Clarifying Physical Properties of Magnetic Fields in Sunspots

被引：4

作者：

Obridko, V. N. ^{[1
]}

Katsova, M. M. ^{[2
]}

Sokoloff, D. D. ^{[1
,3
]}

Shelting, B. D. ^{[1
]}

Livshits, I. M. ^{[1
,2
]}

机构：

[1] IZMIRAN, 4 Kaluzhskoe Shosse, Moscow 108840, Russia

[2] Lomonosov Moscow State Univ, Sternberg State Astron Inst, Univ Skij Prosp 13, Moscow 119991, Russia

[3] Moscow MV Lomonosov State Univ, Moscow 119991, Russia

来源：

SOLAR PHYSICS | 2022年 / 297卷 / 10期

关键词：

Sunspots; magnetic fields; penumbra; umbra; AREA; FLUX;

D O I：

10.1007/s11207-022-02066-6

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We demonstrate that the radial magnetic-field component at the outer boundary of the sunspot penumbra is about 550 Mx cm(-2) independent of the sunspot area and the maximum magnetic field in the umbra. The mean magnetic-field intensity in sunspots grows slightly as the sunspot area increases up to 500 - 1000 millionth of visual hemisphere (m.v.h.) and may reach about 900 - 2000 Mx cm(-2). The total magnetic flux weakly depends on the maximum field strength in a sunspot and is determined by the spottedness, i.e. the sunspot number and the total sunspot area; however, the relation between the total flux and the sunspot area is substantially nonlinear. We suggest an explicit parametrization for this relation. The contribution of the magnetic flux associated with sunspots to the total magnetic flux is small, not achieving more than 20% even at the maximum of the solar activity.

引用

页数：11

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