Global maps of the magnetic field in the solar corona

被引：111

作者：

Yang, Zihao ^{[1
]}

Bethge, Christian ^{[2
,3
]}

Tian, Hui ^{[1
,4
]}

Tomczyk, Steven ^{[3
]}

Morton, Richard ^{[5
]}

Del Zanna, Giulio ^{[6
]}

McIntosh, Scott W. ^{[3
]}

Karak, Bidya Binay ^{[7
]}

Gibson, Sarah ^{[3
]}

Samanta, Tanmoy ^{[8
,9
]}

He, Jiansen ^{[1
]}

Chen, Yajie ^{[1
,10
]}

Wang, Linghua ^{[1
]}

机构：

[1] Peking Univ, Sch Earth & Space Sci, Beijing 100871, Peoples R China

[2] Univ Space Res Assoc, Huntsville, AL 35805 USA

[3] Natl Ctr Atmospher Res, High Altitude Observ, Pob 3000, Boulder, CO 80307 USA

[4] Chinese Acad Sci, Natl Astron Observ, Key Lab Solar Act, Beijing 100012, Peoples R China

[5] Northumbria Univ, Dept Math Phys & Elect Engn, Newcastle Upon Tyne NE1 8ST, Tyne & Wear, England

[6] Univ Cambridge, Ctr Math Sci, Dept Appl Math & Theoret Phys, Cambridge CB3 0WA, England

[7] Banaras Hindu Univ, Indian Inst Technol, Dept Phys, Varanasi 221005, Uttar Pradesh, India

[8] George Mason Univ, Dept Phys & Astron, Fairfax, VA 22030 USA

[9] Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA

[10] Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany

来源：

SCIENCE | 2020年 / 369卷 / 6504期

关键词：

SUFFICIENT ENERGY; WAVE-PROPAGATION; ALFVENIC WAVES; POWER; SEISMOLOGY; FLUX;

D O I：

10.1126/science.abb4462

中图分类号：

O [数理科学和化学]; P [天文学、地球科学]; Q [生物科学]; N [自然科学总论];

学科分类号：

07 ; 0710 ; 09 ;

摘要：

Understanding many physical processes in the solar atmosphere requires determination of the magnetic field in each atmospheric layer. However, direct measurements of the magnetic field in the Sun's corona are difficult to obtain. Using observations with the Corona! Multi-channel Polarimeter, we have determined the spatial distribution of the plasma density in the corona and the phase speed of the prevailing transverse magnetohydrodynamic waves within the plasma. We combined these measurements to map the plane-of-sky component of the global coronal magnetic field. The derived field strengths in the corona, from 1.05 to 1.35 solar radii, are mostly 1 to 4 gauss. Our results demonstrate the capability of imaging spectroscopy in coronal magnetic field diagnostics.

引用

页码：694 / +

页数：20

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