Vol 17, No 8 (2017) / Zheng

Sunspot rotation and magnetic transients associated with flares in NOAA AR 11429

Sunspot rotation and magnetic transients associated with flares in NOAA AR 11429

Zheng Jian-Chuan1, , Yang Zhi-Liang1, Guo Jian-Peng1, 2, , Guo Kai-Ming1, Huang Hui1, Song Xuan1, Wan Wei-Xing2, 3

Department of Astronomy, Beijing Normal University, Beijing 100875, China
Key Laboratory of Earth and Planetary Physics, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing 100029, China
College of Earth Sciences, University of Chinese Academy of Sciences, Beijing 100049, China

† Corresponding author. E-mail: zhengjc@mail.bnu.edu.cn jpguo@bnu.edu.cn


Abstract: Abstract

We analyze sunspot rotation and magnetic transients in NOAA AR 11429 during two X-class (X5.4 and X1.3) flares using data from the Helioseismic and Magnetic Imager on board the Solar Dynamics Observatory. A large leading sunspot with positive magnetic polarity rotated counterclockwise. As expected, the rotation was significantly affected by the two flares. Magnetic transients induced by the flares were clearly evident in the sunspots with negative polarity. They were moving across the sunspots with speed of order 3 – 7 km s−1. Furthermore, the trend of magnetic flux evolution in these sunspots exhibited changes associated with the flares. These results may shed light on understanding the evolution of sunspots.

Keywords: sunspots;Sun: rotation;Sun: magnetic fields



1 Introduction

Sunspots are concentrations of a strong magnetic field on the solar surface, consisting of a dark umbra and a fibrous penumbra (Solanki 2003 ). It is generally accepted that eruption events such as flares occurring in the upper atmosphere are associated with the magnetic field generated from the base of the convection zone, emerging as bipolar magnetic regions at the solar surface, then extending to the corona (Solanki et al. 2006 ). So, visible sunspots play an important role in studying a variety of phenomena on the Sun.

The evolution of sunspots includes formation, movement, deformation and disappearance. Rotation is an important feature during evolution. In general, there are two kinds of rotation: one sunspot rotates around its umbral center and one sunspot rotates around the other (Yan & Qu 2012 ). The rotation of sunspots and spot-groups has been studied for many decades (see e.g., Evershed 1910 ; St. John 1913 ; Maltby 1964 ; Brown et al. 2003 ; Zhang et al. 2007 ; Yan et al. 2009 ; Min & Chae 2009 ). Yan et al. ( 2008b ) found 182 significantly rotating sunspots among 2959 active regions. Some authors believed the rotational motion of sunspotsmay be involvedwith energy build-up and later release by flares (e.g., Stenflo 1969 ; Barnes & Sturrock 1972 ; Hiremath et al. 2005 ; Zhang et al. 2008 ). Furthermore, the relationships between sunspot rotation and coronal consequence (Brown et al. 2003 ; Tian et al. 2008 ), flare productivity (Yan et al. 2008a ; Zhang et al. 2008 ; Ruan et al. 2014 ), direction of rotation (Zheng et al. 2016 ) and magnetic helicities (Vemareddy et al. 2012 ) have been investigated. The association of flares with abnormal rotation rates (Hiremath et al. 2005 ) has been found. Specifically, Wang et al. ( 2014 ) reported two sunspots in AR 11158 rotating along with an X2.2 flare. Liu et al. ( 2016 ) reported a non-uniformrotation induced by an M6.5 flare in NOAA AR 12371, and Bi et al. ( 2016 ) found an abrupt reverse rotation of a sunspot in NOAA AR 12158 caused by back reaction of an X1.6 flare.

