire field of view. The relationship between the radial magnetic-flux density and magnetic filling factor could be more complex in the polar (limb) observations due to the possible contributions of the transverse magnetic-field component to the estimation of the radial magnetic-flux density. |
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言語 |
en |
| 出版者 |
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出版者 |
Springer |
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言語 |
en |
| 言語 |
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|
言語 |
eng |
| 資源タイプ |
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資源タイプresource |
http://purl.org/coar/resource_type/c_6501 |
|
タイプ |
journal article |
| 出版タイプ |
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出版タイプ |
AM |
|
出版タイプResource |
http://purl.org/coar/version/c_ab4af688f83e57aa |
| 関連情報 |
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|
関連タイプ |
isVersionOf |
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|
識別子タイプ |
DOI |
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|
関連識別子 |
https://doi.org/10.1007/s11207-025-02487-z |
| 収録物識別子 |
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収録物識別子タイプ |
PISSN |
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収録物識別子 |
0038-0938 |
| 書誌情報 |
en : Solar Physics
巻 300,
p. 69,
発行日 2025-05-23
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| ファイル公開日 |
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日付 |
2026-05-23 |
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日付タイプ |
Available |
2505_19468v1.pdf (2 MB)
