Murabito Mariarita, Stangalini Marco, Laming J Martin, Baker Deborah, To Andy S H, Long David M, Brooks David H, Jafarzadeh Shahin, Jess David B, Valori Gherardo
INAF Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Capodimonte, 80131 Napoli, Italy.
ASI - Italian Space Agency, Via del Politecnico, s.n.c 00133-Rome, Italy.
Phys Rev Lett. 2024 May 24;132(21):215201. doi: 10.1103/PhysRevLett.132.215201.
We investigate the propagation of Alfvén waves in the solar chromosphere, distinguishing between upward and downward propagating waves. We find clear evidence for the reflection of waves in the chromosphere and differences in propagation between cases with waves interpreted to be resonant or nonresonant with the overlying coronal structures. This establishes the wave connection to coronal element abundance anomalies through the action of the wave ponderomotive force on the chromospheric plasma, which interacts with chromospheric ions but not neutrals, thereby providing a novel mechanism of ion-neutral separation. This is seen as a "first ionization potential effect" when this plasma is lifted into the corona, with implications elsewhere on the Sun for the origin of the slow speed solar wind and its elemental composition.
我们研究了阿尔文波在太阳色球层中的传播，区分了向上和向下传播的波。我们发现了色球层中波反射的明确证据，以及被解释为与上层日冕结构共振或非共振的波在传播上的差异。这通过波的有质动力作用于色球层等离子体，建立了波与日冕元素丰度异常的联系，该等离子体与色球层离子相互作用，但不与中性粒子相互作用，从而提供了一种新的离子-中性粒子分离机制。当这种等离子体被提升到日冕中时，这被视为一种“第一电离势效应”，对太阳其他地方低速太阳风的起源及其元素组成具有启示意义。
