Helical motions of prominence threads

Helical motions of fine-structure prominence threads observed by Hinode and IRIS


Fine-structure dynamics in solar prominences holds critical clues to understanding their physical nature of significant space-weather implications. We report evidence of rotational motions of horizontal helical threads in two active-region prominences observed by the Hinode and/or IRIS satellites at high resolution. In the first event, we found transverse motions of brightening threads at speeds up to 55 km s seen in the plane of the sky. Such motions appeared as sinusoidal space–time trajectories with a typical period of 390 s, which is consistent with plane-of-sky projections of rotational motions. Phase delays at different locations suggest propagation of twists along the threads at phase speeds of 90–270 km s. At least 15 episodes of such motions occurred in two days, none associated with any eruption. For these episodes, the plane-of-sky speed is linearly correlated with the vertical travel distance, suggestive of a constant angular speed. In the second event, we found Doppler velocities of 30–40 km s in opposite directions in the top and bottom portions of the prominence, comparable to the plane-of-sky speed. The moving threads have about twice broader line widths than stationary threads. These observations, when taken together, provide strong evidence for rotations of helical prominence threads, which were likely driven by unwinding twists triggered by magnetic reconnection between twisted prominence magnetic fields and ambient coronal fields.

Sun: filaments, prominences

1 Introduction

Solar prominences are dense, cool plasma residing at elevated heights in the tenuous, hot corona (for recent reviews, see Labrosse et al., 2010; Mackay et al., 2010). According to their relative locations with respect to active regions, they are generally classified into three types: active-region, quiescent, and intermediate prominences (e.g., Engvold, 1998; Mackay et al., 2010; Vial & Engvold, 2015). They have two magnetic-field configurations: normal (Kippenhahn & Schlüter, 1957) and inverse (Kuperus & Raadu, 1974), depending on whether the predominantly horizontal magnetic field threading the prominence material is in the same or opposite direction with respect to the underlying ambient field. There is a correlation between the two configurations and the maximum height of the prominence (Leroy et al., 1984). The inverse configuration is of particular significance, because it can host a helical magnetic flux rope (Karpen et al., 2003), believed to be the progenitor a coronal mass ejection (CME; e.g., Pneuman, 1983; Priest et al., 1989; van Ballegooijen & Martens, 1990; Rust & Kumar, 1994; Amari et al., 1999; Low & Petrie, 2005). Evidence for the inverse configuration or its helical structure has been obtained from polarimetric measurements of the photosphere and chromosphere (e.g., Lites, 2005; López Ariste et al., 2006; Okamoto et al., 2009; Kuckein et al., 2012) and observations of erupting prominences and associated CMEs (e.g. Yurchyshyn, 2002; Maričić et al., 2004; Vršnak et al., 2004; Gibson et al., 2006; Liu et al., 2015).

Although a prominence as a whole can appear macroscopically stationary, it often consists of numerous microscopically dynamic threads. Fine-structure horizontal threads have been identified in active-region prominences and vertical threads in hedgerow, quiescent prominences (Engvold, 1976; Lin et al., 2005). Horizontal threads can travel along magnetic field lines (Zirker et al., 1998) and exhibit transverse oscillations as manifestations of Alfvénic waves (e.g., Okamoto et al., 2007; Lin et al., 2009). In addition, recent high-resolution observations revealed a variety of small-scale dynamics, such as rising dark plumes and bubbles (Berger et al., 2008, 2010), upward plasma blob ejections (Hillier et al., 2011), descending knots (Chae, 2010), and horizontally-moving bright blobs (Lin et al., 2012). Such motions can provide useful diagnostics for various physical quantities, e.g., with a technique called prominence seismology (Terradas et al., 2008; Soler et al., 2009; Oliver, 2009; Arregui et al., 2012).

