Auroral Spiral Structure Formation Through Magnetic Reconnection in the Auroral Acceleration Region. Issue 18 (16th September 2022)

• Record Type: Journal Article
• Authors: Huang, Kai; Liu, Yi‐Hsin; Lu, Quanming; Hu, Zejun; Lynch, Kristina A.; Hesse, Michael; Vaivads, Andris; Yang, Huigen
• Is Part Of: Geophysical research letters. Volume 49:Issue 18(2022)
• Page Start: n/a
• Page End: n/a
• Publication Date: 2022-09-16
• Subjects: Geophysics -- Periodicals; Planets -- Periodicals; Lunar geology -- Periodicals; 550
• DOI: 10.1029/2022GL100466
• Languages: English
• ISSNs: 0094-8276

Abstract

Abstract: Auroral spiral is one of the auroral vortex structures. Here, we propose a model to explain the formation of auroral spiral structure based on three‐dimensional particle‐in‐cell simulations. In our model, an auroral arc develops through precipitations of electrons accelerated during magnetic reconnection in the auroral acceleration region. The arc morphology at low altitudes can be modified by electron‐scale magnetic flux ropes, which are generated through secondary oblique tearing modes in the intensified current sheet along one particular branch of the primary reconnection separatrices. The resulting vortex structures agree well with high‐resolution observations of auroral spirals. We find that the rotational sense of these spirals is determined by electron kinetic processes and controlled by the guide field direction. Our study further suggests that when the field‐aligned length of the auroral acceleration region is shorter than a critical length, these auroral spiral structures will not form. Plain Language Summary: Discrete aurorae, usually displayed as auroral arcs, are universal phenomena in the ionosphere of the Earth and other planets, and are generated by precipitations of electrons from the magnetosphere, ionosphere, and solar wind. Spirals, as frequently observed vortex structures in arcs, have drawn great attention. The formation of auroral spirals is considered to be related to the magnetosphere‐ionosphere coupling process during both magnetically active and quiet times. However, how the auroral spirals develop is still an open question. It is suggested that magnetic reconnection occurs in the auroral acceleration region, typically above ∼4, 000 km altitude in the field‐aligned current sheet. Using kinetic simulations, we study the role of magnetic reconnection in the formation of auroral spirals. Key Points: Auroral acceleration is modeled by considering magnetic reconnection in the field‐aligned current sheet Periodic spiral structures can develop from an auroral arc modified by secondary oblique tearing instability The characteristics of the spiral structures in our simulation agree well with observation