Solar jets are plasma ejection phenomena that are observed throughout the solar atmosphere and have been extensively studied in terms of their morphology, dynamic characteristics, and driving mechanisms since their first detection in the X-ray emission of coronal jets by the Soft X-ray Telescope on board the Yohkoh satellite in the early 1990s (Schmieder et al. 1995;Shen et al. 2019;Raouafi et al. 2016;Shen 2021;Schmieder 2022). Jets are observed in multiple wavelengths in the solar atmosphere. They appear as bright structures in the corona and as plasma flows along magnetic field lines in the chromosphere (Tian et al. 2018;De Pontieu et al. 2021;Schmieder et al. 2022). They have been referred to as H α surges, plasma ejec-tions, and chromospheric jets in previous studies (Roy 1973;Asai et al. 2001;Louis et al. 2014). Recently, some researchers have also called them light walls (Yang et al. 2015) or peacock jets (Robustini et al. 2016). Zhao et al. (2022) analyzed recurrent jets that repeatedly propagated from one end to the other in the chromosphere. Many jets have been observed in sunspots, while others occur in light bridges, such as the fan-shaped jets near sunspot light bridges studied by Liu et al. (2022). The first observation of fan-shaped jets on sunspot light bridges was reported by Asai et al. (2001), who found that these jets had speeds of about 50 km s -1 and a maximum length of 2 mega meters, suggesting that the jets originate from emerging magnetic flux with no compelling observational evidence. Jets can occur above neutral lines of magnetic fields (Hou et al. 2016) and are thought to be triggered by magnetic reconnection, either in combination with magnetic acoustic waves (Zhang et al. 2017), magnetic reconnection (Hou et al. 2017;Bai et al. 2019;Yang et al. 2019), or a combination of both (Tian et al. 2018;Huang et al. 2020). Magnetic reconnection is widely considered as the triggering mechanism for jets, and researchers have been searching for evidence of magnetic reconnection in the solar atmosphere. Some high-resolution observations have shown inverted-Y-shaped jets that frequently occur in coronal holes and active regions around sunspots (Cirtain et al. 2007;Singh et al. 2012;Yang et al. 2011;Tian et al. 2012;Zhang & Ji 2014;Shen et al. 2012). Inverted-Y-shaped jets are considered to be the result of reconnection between smallscale magnetic bipolar and unipolar background fields. The observations provide strong evidence for magnetic reconnection (Moreno-Insertis & Galsgaard 2013;Chen et al. 2015;Tian et al. 2018). The former authors studied reconnectiondriven jets that repeatedly occur on the light bridges of sunspots. They examined jets that frequently occurred in the wings of the H α line and found that many jets exhibited an inverted-Yshaped structure, demonstrating a typical reconnection process in a unipolar magnetic field environment where the overlying magnetic field of the penumbra reconnected with newly emerged magnetic flux. A wealth of evidence was also reported from numerical simulations that supports the connection between jets and magnetic reconnection. For example, Yokoyama & Shibata (1995, 1996) performed numerical simulations based on the magnetic reconnection model to reproduce coronal X-ray jets, which successfully demonstrated the connection between jets and magnetic reconnection. They generated anemone jets and bidirectional jets in their simulations based on two different initial magnetic field configurations. The anemone jets were produced by reconnection between newly emerged and coronal sheared fields, mostly along the spine (Joshi et al. 2020;Zhu et al. 2023). The bidirectional jets were produced by reconnection between newly emerged and overlying fields (Ruan et al. 2019). Both types of jets confirmed the occurrence of magnetic reconnection.
