A 17 June 2011 polar jet and its presence in the background solar wind

NCUIR > College of Earth Sciences > DEPARTMENT OF SPACE SCIENCE AND ENGINEERING > journal & Dissertation > Item 987654321/102090

Please use this identifier to cite or link to this item: https://ir.lib.ncu.edu.tw/handle/987654321/102090

Title:	A 17 June 2011 polar jet and its presence in the background solar wind
Authors:	楊雅惠;Yu, H.‐S.;Jackson, B.V.;Yang, Y.‐H.;Chen, N.‐H.;Buffington, A.;Hick, P. P.
Contributors:	地球科學學院太空科學與工程學系
Keywords:	Coronagraphs;coronal hole;Coronas;Ejection;Geophysics;High speed;Instrumentation;Interplanetary scintillation;Magnetic fields;Magnetic flux;Observatories;Polar environments;polar jet;Polar regions;Reconstruction;Solar activity;Solar corona;Solar observatories;Solar physics;Solar wind;Solar wind acceleration;Solar wind velocity;Spacecraft;Spectrometry;Tracking
Date:	2016-06-01
Issue Date:	2026-04-23 11:02:42 (UTC+8)
Publisher:	Wiley-Blackwell;Washington: Blackwell Publishing Ltd
Abstract:	摘要： High‐speed jet responses in the polar solar wind are enigmatic. Here we measure a jet response that emanates from the southern polar coronal hole on 17 June 2011 at the extreme speed of over 1200 km/s. This response was recorded from the Sun‐Earth line in Solar Dynamics Observatory/Atmospheric Imaging Assembly (SDO/AIA) and Large Angle and Spectrometric Coronagraph/C2 and both Solar TErrestrial RElations Observatory Extreme Ultraviolet Imager and COR2 coronagraphs when the three spacecraft were situated ~90° from one another. These certify the coronal 3‐D location of the response that is associated with an existing solar plume structure and show its high speed to distances of over 14 RS. This jetting is associated with magnetic flux changes in the polar region as measured by the SDO/Helioseismic and Magnetic Imager instrumentation over a period of several hours. The fastest coronal response observed can be tracked to a time near the period of greatest flux changes and to the onset of the brightest flaring in AIA. This high‐speed response can be tracked directly as a small patch of outward moving brightness in coronal images as in Yu et al. (2014) where three slower events were followed from the perspective of Earth. This accumulated jet response has the largest mass and energy we have yet seen in 3‐D reconstructions from Solar Mass Ejection Imager observations, and its outward motion is certified for the first time using interplanetary scintillation observations. This jet response is surrounded by similar high‐speed patches, but these are smoothed out in Ulysses polar measurements, we speculate about how these dynamic activities relate to solar wind acceleration. Key Points An extreme speed jetting feature is observed from three spacecraft perspective views The jetting response is shown for the first time in both IPS and SMEI 3‐D reconstructions The 3‐D relationship between surface brightness and the jet response, as well as the associated field changes, is documented 出版者： Washington: Blackwell Publishing Ltd 出版日期： 2016-06 出處： Journal of geophysical research : Space physics (2013 - Present), 2016-06, Vol.121 (6), p.4985-4997 資源來源： Wiley Online Library Journals 版權： 2016. American Geophysical Union. All Rights Reserved. 識別號： ISSN: 2169-9380 識別號： ISSN: 2169-9402 識別號： EISSN: 2169-9402 識別號： DOI: 10.1002/2016JA022503
Appears in Collections:	[DEPARTMENT OF SPACE SCIENCE AND ENGINEERING] journal & Dissertation

Files in This Item:

File	Description	Size	Format
index.html		0Kb	HTML	12	View/Open

社群 sharing

Loading...