On the generation of solar spicules and Alfvenic waves

被引：167

作者：

Martinez-Sykora, J. ^{[1
,2
]}

De Pontieu, B. ^{[2
,3
]}

Hansteen, V. H. ^{[2
,3
]}

van der Voort, L. Rouppe ^{[3
]}

Carlsson, M. ^{[3
]}

Pereira, T. M. D. ^{[3
]}

机构：

[1] Bay Area Environm Res Inst, Petaluma, CA 94952 USA

[2] Lockheed Martin Solar & Astrophys Lab LMSAL, Palo Alto, CA 94304 USA

[3] Univ Oslo, Inst Theoret Astrophys, POB 1029, N-0315 Oslo, Norway

来源：

SCIENCE | 2017年 / 356卷 / 6344期

基金：

欧洲研究理事会;

关键词：

REGION; SIMULATION; CORONA; POWER;

D O I：

10.1126/science.aah5412

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：

In the lower solar atmosphere, the chromosphere is permeated by jets known as spicules, in which plasma is propelled at speeds of 50 to 150 kilometers per second into the corona. The origin of the spicules is poorly understood, although they are expected to play a role in heating the million-degree corona and are associated with Alfvenic waves that help drive the solar wind. We compare magnetohydrodynamic simulations of spicules with observations from the Interface Region Imaging Spectrograph and the Swedish 1-m Solar Telescope. Spicules are shown to occur when magnetic tension is amplified and transported upward through interactions between ions and neutrals or ambipolar diffusion. The tension is impulsively released to drive flows, heat plasma (through ambipolar diffusion), and generate Alfvenic waves.

引用

页码：1269 / +

页数：4

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