Kinematics and Fine Structure of An Unwinding Polar Jet Observed by SDO/AIA

Details Kinematics and Fine Structure of An Unwinding Polar Jet Observed by SDO/AIA Kinematics and Fine Structure of An Unwinding Polar Jet Observed by SDO/AIA

2011-06-08

arxiv.org/abs/1106.1489v2

2011 ApJ 735 L43

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

Scientific paper

10.1088/2041-8205/735/2/L43

We present an observational study of the kinematics and fine structure of an unwinding polar jet, with high temporal and spatial observations taken by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamic Observatory (SDO) and the Solar Magnetic Activity Research Telescope (SMART). During the rising period, the shape of the jet resembled a cylinder with helical structures on the surface, while the mass of the jet was mainly distributed on the cylinder's shell. In the radial direction, the jet expanded successively at its western side. The radial expansion presented three distinct phases: the gradually expanding phase, the fast expanding phase, and the steady phase. Each phase lasted for about 12 minutes. The angular speed of the unwinding jet and the twist transferred into the outer corona during the eruption are estimated to be 11.1 \times 10{-3} rad/s (period = 564 s) and 1.17 to 2.55 turns (or 2.34 to 5.1{\pi}) respectively. On the other hand, by calculating the azimuthal component of the magnetic field in the jet and comparing the free energy stored in the non-potential magnetic field with the jet's total energy, we find that the non-potential magnetic field in the jet is enough to supply the energy for the ejection. These new observational results strongly support the scenario that the jets are driven by the magnetic twist, which is stored in the twisted closed field of a bipole, and released through magnetic reconnection between the bipole and its ambient open field.

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