Among various prominence fine-structure dynamics, rotational motions are of particular importance, because they are directly relevant to magnetic helicity and free energy, key parameters governing the evolution and ultimate fate a magnetic flux rope. Such motions can be grouped in two categories: flows of mass along largely static, helical magnetic field lines and bodily rotations involving magnetic fields themselves. Category I includes flows along circular paths (projected onto the plane of the sky) detected in H images and spectra (Öhman, 1969; Liggett & Zirin, 1984) and in coronal cavities seen in EUV images (Li et al., 2012; Panesar et al., 2013). Category II includes structural rotations of the prominence (together with its frozen-in magnetic fields) as a whole about its horizontal spine (Williams et al., 2009) or in part about a vertical axis within a so-called “tornado” (Orozco Suárez et al., 2012; Su et al., 2014), the latter of which was argued to be actually a prominence barb where counter-streaming flows along fine threads (Lin et al., 2003) were mistaken as apparent rotations (Panasenco et al., 2014).

All the prior observations of prominence rotations were obtained with limited spatial and/or temporal resolution and thus left considerable ambiguities such as the debate on the nature of “tornadoes”. High spatio-temporal and spectral resolutions are in critical need to resolve such ambiguities and to provide new insights to the details of the physical processes involved. Here we present such observations of two active-region prominences showing clear signatures of rotational motions of horizontal threads. Both events were observed by the Solar Optical Telescope (SOT; Tsuneta et al., 2008; Shimizu et al., 2008; Suematsu et al., 2008) on board the Hinode satellite (Kosugi et al., 2007) offering the highest spatial resolution of the Sun ever achieved in space. The second event was also observed by the Interface Region Imaging Spectrograph (IRIS; De Pontieu et al., 2014) providing critical Doppler measurements with high spectral resolution. In what follows, we present observations and data analysis results in Section 2 and interpretations and discussions in Section 3.

2 Observations

2.1 Event 1: 2007 February 8–10

The Hinode satellite observed the west limb of the Sun from 11:00 UT on 2007 February 8 to 10:49 UT on February 10. We obtained 18,889 images of an active region prominence in NOAA AR 10940 with the SOT Ca ii H-line filter (3968 Å, bandwidth 3 Å) at a spatial sampling of . We had a 108″108″ (10241024 pixel) field of view (FOV), a 0.3 s exposure time, and an 8 s cadence with occasional interruptions because of synoptic observations and data losses. We note that this dataset were also analyzed by Nishizuka et al. (2008) and Liu et al. (2009) for helical chromospheric jets and Zhang et al. (2012) for mass flows in the prominence.

The prominence was elongated in the north-south direction according to H images taken two days earlier (see the left panel of Figure 1). Figure 2 shows a snapshot of Ca ii H-line observed at 17:14 UT on February 8 (also see Movie 1). This prominence consisted of horizontal fine threads with a typical width of 350 km (), as is the case with a typical active region prominence (e.g., Okamoto et al., 2007). While the prominence configuration as a whole remained stationary, each individual thread had gentle horizontal flows and small vertical oscillations. At times, a bundle of bright threads suddenly appeared in the prominence and moved transversely upward, with each thread following one another sequentially. The threads were not exactly parallel to the solar limb, but slightly inclined. After reaching their maximum heights, some threads turned around and moved transversely downward or flowed horizontally along presumably magnetic field lines (also discussed in Zhang et al., 2012). An example of this process is shown in Figure 3.

We selected a bright blob within a thread and made a space–time plot using a vertical cut to track its motion (see top panels in Figure 4). The blob appeared at the top of the prominence and then moved downward. Interestingly, its space–time trajectory has a sinusoidal shape, which is consistent with a line-of-sight projection of rotation about an axis nearly parallel to the plane of the sky. The plane-of-sky speed varied with time and had a maximum of 55 km s near the middle of the prominence and approached zero at the top and bottom edges. The lower-right panel in Figure 4 shows the same space–time plot superimposed with projected trajectories expected from a rotational motion with a period of 390 s and a radius increasing at a rate of 4.5 km s. Notably the brightest trajectory near  s, corresponding to the selected bright blob, is well fitted by the presentative curve.

