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Title: Investigating the Magnetic Imprints of Major Solar Eruptions with SDO /HMI High-cadence Vector Magnetograms

Abstract

The solar active region photospheric magnetic field evolves rapidly during major eruptive events, suggesting appreciable feedback from the corona. Previous studies of these “magnetic imprints” are mostly based on line of sight only or lower-cadence vector observations; a temporally resolved depiction of the vector field evolution is hitherto lacking. Here, we introduce the high-cadence (90 s or 135 s) vector magnetogram data set from the Helioseismic and Magnetic Imager, which is well suited for investigating the phenomenon. These observations allow quantitative characterization of the permanent, step-like changes that are most pronounced in the horizontal field component (B {sub h}). A highly structured pattern emerges from analysis of an archetypical event, SOL2011-02-15T01:56, where B {sub h} near the main polarity inversion line increases significantly during the earlier phase of the associated flare with a timescale of several minutes, while B {sub h} in the periphery decreases at later times with smaller magnitudes and a slightly longer timescale. The data set also allows effective identification of the “magnetic transient” artifact, where enhanced flare emission alters the Stokes profiles and the inferred magnetic field becomes unreliable. Our results provide insights on the momentum processes in solar eruptions. The data set may also bemore » useful to the study of sunquakes and data-driven modeling of the corona.« less

Authors:
; ; ;  [1];  [2]
  1. W. W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305 (United States)
  2. Space Sciences Laboratory, University of California, Berkeley, CA 94720 (United States)
Publication Date:
OSTI Identifier:
22661137
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 839; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; EMISSION; EVOLUTION; FEEDBACK; MAGNETIC FIELDS; PHOTOSPHERE; SIMULATION; SOLAR CORONA; SUN; VECTOR FIELDS

Citation Formats

Sun Xudong, Hoeksema, J. Todd, Liu Yang, Chen Ruizhu, and Kazachenko, Maria, E-mail: xudong@Sun.stanford.edu. Investigating the Magnetic Imprints of Major Solar Eruptions with SDO /HMI High-cadence Vector Magnetograms. United States: N. p., 2017. Web. doi:10.3847/1538-4357/AA69C1.
Sun Xudong, Hoeksema, J. Todd, Liu Yang, Chen Ruizhu, & Kazachenko, Maria, E-mail: xudong@Sun.stanford.edu. Investigating the Magnetic Imprints of Major Solar Eruptions with SDO /HMI High-cadence Vector Magnetograms. United States. doi:10.3847/1538-4357/AA69C1.
Sun Xudong, Hoeksema, J. Todd, Liu Yang, Chen Ruizhu, and Kazachenko, Maria, E-mail: xudong@Sun.stanford.edu. Mon . "Investigating the Magnetic Imprints of Major Solar Eruptions with SDO /HMI High-cadence Vector Magnetograms". United States. doi:10.3847/1538-4357/AA69C1.
@article{osti_22661137,
title = {Investigating the Magnetic Imprints of Major Solar Eruptions with SDO /HMI High-cadence Vector Magnetograms},
author = {Sun Xudong and Hoeksema, J. Todd and Liu Yang and Chen Ruizhu and Kazachenko, Maria, E-mail: xudong@Sun.stanford.edu},
abstractNote = {The solar active region photospheric magnetic field evolves rapidly during major eruptive events, suggesting appreciable feedback from the corona. Previous studies of these “magnetic imprints” are mostly based on line of sight only or lower-cadence vector observations; a temporally resolved depiction of the vector field evolution is hitherto lacking. Here, we introduce the high-cadence (90 s or 135 s) vector magnetogram data set from the Helioseismic and Magnetic Imager, which is well suited for investigating the phenomenon. These observations allow quantitative characterization of the permanent, step-like changes that are most pronounced in the horizontal field component (B {sub h}). A highly structured pattern emerges from analysis of an archetypical event, SOL2011-02-15T01:56, where B {sub h} near the main polarity inversion line increases significantly during the earlier phase of the associated flare with a timescale of several minutes, while B {sub h} in the periphery decreases at later times with smaller magnitudes and a slightly longer timescale. The data set also allows effective identification of the “magnetic transient” artifact, where enhanced flare emission alters the Stokes profiles and the inferred magnetic field becomes unreliable. Our results provide insights on the momentum processes in solar eruptions. The data set may also be useful to the study of sunquakes and data-driven modeling of the corona.},
doi = {10.3847/1538-4357/AA69C1},
journal = {Astrophysical Journal},
number = 1,
volume = 839,
place = {United States},
year = {Mon Apr 10 00:00:00 EDT 2017},
month = {Mon Apr 10 00:00:00 EDT 2017}
}