NASA Logo, External Link
Facebook icon, External Link to NASA STI page on Facebook Twitter icon, External Link to NASA STI on Twitter YouTube icon, External Link to NASA STI Channel on YouTube RSS icon, External Link to New NASA STI RSS Feed AddThis share icon
 

Record Details

Record 1 of 1
Critical Magnetic Field Strengths for Unipolar Solar Coronal Plumes In Quiet Regions and Coronal Holes?
NTRS Full-Text: Click to View  [PDF Size: 6.3 MB]
Author and Affiliation:
Avallone, Ellis(Washington Univ., Seattle, WA, United States)
Tiwari, Sanjiv K.(Bay Area Environmental Research Inst., Huntsville, AL, United States)
Panesar, Navdeep K.(Universities Space Research Association, Huntsville, AL, United States)
Moore, Ronald L.(Alabama Univ., Huntsville, AL, United States)
Winebarger, Amy(NASA Marshall Space Flight Center, Huntsville, AL, United States)
Abstract: Coronal plumes are bright magnetic funnels that are found in quiet regions and coronal holes that extend high into the solar corona whose lifetimes can last from hours to days. The heating processes that make plumes bright involve the magnetic field at the base of the plume, but their intricacies remain mysterious. Raouafi et al. (2014) infer from observation that plume heating is a consequence of magnetic reconnection at the base, whereas Wang et al. (2016) infer that plume heating is a result of convergence of the magnetic flux at the plume's base, or base flux. Both papers suggest that the base flux in their plumes is of mixed polarity, but do not quantitatively measure the base flux or consider whether a critical magnetic field strength is required for plume production. To investigate the magnetic origins of plume heating, we track plume luminosity in the 171 Å wavelength as well as the abundance and strength of the base flux over the lifetimes of six unipolar coronal plumes. Of these, three are in coronal holes and three are in quiet regions. For this sample, we find that plume heating is triggered when convergence of the base flux surpasses a field strength of approximately 300 - 500 Gauss, and that the luminosity of both quiet region and coronal hole plumes respond similarly to the strength of the magnetic field in the base.
Publication Date: Dec 11, 2017
Document ID:
20170011679
(Acquired Dec 19, 2017)
Subject Category: ASTROPHYSICS
Report/Patent Number: MSFC-E-DAA-TN50032
Document Type: Oral/Visual Presentation
Meeting Information: 2017 AGU Fall Meeting; 11-15 Dec. 2017; New Orleans, LA; United States
Meeting Sponsor: American Geophysical Union; Washington, DC, United States
Contract/Grant/Task Num: NNH15CO48B; NNX17AL21G; NNM11AA01A; NSF AGS-1460767
Financial Sponsor: NASA Marshall Space Flight Center; Huntsville, AL, United States
Organization Source: NASA Marshall Space Flight Center; Huntsville, AL, United States
Description: 1p; In English
Distribution Limits: Unclassified; Publicly available; Unlimited
Rights: Copyright; Portions of the document may include copyright protected material
NASA Terms: MAGNETIC FIELDS; FIELD STRENGTH; SOLAR CORONA; PLUMES; CORONAL HOLES; MAGNETIC FLUX; LUMINOSITY; HEATING; CONVERGENCE; MAGNETIC FIELD RECONNECTION; POLARITY
› Back to Top
Find Similar Records
NASA Logo, External Link
NASA Official: Gerald Steeman
Site Curator: STI Program
Last Modified: December 19, 2017
Contact Us