We detected phase delays of sinusoids in space–time plots from different vertical cuts as shown in Figure 5. If the inferred rotational motion is the case, the phase delays indicate that the threads are not parallel, but inclined to their rotational axis along the prominence spine. In other words, the threads are not aligned along a straight cylinder, but in a helical shape. Specifically, the phase delay from cut F to A in Figure 5 suggests a propagation of twists from right to left, i.e., in the direction toward the first appearance of bright threads. The time delays and spatial separations between the cuts translate to a propagation speed that drops with distance from 270 to 90 km s. Considering the typical period of 390 s noted above, the wavelength or pitch of helix thus falls in the range of 35 – 105 Mm. We note a typical value of 20 km s for the maximum transverse speed measured in Figure 5, which corresponds to the rotational speed . We thus obtain the pitch angle of the helical threads in the range of 4 – 13.

Within the two days of observations, appearances of bright thread bundles and subsequent transverse motions repeatedly took place for at least 15 episodes (Figure 6). None of these episodes was associated with any flare or eruptive phenomenon. Each episode lasted from a few to 20 minutes and the bright threads did not reach beyond the maximum height of the prominence. One episode (#14) showed only downward motions of bright threads, while the other episodes had both upward and downward motions. From the corresponding space–time plots, we measured the maximum velocity , vertical travel distance , and duration of the vertical motions of the bright threads in each episode, which are summarized in Table LABEL:tab1. Note that these quantities are typical values for each episode, not for individual threads.

Interestingly, as shown in Figure 7, the maximum velocity and vertical travel distance are strongly correlated with a linear correlation coefficient of . This is again consistent with the inferred plane-of-sky projections of prominence rotations, if and correspond to the rotational speed and diameter, respectively, and thus implies a constant angular velocity or period. Under this assumption, we estimate the rotation period to be , which has a statistical mean of 370 s for all 15 episodes. This value is close to the period of 390 s estimated for one of the episodes using sinusoidal fits to space–time trajectories, as shown in Figure 4. That approach could not be applied to the rest of the episodes, because of lack of well-defined crests and troughs in those trajectories mainly due to line-of-sight overlaps of numerous threads. We note in passing that the linear fit in Figure 7 does not go through the origin, possibly due to a systematic overestimate of the vertical travel distance.

2.2 Event 2: 2013 October 19

We conducted coordinated HinodeIRIS observations of an active region prominence in NOAA AR 11877 (right panel of Figure 1 and also see Movie 2) at the southeast limb on 2013 October 19. Hinode/SOT took 585 images with the Ca ii H line filter at a cadence of 8 s from 09:09 to 10:27 UT. The FOV was 108″108″ (10241024 pixel) and the exposure time was 1.2 s. IRIS performed 360 sets of four-step sparse raster scans from 09:00 to 11:00 UT. The cadence was 20 s between slit locations with spatial and spectral resolutions of (240 – 290 km on the Sun) and 3 km s, respectively. The slit covered 175″ length and the exposure time was 4 s.

Figure 8 shows the observed prominence. We note that this is the same prominence analyzed by Okamoto et al. (2015) and Antolin et al. (2015), who found evidence of resonant absorption of transverse oscillations and associated heating. They focused on the higher portion of the prominence where minimum line-of-sight overlap allowed for spatially resolving fine threads and small-scale dynamics. Here we focused on the prominence’s lower portion, which shows evidence of rotational motions with amplitudes on the order of 10,000 km, about 10 times those of the transverse oscillations in the higher portion of the prominence reported by Okamoto et al. (2015). First, we examined the plane-of-sky motions using SOT data. Similar to Event 1, while the prominence was stationary as a whole, sudden appearances of bundles of bright threads took place. The bottom panels in Figure 8 show space–time plots of running-difference images obtained from vertical cuts S1–S5 shown as green dashed lines in the top panel. The bright threads moved upward sequentially at typical speeds of 30 – 45 km s. The top edge of the bundle, best seen within cuts S1 and S3, also shifted upward at a speed of 10 km s. We note that only a small portion of the prominence threads near their right end was covered by the IRIS slits. The lowest slit position intersects cuts S4 and S5 at locations marked by plus signs P1 and P2, respectively. As clearly seen in the online movie, the transverse motions of the threads and ensuing horizontal flows mainly occurred to the left of cut S5 whose space–time plot shows no clear signature of such motions.