In addition, the photospheric magnetic field changes during the flares and the magnetic field is distorted enough to store energy powering a flare. After a flare has erupted, the distorted field relaxes and restructures (Sakurai & Hiei 1996 ). There are two kinds of changes in the magnetic field based on observations: the first is rapid short-term changes (Patterson & Zirin 1981 ; Zhao et al. 2009 ), which is due to flare-induced spectral line changes (Patterson 1984 ; Qiu & Gary 2003 ). It is generally believed that rapid short-term changes about sign reversal of magnetic field are just an artifact associated with the modification of the emission line profile (see Ding et al. 2002 ). However, Harker & Pevtsov ( 2013 ) also analyzed magnetic transients during the M7.9 flare in NOAA AR 11429 on 2012 March 13 and suggested that magnetic transients represented a real change in the photospheric magnetic field. Another is irreversible changes from pre-flare to post-flare (e.g., Spirock et al. 2002 ; Wang et al. 2002 ; Wang 2006 ; Song & Zhang 2016 ). The irreversible changes were first noticed by Wang et al. ( 1994 ). They showed that magnetic shear increased after flares with vector magnetic field data. Cameron & Sammis ( 1999 ) reported a change in the line-of-sight (LOS) field during the X9.3 flare on 1990 May 24 with videomagnetograph data from Big Bear Solar Observatory (BBSO). Sudol & Harvey ( 2005 ) and Petrie & Sudol ( 2010 ) analyzed changes in the LOS magnetic field during some X- and M-class flares with Global Oscillation Network Group (GONG) magnetograms. The median duration of changes was about 15minutes and themedian absolute value of changeswas about 69G. Wang & Liu ( 2010 ) demonstrated that the change in LOS magnetic field is due to an increase in the horizontal magnetic field near the polarity inversion line. With the seeing-free data of vector magnetograms, Liu et al. ( 2012 ) found that the photospheric transverse magnetic field enhancementwas associated with anM6.6 flare in NOAA AR 11158. Wang et al. ( 2012 ) observed the same phenomenon associated with an X2.2 flare in this active region. These results suggested that the magnetic field near the polarity inversion line could become more horizontal after a flare.

In this study, we analyze the evolution of sunspots in NOAA AR 11429. We will explore the rotation of sunspots along with the flares, i.e., how do the flares and the rotation of sunspots affect each other. The magnetic transients induced by flares are studied in prior works. We further study the motion of magnetic transients to understand how the flares influence sunspots. The paper is organized as follows. In Section 2 we describe the data used and the entire structure of the active region. Section 3 highlights the associated data processing method. We summarize and discuss the results in Section 4.

2 Observational Data

The 45 s cadence and spatial sampling of 0.5″ pixel−1 full-disk continuum intensity images and LOS magnetograms observed by the Helioseismic and Magnetic Imager (HMI; Schou et al. 2012 ) on board Solar Dynamics Observatory (SDO) are used to analyze the variation of sunspots in NOAA AR 11429. Images from the Atmospheric Imaging Assembly (AIA; Lemen et al. 2012 ) on board SDO are used to investigate the chromospheric and coronal context: AIA 304 Å formed in the transition region and chromosphere, and AIA 1600 Å formed in the upper photosphere and transition region.

AR 11429 appeared on the eastern limb on 2012 March 3, and then rapidly became a complicated reverse-polarity βγδ active region. The evolution and development of AR 11429 from March 5 to March 12 are displayed in Figure 1. It is interesting to note that the sunspots in this active region were moving away from each other, i.e., the leading sunspots are moving westward and the following sunspots are moving eastward. Several major eruptions were clearly visible in this active region. Typically, three X-class flares occurred: one (X1.1) on March 5 and two of interest (X5.4 and X1.3) on March 7. The Geostationary Operational Environmental Satellite (GOES) soft X-ray flux (Fig. 3a) indicates that the X5.4 flare started at 00:02 UT, peaked at 00:27 UT and ended at 00:40 UT, and the X1.3 flare started at 01:05 UT, peaked at 01:14 UT and ended at 01:23 UT. The evolutions of five prominent sunspots, two positive polarity sunspots (P1 and P2) and three negative polarity sunspots (N1, N2 and N3) were associated with these two flares, as will be discussed in the next section.

Fig. 1 The HMI intensity images and magnetograms show the evolution of AR 11429 during 2012 March 5–12. The field of view is 200″ × 200″. The main sunspots are labeled with P/N*. The white/black areas in magnetograms represent positive/negative magnetic polarity. The red rectangular boxes are regions selected for further study.

3 Analysis and Results

3.1 Sunspot Rotation Associated with Flares

To study the rotation, we regard rotation of individual sunspots as simplified solid-body rotation (i.e., a sunspot rotates around its umbral center), and track the variation of ellipses that best fit individual sunspots on time-series intensity images (see Bi et al. 2016 ). Take sunspot P1 as an example. The best-fit ellipses on the intensity images at 23:29:23 UT on March 6 and 01:28:38 UT on March 7 are shown in Figure 2(a) and Figure 2(b), respectively. Obviously, the major axis rotates counterclockwise about 7°. In the present study, changes in the angle between the major axis and the horizontal direction of the best-fit ellipses are used to describe the rotation of the sunspot. The results together with GOES soft X-ray flux are shown in Figure 3.