It is generally thought that jets are associated with the emergence and cancellation of magnetic flux. Many observational results support the model based on which magnetic reconnection triggers jet events. The interaction between emerging magnetic flux fields and the mobile magnetic structure can trigger jet events (Brooks et al. 2007). Kurokawa & Kawai (1993) found that jets were frequently observed and recurred for several hours, leading to the conclusion that magnetic reconnection between the newly emerged flux and preexisting magnetic fields is the basic mechanism for generating jets. Shimojo et al. (1998) studied the magnetic field characteristics of X-ray jets and found that jets occur in unipolar, bipolar, and mixed-polarity regions, highlighting the importance of the magnetic field environment in the occurrence of jets. Chae et al. (1999) analyzed ultraviolet jets in the transition region and found that they repeatedly occur in regions where preexisting magnetic flux of opposite polarity cancels out with newly emerged magnetic flux. Liu & Kurokawa (2004) studied a jet event in an emerging flux region and found a close correlation between the jet and the newly emerged bipolar structure, suggesting that an enhanced magnetic cancellation process triggered the jet. Yoshimura et al. (2003) reported a close correlation between a jet at the edge of emerging flux regions, magnetic cancellation, and ultraviolet brightening, indicating a strong spatiotemporal relation between jets and the brightening observed in the photosphere, especially during the early stages of flux emergence, which is consistent with the model of magnetic reconnection.
In addition to the scenario that magnetic reconnection triggers jets, magnetohydrodynamic (MHD) waves in the photosphere may also play a role. Magneto-acoustic waves caused by p-mode leakage or Alfvén waves can lead to the formation of shocks, which then propel the plasma into magnetic flux tubes by increasing the magnetic pressure of the giant spicules (Shibata 1982). Shibata (1982) used a one-dimensional (1D) MHD model to explain why the spicules are longer in coronal holes, with the key process being the increased intensity of the chromospheric shock waves. Based on this, Iijima & Yokoyama (2015) studied the influence of the coronal temperature on chromospheric jets and found through two-dimensional (2D) MHD simulations that jets are ejected farther outward when the coronal temperature is lower (similar to coronal holes). Subsequently, Iijima & Yokoyama (2017) used a three-dimensional (3D) MHD model to study jets that were generated by twisted magnetic field lines and observed the excitation of various MHD waves and the generation of chromospheric jets in their simulations. The strong twisting of magnetic field lines in the chromosphere helps to drive the jets through the action of the Lorentz force, which means that jets are a natural outcome of oscillatory motion.
Repeated jets often occur in mixed-polarity regions (Chen et al. 2015;Jiang & Wang 2000;Guo et al. 2013;Joshi et al. 2017), where persistent flux emergence, cancellation, and convergence can lead to the repeated occurrence of jets. Repeating jets often occur in nearly the same location (Schmieder et al. 1995;Chifor et al. 2008;Zhang et al. 2012;Wang & Liu 2012;Wang et al. 2006). Cirtain et al. (2007) detected an average of ten jet events per hour in a 100-h observation and found that jets often occurred at the same X-ray bright point or very close to the location of the previous jet onset. Jiang et al. (2007) observed three jet events that occurred intermittently within approximately 70 min. Guo et al. (2013) reported three recurring extreme-ultraviolet (EUV) jets within an hour and attributed them to repeated accumulated currents. Mulay et al. (2017) studied periodic jets using Si IV 1400 Å data obtained from the Interface Region Imaging Spectrograph (IRIS) Slit-Jaw Imager (SJI) and observed bright and compact plasmas, suggesting a helical motion along the apex of the jet. Yang et al. (2015) discovered many bright structures rooted in the light bridges of active region sunspots and named them "light walls". The tops of these bright walls exhibit sustained upward and downward motion that oscillates in height with a period of approximately 4 min. They interpreted these oscillations as leakage of p-mode waves from beneath the photosphere.
