Solar wind outflow and the chromospheric magnetic network
Solar wind outflow and the chromospheric magnetic network
复制标题
DOI：
10.1126/science.283.5403.810
复制
发表时间：
1999-02
期刊：
影响因子：
56.9
通讯作者：
Donald M. Hassler;I. Dammasch;P. Lemaire;Pål Brekke;W. Curdt;Helen E. Mason;Jean-Claude Vial
中科院分区：
文献类型：
--
作者：
Donald M. Hassler;I. Dammasch;P. Lemaire;Pål Brekke;W. Curdt;Helen E. Mason;Jean-Claude Vial
最近利用太阳和日光层观测站（SOHO）航天器观测了冕洞（开放的日冕磁场区域）中的外流速度。Ne 7+在日冕底部形成的770埃明亮共振线的速度图显示出流出速度与色球磁网络结构之间的关系，表明太阳风植根于色球磁网络结构的底部，从沿着边界和边界交叉点的局部区域发出。这种与色球磁网络的明显关系和相对较大的外流速度特征将有助于了解日冕底部和太阳风源区的复杂结构和动力学。
Observations of outflow velocities in coronal holes (regions of open coronal magnetic field) have recently been obtained with the Solar and Heliospheric Observatory (SOHO) spacecraft. Velocity maps of Ne7+ from its bright resonance line at 770 angstroms, formed at the base of the corona, show a relationship between outflow velocity and chromospheric magnetic network structure, suggesting that the solar wind is rooted at its base to this structure, emanating from localized regions along boundaries and boundary intersections of magnetic network cells. This apparent relation to the chromospheric magnetic network and the relatively large outflow velocity signatures will improve understanding of the complex structure and dynamics at the base of the corona and the source region of the solar wind.