Fig. 2 HMI intensity images before and after the X5.4 class flare. The green dashed lines represent the ellipse fit to the sunspot P1. The blue and yellow dashed lines are the major axes of the ellipses.
Fig. 3 (a) Evolution of GOES soft X-ray emission from 23:30 UT on March 6 to 01:30 UT on March 7. The vertical dashed lines represent the GOES flare start, peak and end times. (b)–(e) Time profiles of orientation angle (between the major axis and horizontal direction) of sunspots P1, N1, N2 and N3, respectively. The green and blue curves are profiles of relative mean intensity within each sunspot region with respect to the quiet Sun in AIA 304 Å and AIA 1600 Å respectively.

Figure 3(b) shows that P1 rotated mainly counterclockwise from ∼23:30 UT on March 6 to ∼01:30 UT on March 7. Before the start of the X5.4 flare, the rotation was very fast with speed up to 7.92° h−1. From the start to the peak of the flare, the rotation speed decreased slowly to about 4.89° h−1 and the rotation trend stayed counterclockwise. Just after the peak of the flare, the rotation trend reversed from counterclockwise to clockwise. Its speed was about 4.07° h−1. After the flare, the rotation direction returned to being counterclockwise with a rotation speed of about 6.56° h−1, and the rotation speed increased gradually until the beginning of the X1.3 flare. Later, the rotation trend reversed to be clockwise again with a rotation speed of about 6.44° h−1 and slowed down. These results indicate that the rotation of sunspot P1 was significantly affected by both flares. The relative mean intensity profiles in different AIA wavelengths, obtained from the corresponding co-aligned HMI images, are also plotted in Figure 3. The intensity in the AIA wavelengths of 304 Å (green curve) and AIA 1600 Å (blue curve) started rising around 00:05 UT, peaked at about 00:07 UT and then decreased during the impulsive phase of the X5.4 flare. At about 01:05 UT, the intensities started rising again and peaked at about 01:14 UT. This behavior provides further support to the view that solar flares are often related to the rotation of sunspots.

The rotation of sunspot N1 was complicated (Fig. 3c). Before the peak of the X5.4 flare, the rotation trend was mainly counterclockwise, and then reversed to be clockwise. The situation around the X1.3 flare was similar to that around the former flare. The intensity of AIA wavelengths increased and the rotation changed significantly during the impulsive phases of the X5.4 and X1.3 flares. As shown in Figure 3(d), sunspot N2 rotated clockwise from ∼00:15 UT to ∼00:40 UT. The relative mean intensity of 1600 Å in this sunspot started rising at ∼00:05 UT and reached its maximum at ∼00:20 UT. The relative mean intensity of 304 Å started rising at ∼00:05 UT and reached its maximum at ∼00:30 UT. So, the X5.4 flare affected the rotation of sunspot N2. Sunspot N3 remained stable during the two flares (Fig. 3e). The rotation speed was poorly correlated with the intensity of AIA wavelengths, and therefore the X5.4 and X1.3 flares.

3.2 The Motion of Magnetic Transients

Magnetic transients induced by flares have been thoroughly investigated by Patterson ( 1984 ) and Qiu & Gary ( 2003 ). They analyzed the cause, location and level of the magnetic transients. Here, we find that there are some magnetic transientsmoving through sunspotsN1, N2 and N3, and there is no apparent magnetic transient motion in sunspots P1 and P2. Because the polarity of sunspots N1, N2 and N3 is negative (black regions in the magnetograms), the magnetic transients mean that the polarity is reversed.

Figure 4 shows changes of the magnetic field in sunspot N1. At 01:09 UT on March 7, the magnetic transients marked by red arrows in the umbra of the sunspot can be clearly seen. These magnetic transients (the positive magnetic field) moved toward the southeast direction. At 01:14 UT, the area with positive magnetic field became larger while the strength became weaker, as shown in Figure 4(a2). The green line in Figure 4(a3) indicates the moving trajectory of the positive polarity points. To investigate the kinematic evolution of the reversed polarity, the time-distance plots obtained along the green trajectory line are shown in Figure 4(d). A white streak is clearly visible. It started at ∼01:07 UT and ended at ∼01:16 UT, consistent with the time of the X1.3 flare. It might imply that the reversed magnetic polarity was caused by this flare. The distance corresponding to the streak was about 5 arcsec. Thus, the moving speed of the magnetic transients can be estimated to be about 6.59 km s−1. Similarly, some magnetic transients (i.e., the reversed magnetic field) were present in sunspots N2 and N3, and probably associated with the X5.4 flare, as shown in Figures 5 and 6. They were moving toward the southeast with speed about 3.69 km s−1 and 3.22 km s−1 respectively.