P-mode oscillations in the photosphere may contribute to periodic solar activities, as shown by Chandra et al. (2015), who reported recurring jets with an oscillation period of approximately 3 min. They suggested that the increase and decrease of the sunspot oscillation power before and after the jet can indicate the occurrence of magnetic reconnection dominated by a wave, and then modulated the 3-min period of the jet, which might correspond to the leakage of 3-min slow magnetoacoustic waves. Recently, 3D numerical MHD simulations of a model solar atmosphere with a uniform, vertical, and cylindrically symmetric magnetic field, mimicking the behavior of p-mode oscillations were performed in a pore (Griffiths et al. 2023). The authors concluded that the magnetic regions of the solar atmosphere are favorable for the propagation of a small leakage of energy by slow magnetosonic modes. It was found that the oscillations are enhanced by a vertical magnetic field. The results also exhibit a variation in the frequency of the oscillations at different A183, page 2 of 14 heights in the low to medium solar atmosphere and for different values of the magnetic field. Zeng et al. (2013) found a recurring jet with a 5-min period in their previous study. Hong et al. (2022) studied quasi-periodic microjets driven by granulation convection and proposed that the persistent cancellation of opposite-polarity magnetic flux triggered by p-mode oscillations from the solar interior modulates the possibly intermittent magnetic reconnection and thus controls the 5-min periodicity of the jets. The modulation of magnetic reconnection by p-mode oscillations is more likely to occur in small-scale, low jet events beneath the chromosphere (Chen & Priest 2006;Hansteen et al. 2006;De Pontieu et al. 2007), and further observational evidence is expected to support this.
In this paper, we present high-resolution observations of intermittent jets obtained by the Goode Solar Telescope (GST) operating at the Big Bear Solar Observatory (BBSO), as well as observations by the Solar Dynamic Observatory (SDO) coupled with the Helioseismic and Magnetic Imager (HMI) and the Interface Region Imaging Spectrograph (IRIS). We analyze the dynamic characteristics of the intermittent jets, the line profile, and the Doppler velocity at the footpoints of jets. Additionally, we analyze the transition region brightening phenomenon and the magnetic field environment of the jets studied by a nonlinear force-free-field (NLFFF) analysis in Sect. 2. In Sect. 3 we summarize our results and discuss the influence of granular motions on the triggering mechanism of intermittent jets.
On August 6 2016, intermittent jets were observed between the two main sunspots of negative polarity that formed the leading part of NOAA AR 12571 located at N13W05 with the BBSO coupled with the 1.6-m GST (Goode & Cao 2012) as well as with the SDO (Pesnell et al. 2012) coupled with the HMI (Scherrer et al. 2012;Schou et al. 2012) and the IRIS (De Pontieu et al. 2014). The pointer of the GST was centered on the eastern sunspot in the leading polarity of the active region.
The GST data contain simultaneous observations of the photosphere, using the titanium oxide (TiO) line taken with the Broadband Filter Imager, and the chromosphere, using the H α 6563 Å line obtained with the Visible Imaging Spectrometer (VIS; Cao et al. 2010). The passband of the TiO filter is 10 Å, centered at 705.7 nm, and its temporal resolution is about 15 s with a pixel scale of 0 . 034. A combination of a 5 Å interference filter and a Fabry-Pérot etalon is used at the VIS to obtain a bandpass of 0.07 Å in the H α line. The VIS field of view (FOV) is about 70 with a pixel scale of 0 . 029. To obtain more spectral information, we scanned the H α line at five positions with a step of 0.4 Å following this sequence: ±0.8, ±0.4, 0.0 Å. We obtained a full Stokes spectroscopic polarimetry using the Fe I 1565 nm doublet over a 85 round FOV with the aid of a dual Fabry-Pérot etalon by the NIRIS Spectropolarimeter. Stokes I, Q, U, and V profiles were obtained every 72 s with a pixel scale of 0 . 081. All TiO and H α data were speckle reconstructed using the Kiepenheuer-Institute Speckle Interferometry Package (Wöger et al. 2008).
