DETERMINATION OF SUB-RESOLUTION STRUCTURE OF A JET BY SOLAR MAGNETOSEISMOLOGY

Journal Article · Sun Jan 01 04:00:00 EST 2012 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/744/1/5· OSTI ID:22004374

Morton, R J; Erdelyi, R ^[1]; Verth, G

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1. Solar Physics and Space Plasma Research Centre (SP2RC), University of Sheffield, Hicks Building, Hounsfield Road, Sheffield S3 7RH (United Kingdom)

A thin dark thread is observed in a UV/EUV solar jet in the 171 A, 193 A, and 211 A, and partially in 304 A. The dark thread appears to originate in the chromosphere but its temperature does not appear to lie within the passbands of the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory. We therefore implement solar magnetoseismology to estimate the plasma parameters of the dark thread. A propagating kink (transverse) wave is observed to travel along the dark thread. The wave is tracked over a range of {approx}7000 km by placing multiple slits along the axis of the dark thread. The phase speed and amplitude of the wave are estimated and magnetoseismological theory is employed to determine the plasma parameters. We are able to estimate the plasma temperature, density gradient, magnetic field gradient, and sub-resolution expansion of the dark thread. The dark thread is found to be cool, T {approx}< 3 Multiplication-Sign 10{sup 4}, with both strong density and magnetic field gradients. The expansion of the flux tube along its length is {approx}300-400 km.

• OSTI ID: 22004374
• Journal Information: Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 1 Vol. 744; ISSN ASJOAB; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
ASTROPHYSICS
CHROMOSPHERE
ELECTRON TEMPERATURE
ION TEMPERATURE
MAGNETIC FIELDS
MAGNETOHYDRODYNAMICS
SUN