Next, we analyzed the spectral data taken by IRIS. We focused on the strong Mg ii k line that has sufficient signal to noise ratio required for spectral fits. In general, the Mg ii k line profile in on-disk observations has a central reversal in the emission peak within an even broader absorption component, which are produced by a complex radiative transfer process (Leenaarts et al., 2013a, b; Pereira et al., 2013). In off-limb observations, as long as there is no spatial overlap of different features along the line of sight, the profile is simple with a single, Gaussian-shaped peak indicative of optically thin emission (e.g., Schmieder et al., 2014; Liu et al., 2015; Vial et al., 2016). This is indeed the case for most parts of our observed prominence. Let us examine the spectra at the locations of the bright threads. Figure 9 shows time-series of the spectra before and after the bright threads passed through the positions at the cyan and pink plus signs (P1 and P2) in Figure 8. At P1, the spectrum in the beginning had a single Gaussian profile with a negligible Doppler velocity (4 km s) that corresponds to the rest component. As time progresses, while the rest component remained without significant changes, an enhancement in the blue wing appeared with a Doppler velocity up to  km s. This blueshifted component represents a new feature appearing in front of or behind (along the line of sight) the pre-existing rest component. Likewise, the spectrum at P2 also showed double components, but with a dominant red-wing enhancement. Noting that P1 and P2 are respectively located in the top and bottom portions of the bundle of threads, these opposite Doppler shifts indicate a clockwise rotation6 (when viewed from left to right in Figure 8) of the prominence about an horizontal axis within/near the plane of the sky. To satisfy the continuity condition, the threads seen transversely moving upward must be located on the back side of the rotating structure.

Figure 10 shows history of the Doppler velocity and the line width at positions P1 and P2 derived from double or single Gaussian fits (see examples in Figure 9). The bright prominence threads exhibited large Doppler velocities up to 30–40 km s of dominant blueshifts at P1 and redshifts at P2. Both components had broad line widths of 20 km s, about twice those of the corresponding rest components. We note that the dominant blue components at P1 appeared about 14 min earlier and had slightly greater Doppler velocities than the red ones at P2. This is because the IRIS slit was inclined to the threads and thus it sampled different parts of the horizontal extent of the prominence, with a lag in arrival time of horizontal flows at the slit locations.

3 Summary and Discussion

We have reported two events in which bright bundles of horizontal prominence threads appeared and exhibited transverse motions in the vertical direction. In the first event (see Section 2.1), we found sinusoidal trajectories of bright threads in space–time plots, which are consistent with plane-of-sky projections of rotational motions. Clear phase delays suggest that those threads are not straight, but of helical shapes. Further and more decisive evidence of rotation was found in the second event (Section 2.2) exhibiting similar transverse motions in the sky plane at speeds up to 45 km s, which were accompanied by Doppler velocities of comparable magnitudes up to 30 – 40 km s in opposite directions near the top and bottom edges of the prominence. The combination of consistent plane-of-sky and line-of-sight motions observed here allows us to conclude that these events involved bodily rotations of helical prominence threads.

Although rotations have been observed in prominences (e.g., Williams et al., 2009) and helical jets (e.g., Liu et al., 2009), our observations were obtained with the highest spatial and spectral resolution ever achieved together in space. The rotations of helical threads reported here fall into the second category of prominence rotations mentioned in Section 1, i.e., structural rotations rather than mass flows along field lines (Category I). The novelty of these observations lies in the fact that such rotations involve certain portions of horizontal threads, which differs from previously reported Category II rotations of an entire prominence (e.g., Williams et al., 2009) or of the debatable “prominence tornado” about a vertical rotational axis (e.g., Su et al., 2014). We provide below an interpretation of the observed phenomenon and discuss its implications.