We first analyzes the vector magnetic field and continuum intensity data given by HMI. Generally, HMI provides four main types of data: dopplergrams (maps of solar surface velocity), continuum filtergrams (broad-wavelength photographs of the solar photosphere), and both line-of-sight and vector mag-netograms (maps of the photospheric magnetic field). The processed HMI continuum intensities and magnetograms data are obtained with a 45 s cadence and a size of 0 . 6 pixels provided by the HMI team. For comparison with NIRIS, we analyzed the HMI magnetograms in the 24 h before the event. Continuum-intensity maps of HMI help us to co-align the TiO and H α images and the magnetograms taken by GST. The GST images taken at each wavelength position were internally aligned using the cross-correlation technique provided by the BBSO programmers.
IRIS provides ultraviolet images focused on the three main channels of the IRIS telescope. Their corresponding wavelengths are far-ultraviolet short (FUVS; 1331.56 Å-1358.40 Å), far-ultraviolet long (FUVL; 1390.00 Å-1406.79 Å), and nearultraviolet (NUV; 2782.56 Å-2833.89 Å). Wideband filters in CCD imaging provide the imaging data for the Slit-Jaw Imager (SJI). IRIS observed in the sit-and-stare spectral mode with one slit located just at the northern edge of the eastern leading sunspot, just in the middle of the FOV of GST. In this study, we used the image from the SJI channels at 2832 Å, 2796 Å, and 1400 Å and the Si IV spectra (see Sect. 3). The coalignment between HMI continuum and GST/IRIS images was achieved by comparing commonly observed features of sunspots in Fe I 6173 Å images and TiO and H α ± 0.8 Å images taken frame by frame.
We are interested in intermittent jets in the leading spot of AR 12571 observed in the H α lines with the GST. According to the sunspot whorls, the helicity of the active region is positive. The event occured between 17:50:53 UT and 21:40:16 UT and lasted for 4 h. Figure 1 shows the temporal evolution of the event for three wavelengths: TiO, H α -0.8 Å, and H α +0.8 Å at four different times, indicating the occurrence of jets throughout observations of nearly 4 h. From the H α blue-wing (-0.8 Å) images, it is evident that the jets predominantly erupted from the right side of the observed spot. The evolution of the images in the TiO show compression motion in the granulation at the jet location, which may trigger magnetic reconnection.
Using the observation data from the H α blue wing (-0.8 Å), we selected the red curve shown in Fig. 2a as the slice position (referred to as S1) and obtained a time-distance diagram of the jet eruption from 17:59:25 UT to 19:58:32 UT (Fig. 2b). It can be observed that the jet continuously erupted at varying heights. Interestingly, between 18:00:00 UT and 18:50:00 UT, the time-distance diagram of the jets shows a certain periodicity. In Fig. 2b, we marked the peak time of jet eruption height with green vertical lines, and it was found that the jet erupted approximately every 5 min during this period. This periodicity is likely related to the magnetic field environment in which the jet is situated.
To investigate the phenomena of intermittent jets in the solar atmosphere above the chromosphere, we obtained Slit-Jaw Imaging (SJI) data from the Interface Region Imaging Spectrograph (IRIS) for three wavelengths: 2832 Å, 2796 Å, and 1400 Å. The IRIS observation data cover approximately two hours from 17:59:26 UT to 19:58:41 UT. To confirm whether these brightenings correspond to the intermittent jets, we overlaid the longitudinal magnetic field data from GST on the SJI A183, page 3 of 14 images of the three wavelengths in Fig. 3. We also identified UV brigthenings in 1400 Å and 2796 Å at the location of the jets. The brightenings precisely correspond to the boundaries of positive and negative magnetic fields, indicating the response of the inter-mittent jets to brightenings in the chromosphere and transition region.
To further investigate the brightening phenomena, we chose the same slice position (S1 in Fig. 2) in the SJI images and A183, page 4 of 14 plotted the time-distance diagrams in 1400 Å and 2796 Å at this slice position (see Figs. 4 and5). The two time-distance diagrams show that the recurring brightening phenomena are presented throughout the two-hour observation period in both 1400 Å and 2796 Å, exhibiting a periodic behavior. We mark the peak time of the brightenings in the time-distance diagrams with vertical blue lines, and we found that the brightenings in 2796 Å and 1400 Å are consistently delayed for 2-3 min compared to the vertical green line in Fig. 2b. This indicates that the intermittent jets require some time to heat the upper solar atmosphere, and these brightening phenomena correspond to the response of intermittent jets in the lower transition region.