Fig. 4 The reversed magnetic field moving through sunspot N1. The red arrows in (a1) and (a2) indicate the location of the reversed magnetic field and the green line in (a3) delineates the trajectory of the moving reversed magnetic field. (b1)–(b3) The co-aligned AIA 304 Å images corresponding to HMI magnetograms. The blue contours represent the magnetic field of sunspot N1 at −800 G. (c1)–(c3) The co-aligned AIA 1600 Å images overlaid by magnetogram contours of sunspot N1. (d) Time-slice plot of the trajectory. The blue dashed line shows the evolution of the reversed magnetic field. The red curve overlaid on the time-slice plot is the GOES soft X-ray flux.
Fig. 5 Same as Fig. 4, but for sunspot N2.
Fig. 6 Same as Fig. 4, but for sunspot N3.

In order to check whether the magnetic transients were co-spatial with flare ribbons, we further examined the co-aligned AIA 304 Å and AIA 1600 Å images corresponding to HMI magnetograms, which are displayed in panels (b1)–(b3) and panels (c1)–(c3) in Figures 4, 5 and 6 respectively. The flare ribbons can be seen in these panels. They were separating from each other. The locations of sunspots N1, N2 and N3 in AIA images, marked by magnetogram contours at −800 G, were moving with flare ribbons. This implies the magnetic transients were co-spatial with flare ribbons.

We calculated the magnetic flux of sunspots N1, N2 and N3 for the regions marked by the red rectangular boxes in Figure 1. The magnetic flux of sunspots with negative polarity together with GOES soft X-ray flux are shown in Figure 7. Before the start of the X5.4 flare, the absolute value of magnetic flux in sunspot N1 decreased slowly. From the start to peak of the flare, it decreased gradually. Then, the value stayed almost unchanged. At the end of the flare, it increased slightly. During the period of the X1.3 flare, the absolute value of magnetic flux decreased first and then increased abruptly. These results suggest that changes in the trend of magnetic flux in sunspot N1 were caused by both the X5.4 flare and the X1.3 flare.

Fig. 7 Magnetic flux of sunspots N1, N2 and N3. (a) Evolution of GOES soft X-ray emission from 23:30 UT on March 6 to 01:30 UT on March 7. The vertical dashed lines represent the GOES flare start, peak and end times. (b)–(d)Time profiles of magnetic flux of sunspots N1, N2 and N3, respectively.

The magnetic flux of sunspot N2 mainly increased from 23:30 UT on March 6 to 01:30 UT on March 7. There was an obvious change near the peak of the X5.4 flare. Specifically, the absolute value decreased first and then increased, as shown in Figure 7(c). The absolute magnetic flux value of sunspot N3 (Fig. 7d) almost stayed unchanged before the start of the X5.4 flare. Similarly, during the X5.4 flare, the magnetic flux decreased rapidly, and then increased monotonically. These results suggest that changes in the trend of magnetic flux in sunspots N2 and N3 were mainly due to the X5.4 flare.

4 Summary and Discussion

AR 11429 is a complicated active region with a reversed polarity structure, in contrast with the nature of solar cycle 24. It has a large leading sunspot with positive magnetic polarity (P1) exhibiting significant counterclockwise rotation. The rotation underwent some changes during two X-class (X5.4 and X1.3) flares. It is possible that the flares were triggered by the sunspot rotation (see Zhang et al. 2008 ; Vemareddy et al. 2016 ), and in turn they reacted back and affected the sunspot P1 rotation.

The magnetic transients induced by the two X-class flares can be seen in sunspots with negative magnetic polarity (N1, N2 and N3). They moved outward with respect to the center of the active region and moved through the sunspots quickly with speed up to about 6.59 km s−1. The magnetic transients lasted for about ten minutes within the period of the X5.4 and X1.3 flare. As expected, the magnetic transients, which are clearly illustrated in sunspots N1, N2 and N3, were moving away from the polarity inversion line shown in Figures 4, 5 and 6. The magnetic transients that occurred during the X5.4 and X1.3 flares were co-spatial with flare ribbons. This is consistent with Maurya et al. ( 2012 ), who found that magnetic transients in AR 11158 during an X2.2 flare persisted for a few minutes and appeared co-spatial with flare ribbons, which were separating with a mean velocity of 8 km s−1.

During the evolution of sunspots (N1, N2 and N3), changes in the trend of magnetic field evolutionwere presented, and are associated with the two X-class flares. Similar results in five δ sunspots were found by Wang ( 2006 ). The increasing and decreasing tendency of the magnetic flux in the active region might be attributed to magnetic flux emergence and magnetic cancelation (van Driel-Gesztelyi & Green 2015 ).