3.1 Interpretation and Basic Scenarios

This phenomenon occurred episodically in otherwise stationary prominences, with no indication of solar flares, jets, or other catastrophic processes. This means that the integrity of the overall magnetic geometry must remain largely unchanged through these episodes. Whatever process is, changes to the magnetic field must be minor and gentle, and the involved energy release is small, insufficient to cause an eruption. With these inferences, we propose two possible scenarios, schematically shown in Figure 11, to explain the observations. In both scenarios, magnetic reconnection plays an important role in transferring twists and magnetic helicity from highly twisted fields to less twisted or untwisted fields and in triggering the unwinding rotational motions of helical prominence threads.

In Scenario A (Figure 11, left), when highly twisted helical flux emerges into the atmosphere and reaches the height of prominence threads of straight or less twisted magnetic field, magnetic reconnection between the two flux systems can occur. Magnetic helicity and twists can be transferred to the prominence field so as to cause it to rotate. The propagation of twists can also explain the observed phase delays along the prominence threads for projected sinusoidal transverse motions.

In Scenario B (Figure 11, right), the helical prominence magnetic field is assumed to be more twisted than the ambient field, e.g., of the neighboring coronal loops. Magnetic reconnection between them would cause transfer of twists and helicity in an opposite direction, i.e., away from the prominence, compared with Scenario A. As such, the helical prominence threads would undergo unwinding rotational motions and relaxation until a new equilibrium state is reached with twists evenly distributed along the entire, newly reconnected field line.

Our observations suggest that Scenario B is more likely. In the case of the helical flux emergence (Scenario A), the effects of rotations would propagate upward from the lower atmosphere, where we found no such signature. In addition, flux emergence, because of its usually large free magnetic energy content, could cause more dramatic response such as jets (Kurokawa et al., 1987), as detected in the same Hinode/SOT dataset for Event 1 (Nishizuka et al., 2008; Liu et al., 2009). In both events here, the change of the magnetic configuration appeared gentle. It is thus more likely the case that reconnection occurred between twisted prominence fields and ambient coronal loops. Moreover, the observed twist propagation is consistent with this scenario, in which the unwinding motion traveled from the twisted part of the prominence to the less-twisted part where the brightening threads first appeared, suggestive of heating or energy release caused by magnetic reconnection there. Note that the rate or amount of energy release is likely not high enough to cause significant heating at coronal temperatures of a sufficiently large volume to be detected by AIA, because we found no clear signature of brightening in AIA passbands (which also have a spatial resolution of , much smaller than Hinode or IRIS).

3.2 Discussion on Helical Motions of Prominence Threads

Our observed prominence activations were not associated with drastic activities such as flares. In contrast, with on-disk observations by the Hinode EUV Imaging Spectrometer (EIS), Williams et al. (2009) detected a prominence with a somewhat smaller rotational speed of 20 km s before a flare occurred. In their case, the entire prominence rotated synchronously like a cylinder. They suggested that the rotation was caused by some change in the surrounding magnetic environment, such as small-scale flux emergence (Moore & Roumeliotis, 1992) which is consistent with our Scenario A, or by some form of the so-called break-out process (Antiochos et al., 1999; Aulanier et al., 2000). The change of magnetic configuration affected the entire prominence and thus led to its synchronous rotation. In our case, the prominence, at least in Event 2, was not rotating entirely, because we detected both the rotational and stationary components simultaneously (Figure 9). Therefore, it is more likely that reconnection took place only in some part of the prominence magnetic field, as shown in Figure 11 for Scenario B.

Measurements of magnetic helicity or twists can provide critical clues to the generation of magnetic fields either by convective dynamo action or differential rotation (see e.g., Pevtsov et al., 1995). This is one of the most important issues in prominence research in regard to the mechanism of prominence formation. However, in both events, the pitch angle of the helical prominence threads and thus of their frozen-in magnetic-field lines is very small, on the order of or smaller. This introduces large uncertainty or ambiguity in determining the sign of the pitch angle with respect to the rotational axis. Therefore, we could not infer the handedness of the helical field lines here, unlike in other case (e.g., Liu et al., 2015) with large pitch angles combined with simultaneous plane-of-sky and Doppler velocity measurements.