No spectral data in this region are available for the IRIS observations,
In order to determine the line-of-sight (LOS) velocity of the intermittent jet material, we created Doppler diagrams of the plasma using the H α 5 wavelength images from the GST observations. We calculated the center of weight of the H α line profile at each pixel to estimate the Doppler shift relative to the reference line center. We averaged the entire observing FOV to obtain the reference line center (except in the region where the sunspot was located), and all the line profiles were corrected by comparing them with a standard H α profile, obtained from the NSO/Kitt Peak FTS data (Su et al. 2016).
Dopplershift maps presenting the LoS velocities are shown in Fig. 6 in blue and red for the blue and redshift motions. The jet exhibits a Doppler blueshift in Fig. 6a and a Doppler redshift in Fig. 6b. This is consistent with the observations in H α , in which the jet displays continuous upflow and downflow over 4 h, indicating that the jet is intermittent. We found that the average upflow speed is up to -13 km s -1 and the average downflow speed is about 11 km s -1 between 18:00 UT and 18:50 UT by using the shift of the central wavelength of the Hα profile. Contrast or cloud model methods for deriving the jet Dopplershifts would lead to upflows and downflows of -40 and 80 km s -1 , respectively.
We normalized the intensity and exposure time of the H α 5 wavelength images. It is worth noting that the reference H α profile (averaged spectral profile of H α in the quiet region) and the footpoint profiles are symmetric.
A183, page 5 of 14 The corrected spectral line profile of the quiet region was used as reference to analyze the footpoint. In Fig. 7a, we selected the footpoint [x, y] = [617, 355] (yellow dot) in the image of H α +0.8 Å. The green curve shows the spectral line profile of the quiet region, and the yellow curve shows the spectral line profile of the footpoint. Compared with the quiet region, the spectral line profile of the footpoint is elevated at the center of the H α line, but there is no obvious change in the line wing, which may be because the footpoint is heated while the jet is mainly controlled by cold plasma, so that there is no obvious heating.
In Fig. 7b, we selected the upflow [x, y] = [637, 556] (blue dot) in the image of H α -0.8 Å. The green curve shows the line profile of the quiet region, and the blue curve shows the line profile of the upflow. The spectral line profile of the jet in the process of eruption is blueshifted, that is, the direction of the eruption is toward the observer. In Fig. 7c, we selected the position of the downflow [x, y] = [704, 477] (red dot) in the image of H α +0.8 Å. The spectral line profile of the downflow is redshifted, that is, the falling direction is away from the observer.
Using SDO/HMI Sharp cea vector magnetogram data, we overlaid the transverse field as arrows on the longitudinal field image to visualize the overall magnetic field information. In Fig. 8a, the negative-polarity magnetic field converges inward, while the positive-polarity magnetic field diverges outward, A183, page 6 of 14 consistent with the direction of the positive and negative magnetic field lines. Additionally, in the regions in which positive and negative magnetic fields intersect, indicated by the nearparallel red and blue arrows, the magnetic field could imply a shearing behavior. This may provide the conditions for magnetic reconnection (see the area inserted with the purple contour in panel a). Figure 8b shows the NIRIS vector magnetogram of the sunspot at the time of 18:00:24 UT obtained by applying the Milne-Eddington (ME) inversion to the Stokes profiles of the Fe I 1565 nm doublet using the inversion code of J. Chae (Degl'Innocenti 1992). The azimuth component of the inverted vector magnetic field was processed to remove the 180 • ambiguity (Leka et al. 2009). A more detailed magnetic field structure appears that is consistent with the SDO/HMI vector magnetogram observations.
