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<p>We study the evolution and reorganization of magnetic field lines and associated plasma dynamics during the formation of a quiescent prominence. For this purpose, we have utilized the observations taken by the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO). Our observations revealed an abrupt ascent of an EUV bright structure (or EUV jet) accompanied by a downflow during the early stage of the prominence formation. We closely tracked the rising motion and the associated downflow, estimating their average speeds around 2.8&#xa0;km s<sup>−1</sup> and 10.1&#xa0;km s<sup>−1</sup>, respectively, in conjunction with the brightening of a rising jet. We derived the temperature of the jet plasma by employing the Differential Emission Measure (DEM) on AIA observations and found it to be higher than expected temperature of prominence plasma (around <InlineEquation ID="IEq1"> <InlineMediaObject> <ImageObject Color="BlackWhite" FileRef="11207_2025_2493_Article_IEq1.gif" Format="GIF" Height="18" Rendition="HTML" Resolution="72" Type="Linedraw" Width="93" /> </InlineMediaObject> <EquationSource Format="MATHML"><math> <msub> <mo>log</mo> <mn>10</mn> </msub> <mi>T</mi> <mo>≈</mo> <mn>5.2</mn> </math></EquationSource> <EquationSource Format="TEX">$\log _{10}T \approx 5.2$</EquationSource> </InlineEquation>). Moreover, we observed bi-directional plasma motions and brightening in jet plasma at the same time. These observations could be due to the reorganization of the magnetic field lines as part of magnetic reconnection within the prominence during early phase of its formation.</p>

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Dynamics of Plasma and Magnetic Fields in a Quiescent Prominence Formation

  • 期刊论文

  • 发表日期：

    2025年6月19日

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  • P. T. Jain Jacob,
  • Ram Ajor Maurya,
  • Durgesh Tripathi

摘要

We study the evolution and reorganization of magnetic field lines and associated plasma dynamics during the formation of a quiescent prominence. For this purpose, we have utilized the observations taken by the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO). Our observations revealed an abrupt ascent of an EUV bright structure (or EUV jet) accompanied by a downflow during the early stage of the prominence formation. We closely tracked the rising motion and the associated downflow, estimating their average speeds around 2.8 km s−1 and 10.1 km s−1, respectively, in conjunction with the brightening of a rising jet. We derived the temperature of the jet plasma by employing the Differential Emission Measure (DEM) on AIA observations and found it to be higher than expected temperature of prominence plasma (around log 10 T ≈ 5.2 $\log _{10}T \approx 5.2$ ). Moreover, we observed bi-directional plasma motions and brightening in jet plasma at the same time. These observations could be due to the reorganization of the magnetic field lines as part of magnetic reconnection within the prominence during early phase of its formation.