The Hinode and IRIS observations presented here, at a level of clarity not previously achieved, have offered new insights to rotational motions of fine-structure prominence threads. Additional observations in even greater detail, including temperature measurements, will soon be provided by the Atacama Large Millimeter/submillimeter Array (ALMA) in its observing Cycle 4 starting 2016 (see Wedemeyer et al., 2016). We anticipate to utilize the combination of such unprecedented observations to further probe the physics of prominence activations and related phenomena.

Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in cooperation with ESA and NSC (Norway). IRIS is a NASA small explorer mission developed and operated by LMSAL with mission operations executed at NASA Ames Research center and major contributions to downlink communications funded by ESA and the Norwegian Space Centre. T.J.O. thanks Ippon-kakou-kai for their encouragement and was supported by JSPS KAKENHI Grant Number 25800120/16K17663 (PI: T.J.O.) and 25220703 (PI: S. Tsuneta). W.L. is supported by IRIS Guest Investigator grant NNX15AR15G and NASA contract NNG09FA40C (IRIS). This work was partly carried out on the Solar Data Analysis System operated by the Astronomy Data Center in cooperation with the Hinode Science Center of NAOJ.
Episode Maximum velocity Duration Vertical travel distance
(km s) (s) (km)
1 22 270 3120
2 10 540 2150
3 11 510 4150
4 34 480 4440
5 55 1220 9130
6 56 490 7770
7 24 400 5410
8 22 620 4050
9 35 1220 6300
10 10 1130 2720
11 38 990 8310
12 44 960 5660
13 12 400 3300
14 14 840 3200
15 15 990 4120
Range 10–56 270–1220 2150–9130
Mean 27 737 4922
Median 22 620 4150
Table 1: Characteristics of detected episodes of transverse motions in the vertical direction of horizontal prominence threads in Event 1.
Figure 1: H images from the Solar Magnetic Activity Research Telescope (SMART) at the Hida Observatory showing the two prominences of interest and their associated active regions, two days before (left) and after (right) the events under study when they appeared at the solar limb. The white boxes indicate the Hinode/SOT’s FOV at the limb, while the black dashed boxes mark the observing targets at their corresponding disk locations.
Figure 2: Snapshot of the prominence in Event 1 observed in the Ca ii H line by Hinode/SOT at 17:14:10 UT on 2007 February 8. The solar north is to the left and the west is up. The red brackets indicate the FOV of Figure 3 showing the sudden appearance of bright threads. The blue and green brackets mark the regions for rotational motions shown in Figure 4 and propagating waves shown in Figure 5, respectively. The white dotted line indicates a vertical cut that was used to make the space-time plot in Figure 6. (An animation of this figure is available.)
Figure 3: Time-series of Ca ii H images in the red-boxed region of Figure 2 showing prominence threads undergoing brightening. The two top rows are intensity maps, while the two bottom rows are running differences between consecutive images to emphasize the transversely moving threads that appear as adjacent bright and dark stripes. The reference () for the time stamps (in sec) is 16:58:50 UT on February 8.
Figure 4: Snapshot (left panel) showing prominence threads in the blue box of Figure 2 and space–time plots (right panels) obtained from a vertical cut (dashed line on the left) located on a bright blob. The two right panels are identical, but the bottom one is overlaid with representative sinusoidal curves that correspond to projected trajectories of assumed rotations (period 390 s) of a bundle of threads that expand radially at a rate of 4.5 km s. The origin of time on the horizontal axis is 16:58:10 UT on February 8.