Using the data from the BBSO four Stokes components, Fig. 9a shows the image of the longitudinal field. The spot in the center of the field of view is a negative magnetic field, and there is a positive magnetic field in the middle of the spot. The jet occurs in the mixed polar magnetic field region. It may indicate the magnetic flux emergence, magnetic cancellation, and so on. In order to better determine the magnetic field environment of the jet, the high-resolution BBSO longitudinal magnetic field data were superimposed on the H α -0.8 Å image. In Fig. 9b, the footpoint is the junction of positive and negative magnetic fields, near the magnetic neutral line. Compared with IRIS observations (see Fig. 3), we found that the jet corresponds to the brightening phenomenon.
In Fig. 10, using the longitudinal field data of hmi.M_45s, we selected two boundary values of positive and negative magnetic fields to determine the evolution region, and we then calculated the magnetic flux. In Fig. 11, the positive magnetic flux continues to increase, which corresponds to the emergence of a positive magnetic field, while the negative magnetic flux first increases and then decreases, which may imply the cancellation of positive and negative magnetic fields. The emergence and cancellation of positive and negative magnetic fields may result in parallel and opposite-polarity magnetic field components, which may trigger magnetic field reconnection. This might trigger the intermittent jet.
In the evolution images of TiO band, we found that there is an extrusion movement of granulation right of the spot. The local correlation tracking (LCT) method was used to superimpose the horizontal flow velocity of the photosphere on the TiO image to show the motion of granulation.
Panels b and c in Fig. 12 represent the TiO emission in the area inserted in the small box drawn in panel a. This area is on the west side of the sunspot in its penumbra. In this area, the fibrils are not radial but turn counterclockwise around the spot. The fibrils and magnetic field lines are anchored in the penumbra. In panels b and c, elongated granules lie in this area, and around it lie fragmented granules with filigrees in the intergranules and black pores. The horizontal components of the velocity vectors are overlaid on the TiO maps. In a few points, the arrows converge (in panel b point (2,2.5), and (3.5,5). They move southwest to points (in panel c) (1,1) and (4,4). These locations move continuously away from the spot with time as the area of the elongated granules extends toward the quiet Sun.
This continuous motion might favor flux cancellation. The periodicity of the brightenings of around 5 min measured in this region (Figs. 2, 4, and5) would be due to the p-mode oscillations of the photosphere that modulate the radiation in this region.
To identify the magnetic structure of these intermittent jets, we reconstructed the 3D magnetic fields with the NLFFF extrapolation. The NLFFF extrapolation was carried out with the magnetofrictional (MF) method (Guo et al. 2016a,b) that is implemented in the framework of MPI-AMRVAC (Xia et al. 2018;Keppens et al. 2021Keppens et al. , 2023)). The magnetofrictional model simplifies the MHD relaxation process by omitting the effects of inertia, gravity, and pressure gradients, and the velocity is assumed to be proportional to the local Lorentz force. Consequently, the magnetic field evolution is governed by the magnetic induction equation, and the relaxed state approaches a force-free state (Yang et al. 1986). More details regarding the implementation and numerical schemes of the magnetofrictional A183, page 7 of 14 model in the AMRVAC framework can be found in Guo et al. (2016a,b).
We adopted the vector magnetogram (hmi.B_720s) at 18:24 UT observed by the SDO/HMI to reconstruct the coronal magnetic field. To ensure that the observed vector magnetic fields in the photosphere adhere to the assumptions of the boundary condition of the NLFFF model, we performed some preprocessing steps, including correcting projection effects (Guo et al. 2017) and removing the Lorentz force and torque (Wiegelmann et al. 2006). The initial magnetic field for the magnetofrictional model was derived using the Green function method (Chiu & Hilton 1977) with the B z component. The processed vector magnetic fields (B x , B y , and B z ) were imposed on the inner ghost layer of the bottom boundary, and the values in the outer ghost layer were provided by zero-gradient extrapolation. After 60 000 iterations of the magnetofrictional relaxation, the force-free metric (for more details, see Guo et al. 2016b) decreased to half the value of the initial potential field, while the electric current doubled. Figure 13 illustrates the results after 60 000 iterations of the magnetofrictional relaxation.