The evolution of sunspots with a complicated structure can be affected by many factors such as interaction among sunspots within the same active region, physical change induced by the flare, and interaction between magnetic field and plasma. In this study, we have found that the motion and trend of magnetic field evolution in sunspots are significantly affected by flares. Other influences on the evolution of sunspots will be examined in future studies.


References

Barnes C. W. Sturrock P. A. 1972 ApJ 174 659
Bi Y. Jiang Y. Yang J. et al. 2016 Nature Communications 7 13798
Brown D. S. Nightingale R. W. Alexander D. et al. 2003 Sol. Phys. 216 79
Cameron R. Sammis I. 1999 ApJ 525 L61
Ding M. D. Qiu J. Wang H. 2002 ApJ 576 L83
Evershed J. 1910 MNRAS 70 217
Harker B. J. Pevtsov A. A. 2013 ApJ 778 175
Hiremath K. M. Suryanarayana G. S. Lovely M. R. 2005 A&A 437 297
Lemen J. R. Title A. M. Akin D. J. et al. 2012 Sol. Phys. 275 17
Liu C. Deng N. Liu R. et al. 2012 ApJ 745 L4
Liu C. Xu Y. Cao W. et al. 2016 Nature Communications 7 13104
Maltby P. 1964 Astrophysica Norvegica 8 205
Maurya R. A. Vemareddy P. Ambastha A. 2012 ApJ 747 134
Min S. Chae J. 2009 Sol. Phys. 258 203
Patterson A. 1984 ApJ 280 884
Patterson A. Zirin H. 1981 ApJ 243 L99
Petrie G. J. D. Sudol J. J. 2010 ApJ 724 1218
Qiu J. Gary D. E. 2003 ApJ 599 615
Ruan G. Chen Y. Wang S. et al. 2014 ApJ 784 165
Sakurai T. Hiei E. 1996 Advances in Space Research 17 91
Schou J. Scherrer P. H. Bush R. I. et al. 2012 Sol. Phys. 275 229
Solanki S. K. 2003 A&A Rev. 11 153
Solanki S. K. Inhester B. Schüssler M. 2006 Reports on Progress in Physics 69 563
Song Y. L. Zhang M. 2016 ApJ 826 173
Spirock T. J. Yurchyshyn V. B. Wang H. 2002 ApJ 572 1072
John C. E. St. 1913 ApJ 37 322
Stenflo J. O. 1969 Sol. Phys. 8 115
Sudol J. J. Harvey J. W. 2005 ApJ 635 647
Tian L. Alexander D. Nightingale R. 2008 ApJ 684 747
van Driel-Gesztelyi L. Green L. M. 2015 Living Reviews in Solar Physics 12 1
Vemareddy P. Ambastha A. Maurya R. A. Chae J. 2012 ApJ 761 86
Vemareddy P. Cheng X. Ravindra B. 2016 ApJ 829 24
Wang H. 2006 ApJ 649 490
Wang H. Ewell M. W. Jr. Zirin H. Ai G. 1994 ApJ 424 436
Wang H. Liu C. 2010 ApJ 716 L195
Wang H. Spirock T. J. Qiu J. et al. 2002 ApJ 576 497
Wang S. Liu C. Deng N. Wang H. 2014 ApJ 782 L31
Wang S. Liu C. Liu R. et al. 2012 ApJ 745 L17
Yan X. L. Qu Z. Q. 2012 EAS Publications Series 55 EAS Publications Series Faurobert M. Fang C. Corbard T. 137
Yan X.-L. Qu Z.-Q. Kong D.-F. 2008a MNRAS 391 1887
Yan X. L. Qu Z. Q. Xu C. L. 2008b ApJ 682 L65
Yan X.-L. Qu Z.-Q. Xu C.-L. Xue Z.-K. Kong D.-F. 2009 RAA (Research in Astronomy and Astrophysics) 9 596
Zhang J. Li L. Song Q. 2007 ApJ 662 L35
Zhang Y. Liu J. Zhang H. 2008 Sol. Phys. 247 39
Zhao M. Wang J.-X. Matthews S. et al. 2009 RAA (Research in Astronomy and Astrophysics) 9 812
Zheng J. Yang Z. Guo K. Wang H. Wang S. 2016 ApJ 826 6
Cite this article: Zheng Jian-Chuan, Yang Zhi-Liang, Guo Jian-Peng, Guo Kai-Ming, Huang Hui, Song Xuan, Wan Wei-Xing. Sunspot rotation and magnetic transients associated with flares in NOAA AR 11429. Cancer Biol Med. 2017; 8:081.

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