Figure 5: Left: Snapshot image of swaying threads seen in the green box shown in Figure 2. Right: Space–time plots obtained from vertical cuts A – F, evenly spaced in the horizontal direction, as shown on the left. We identified one prominent thread captured by all cuts. Its corresponding peak excursions in space–time plots are delayed in time, indicative of propagation of twists at speeds of 270 km s from cut F to E and 90 km s from cut B to A. The reference time is 17:07:29 UT on February 8.
Figure 6: Diagram of prominence evolution over two days for Event 1. The upper panels are snapshots of each episode of recurrent activations. The red ovals mark the appearances of bright threads. The lower panel is a space–time plot obtained from a selected vertical cut along the white dotted line in Figure 2. The white dashed curve indicates the plane-of-sky projection of the prominence height assumed to be constant at 16,500 km (23″), whose temporal variation is caused by the solar rotation. The red horizontal bars in the lower panel indicate times of occasional interruptions and data loss.
Figure 7: Scatter plot showing the correlation between the maximum velocity and the travel distance of vertical motions of bright threads for Event 1. The solid line represents a linear fit to the data, which has a linear correlation coefficient of .
Figure 8: Top: Snapshot of the prominence in Event 2 observed in the Ca ii H line by Hinode/SOT at 10:05:24 UT on 2013 October 19. The four inclined white lines indicate the IRIS slit locations. The green dashed lines (S1–S5) cover the locations of the bundles of appearing bright threads. Two locations at P1 and P2 are used to show the spectra of bright threads in Figures 9 and 10. The FOV is rotated to have the solar limb oriented horizontally. Bottom: Space–time plots of running difference images obtained from vertical cuts marked by S1–S5 in the top panel. (An animation of this figure is available.)
Figure 9: Time series of Mg ii k spectra at the positions of the two plus signs P1 and P2 shown in Figure 8. Black plus signs here present the original data. Thick gray and orange curves are single and double Gaussian fits, respectively. For double Gaussian fits, the thin black curve is the rest component, while the thin blue/red curve is the blue-/red-shifted component. The thick black and blue/red bars indicate the central wavelengths of the corresponding Gaussian components.
Figure 10: Temporal evolution of the Doppler shift and line width at positions P1 and P2 shown in Figure 8. Red and blue symbols represent red and blue components derived from double Gaussian fits, respectively. Gray symbols are from single Gaussian fits in cases of failure of double Gaussian fits. The vertical dotted lines indicate the start times of the spectra shown in Figure 9, which exhibit dominant blueshifts at P1 and redshifts at P2, as marked by the black boxes.
Figure 11: Schematic of two possible scenarios that can explain the observed prominence rotation. Both scenarios involve magnetic reconnection between twisted and untwisted field lines and transfer of twists and magnetic helicity. Left: Emerging helical flux reconnects with the prominence field and triggers its rotation. Right: Helical prominence field reconnects with the ambient field and the ensuing unwinding relaxation causes the prominence to spin. The numbered labels in each scenario indicate the temporal development.