A183, page 9 of 14 Fig. 10. Observation image of the HMI M45s longitudinal field. The region surrounded by red lines in panels a and b is the positive polar magnetic field evolution region 1 determined by the magnetic field value at 20:30:06 UT of +25 Gauss, and the blue line is the negative polar magnetic field evolution region 2 determined by the magnetic field value at 21:51:16 UT of -120 Gauss. The yellow and green box represent the rectangular region in which the positive and negative magnetic field evolution region, respectively, is located. pink tubes exhibit a morphology the bright structures observed by the IRIS/SJI 1400 Å. On the other hand, the cyan tubes are similar to the observed fibrils in H α red-wing images. These results suggest that our NLFFF model almost retrieves the magnetic-field structures of the observations to a great extent.
Hereafter, to understand the underlying mechanisms resulting in the observed jets, we calculate the distribution of the squashing degree Q (Priest & Démoulin 1995;Demoulin et al. 1996) with the method proposed by Scott et al. (2017). The regions of Q 2 depict the areas in which magnetic connectivity undergoes drastic changes, commonly refereed to as quasiseparatrix layers (QSLs), which outline the favorite places for magnetic reconnection (Titov & Démoulin 1999;Aulanier et al. 2010;Janvier et al. 2013;Guo et al. 2013Guo et al. , 2023;;Li et al. 2022;Zhong et al. 2021). Figure 13f shows selected magnetic fields around the QSLs. It shows that the cyan and orange field lines form an X-shaped configuration featured by the areas with high Q values. The reconnection between them could produce longer pink S-shaped field lines above and the green shorter loops below. A strong squashing factor (Q) value is detected at the base of the jet. This will allow for the field lines to move their direction from north to south and explains the southern component of the jets. For instance, the yellow lines in panel c with southern ends in the high-value Q factor can reconnect toward the south instead of joining the positive northern polarities.
Figure 14a illustrates the configuration of the core magnetic field of the jets. The field lines traced from the electric current channel are sheared and twisted. To quantify the degree of twist, we computed the distribution of the twist number in the same plane as the electric current intensity, denoted as T w , using the open-source code implemented by Liu et al. (2016). As depicted A183, page 12 of 14 in Fig. 14b, the high-T w region forms a quasi-circular shape, corresponding to the electric current channel in Fig. 14a. Furthermore, the twist number of the purple field line in Fig. 14a can reach a value of 0.82, which is formed due to magnetic reconnection illustrated in Fig. 13. Taken as a whole, the investigation of the 3D magnetic fields indicates that magnetic reconnection might cause the observed jets. This agrees with our observations.
We checked the IRIS Si IV spectra along the slit indicated in Fig. 13d. Two mini flares were registered at this location. During one flare at 18:33 UT, bilateral flows occur (Fig. 13d inset). This indicates reconnection between the strands of the jet (Ruan et al. 2019).
We reported coordinated observations with the GST at BBSO, SDO/HMI, and IRIS SJI of active region NOAA 12571 on August 6 2016. The observed event shows intermittent jets that occur right of a negative-polarity sunspot.
