分类： 天文学 >> 天文学 提交时间： 2023-02-19
Nour E. Raouafi
G. Stenborg
D. B. Seaton
H. Wang
J. Wang
C. E. DeForest
S. D. Bale
J. F. Drake
V. M. Uritsky
J. T. Karpen
C. R. DeVore
A. C. Sterling
T. S. Horbury
L. K. Harra
S. Bourouaine
J. C. Kasper
P. Kumar
T. D. Phan
M. Velli
摘要： We present EUV solar observations showing evidence for omnipresent jetting activity driven by small-scale magnetic reconnection at the base of the solar corona. We argue that the physical mechanism that heats and drives the solar wind at its source is ubiquitous magnetic reconnection in the form of small-scale jetting activity (i.e., a.k.a. jetlets). This jetting activity, like the solar wind and the heating of the coronal plasma, are ubiquitous regardless of the solar cycle phase. Each event arises from small-scale reconnection of opposite polarity magnetic fields producing a short-lived jet of hot plasma and Alfv\'en waves into the corona. The discrete nature of these jetlet events leads to intermittent outflows from the corona, which homogenize as they propagate away from the Sun and form the solar wind. This discovery establishes the importance of small-scale magnetic reconnection in solar and stellar atmospheres in understanding ubiquitous phenomena such as coronal heating and solar wind acceleration. Based on previous analyses linking the switchbacks to the magnetic network, we also argue that these new observations might provide the link between the magnetic activity at the base of the corona and the switchback solar wind phenomenon. These new observations need to be put in the bigger picture of the role of magnetic reconnection and the diverse form of jetting in the solar atmosphere.
分类： 天文学 >> 天文学 提交时间： 2023-02-19
N. Gopalswamy
S. Christe
S. F. Fung
Q. Gong
J. R. Gruesbeck
L. K. Jian
S. G. Kanekal
C. Kay
T. A. Kucera
J. E. Leake
L. Li
P. Makela
P. Nikulla
N. L. Reginald
A. Shih
S. K. Tadikonda
N. Viall
L. B. Wilson
S. Yashiro
L. Golub
摘要： We report on a study of the Multiview Observatory for Solar Terrestrial Science (MOST) mission that will provide comprehensive imagery and time series data needed to understand the magnetic connection between the solar interior and the solar atmosphere/inner heliosphere. MOST will build upon the successes of SOHO and STEREO missions with new views of the Sun and enhanced instrument capabilities. This article is based on a study conducted at NASA Goddard Space Flight Center that determined the required instrument refinement, spacecraft accommodation, launch configuration, and flight dynamics for mission success. MOST is envisioned as the next generation great observatory positioned to obtain three-dimensional information of solar wind structures such as coronal mass ejections, stream interaction regions, and the solar wind. The MOST mission consists of 2 pairs of spacecraft located in the vicinity of Sun Earth Lagrange points L4 (MOST1, MOST3) and L5 (MOST2 and MOST4). The spacecraft stationed at L4 (MOST1) and L5 (MOST2) will each carry seven remote-sensing and three in-situ instrument suites. MOST will also carry a novel radio package known as the Faraday Effect Tracker of Coronal and Heliospheric structures (FETCH). FETCH will have polarized radio transmitters and receivers on all four spacecraft to measure the magnetic content of solar wind structures propagating from the Sun to Earth using the Faraday rotation technique. The MOST mission will be able to sample the magnetized plasma throughout the Sun Earth connected space during the mission lifetime over a solar cycle.
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