We obtained the following results: 1. In the H α ± 0.8 Å, we found a persistent jet right of the sunspot that lasted for up to 4 h. The intermittent jets exhibited outward-diverging dark absorption features. The timedistance diagram shows that the peak of the jet has clear periodic eruption characteristics (5 min) during 18:00 UT-18:50 UT. 2. We also observed a periodic brightening in the transition region during the jets, which was reflected in the timedistance diagram. This may be a response of the intermittent jets in the higher solar atmosphere. 3. By calculating the Doppler velocities of the jets, we found alternating redshifts and blueshifts during the eruption that correspond to the intermittent eruptive nature of the jets. The average velocities of the upflow and downflow are -13.47 km s -1 and 11.11 km s -1 , respectively, when we consider the displacement of the central wavelength in the Hα profiles. 4. Compared to the quiet region of the Sun, we found that the spectral line profiles at the footpoint showed an intensity increase at the line center, but no significant changes in the line wings. This indicates prolonged heating at the footpoints. 5. In the vector magnetograms of the intermittent jets, we observed a strong shear behavior in the magnetic field near the neutral line. This provides a favorable magnetic environment for magnetic reconnection. 6. By overlaying the BBSO longitudinal magnetic field onto the H α and the IRIS SJI images in three wavelengths, we determined that the footpoints were located on the neutral line, corresponding to the brightening in the transition region and lower chromosphere. The magnetic flux evolution diagram shows that positive magnetic flux emerges continuously, and negative magnetic flux first increases and then decreases, indicating that the magnetic field has a long-duration emergence and cancellation behavior. 7. The evolution image in the TiO wavelength shows horizontal motions of the granulation at the location of jets. Granules intrude in this place. This may contribute to the compression of opposite-polarity magnetic fields and might trigger magnetic reconnection. 8. The magneto-topology analysis for the 3D NLFFF model confirms the possibility that magnetic reconnection in the corona is the main mechanism for the production of inter-mittent jets. This is also confirmed by spectroscopy data with bilateral flows. 9. The magnetic field lines containing the jets are anchored in the mixed magnetic polarity channel inside the negativepolarity spot. Magnetic reconnection has been widely accepted as the driving mechanism of most solar eruptive events. Many small-scale events in the solar atmosphere, such as solar jets (Asai et al. 2001;Mulay et al. 2016;Raouafi et al. 2016;Shen 2021). Many observational events can be explained by magnetic reconnection between preexisting open magnetic field lines and newly emerging magnetic fields, and the magnetic cancellation driven by newly emerging magnetic bipoles can be regarded as slow magnetic reconnection in the lower solar atmosphere (Wang & Shi 1993;Jiang & Wang 2000). The appearance of microflares, the converging form of EUV jets, and the relation between their footpoints and annular flare brightenings all serve as evidence of magnetic reconnection in jets (Shibata 1998).
In this paper, the intermittent jet occurred in a mixed-polarity region at the boundary negative magnetic fields. By overlaying the magnetic field onto the observed images of the jets, we found that jets were located near the neutral line. The evolution of the magnetic flux showed a prolonged magnetic flux emergence and magnetic cancellation. This provides a favorable magnetic environment for the intermittent jets that continuously drive the ejection of plasma material. Furthermore, in the observations of the photosphere, we found horizontal motion of the granulation in the eruption area.
The relative motion between granulation and the magnetic field along the neutral line may lead to flux cancellation, which is favorable for initiating jets (Tian et al. 2017;Yang et al. 2015;Li et al. 2020). The magnetic field lines could be submitted to the oscillations present in the sunspot and its environment. We showed some evidence that magnetic reconnection could be the mechanism that triggers the intermittent jets, although to confirm the temporal nature of our proposed mechanism, a time series of extrapolations is required.
Previous studies have investigated the triggering of repetitive jets by magnetic emergence and cancellation (Zhang & Ji 2014;Chae et al. 1999;Liu et al. 2016;Zeng et al. 2013), but most events lack a periodicity. However, Ning et al. (2004), Doyle et al. (2006), Chandra et al. (2015) discovered repetitive eruptive events in the transition region with quasi-periodic characteristics. Wang et al. (2021Wang et al. ( , 2023) ) analyzed jets that also exhibited quasi-periodic features of approximately 5 min, and Hong et al. (2022) observed long-duration microjets that displayed a quasi-periodic behavior of approximately 5 min. Additionally, Chen & Priest (2006) used MHD simulations to demonstrate the scenario of periodic magnetic reconnection modulated by p-mode oscillations in eruptive events.