  1. affiliationtext: National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan
  2. affiliationtext: Bay Area Environmental Research Institute, 625 2nd Street, Suite 209, Petaluma, CA 94952, USA
  3. affiliationtext: Lockheed Martin Solar and Astrophysics Laboratory, 3251 Hanover Street, Bldg. 252, Palo Alto, CA 94304, USA
  4. affiliationtext: W. W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, USA
  5. affiliationtext: ISAS/JAXA, Sagamihara, Kanagawa 252-5210, Japan
  6. Note that there is a possibility that these opposite Doppler shifts are indications of counter-streaming flows, commonly seen in prominence threads (e.g., Lin et al., 2003). However, this possibility is very small in our case, given the two observational facts that (1) the opposite Doppler shifts are detected right at the top and bottom edges of the transverse motions of the thread bundle, and (2) the Doppler and transverse velocities have similar magnitudes of 40 km s. Therefore, these facts naturally fit in the picture of prominence rotation, but it would be very coincidental for a counter-streaming scenario to be applicable here.


  1. Amari, T., Luciani, J. F., Mikic, Z., & Linker, J. 1999, ApJ, 518, L57
  2. Antiochos, S. K., DeVore, C. R., & Klimchuk, J. A. 1999, ApJ, 510, 485
  3. Antolin, P., Okamoto, T. J., De Pontieu, B., et al. 2015, ApJ, 809, 72
  4. Arregui, I., Oliver, R., & Ballester, J. L. 2012, Living Reviews in Solar Physics, 9, 2
  5. Aulanier, G., DeLuca, E. E., Antiochos, S. K., McMullen, R. A., & Golub, L. 2000, ApJ, 540, 1126
  6. Berger, T. E., Shine, R. A., Slater, G. L., et al. 2008, ApJ, 676, L89
  7. Berger, T. E., Slater, G., Hurlburt, N., et al. 2010, ApJ, 716, 1288
  8. Chae, J. 2010, ApJ, 714, 618
  9. De Pontieu, B., Title, A. M., Lemen, J. R., et al. 2014, Sol. Phys., 289, 2733
  10. Engvold, O. 1976, Sol. Phys., 49, 283
  11. Engvold, O. 1998, IAU Colloq. 167: New Perspectives on Solar Prominences, 150, 23
  12. Gibson, S. E., Foster, D., Burkepile, J., de Toma, G., & Stanger, A. 2006, ApJ, 641, 590
  13. Hillier, A., Isobe, H., & Watanabe, H. 2011, PASJ, 63, L19
  14. Karpen, J. T., Antiochos, S. K., Klimchuk, J. A., & MacNeice, P. J. 2003, ApJ, 593, 1187
  15. Kippenhahn, R., & Schlüter, A. 1957, ZAp, 43, 36
  16. Kosugi, T., Matsuzaki, K., Sakao, T., et al. 2007, Sol. Phys., 243, 3
  17. Kuckein, C., Martínez Pillet, V., & Centeno, R. 2012, A&A, 539, A131
  18. Kuperus, M., & Raadu, M. A. 1974, A&A, 31, 189
  19. Kurokawa, H., Hanaoka, Y., Shibata, K., & Uchida, Y. 1987, Sol. Phys., 108, 251
  20. Labrosse, N., Heinzel, P., Vial, J.-C., et al. 2010, Space Sci. Rev., 151, 243
  21. Leenaarts, J., Pereira, T. M. D., Carlsson, M., Uitenbroek, H., & De Pontieu, B. 2013a, ApJ, 772, 89
  22. Leenaarts, J., Pereira, T. M. D., Carlsson, M., Uitenbroek, H., & De Pontieu, B. 2013b, ApJ, 772, 90
  23. Leroy, J. L., Bommier, V., & Sahal-Brechot, S. 1984, A&A, 131, 33
  24. Li, X., Morgan, H., Leonard, D., & Jeska, L. 2012, ApJ, 752, L22
  25. Liggett, M., & Zirin, H. 1984, Sol. Phys., 91, 259
  26. Lin, Y., Engvold, O. R., & Wiik, J. E. 2003, Sol. Phys., 216, 109
  27. Lin, Y., Engvold, O., Rouppe van der Voort, L., Wiik, J. E., & Berger, T. E. 2005, Sol. Phys., 226, 239
  28. Lin, Y., Soler, R., Engvold, O., et al. 2009, ApJ, 704, 870
  29. Lin, Y., Engvold, O., & Rouppe van der Voort, L. H. M. 2012, ApJ, 747, 129
  30. Lites, B. W. 2005, ApJ, 622, 1275
  31. Liu, W., Berger, T. E., Title, A. M., & Tarbell, T. D. 2009, ApJ, 707, L37
  32. Liu, W., De Pontieu, B., Vial, J.-C., et al. 2015, ApJ, 803, 85
  33. López Ariste, A., Aulanier, G., Schmieder, B., & Sainz Dalda, A. 2006, A&A, 456, 725
  34. Low, B. C., & Petrie, G. J. D. 2005, ApJ, 626, 551
  35. Mackay, D. H., Karpen, J. T., Ballester, J. L., Schmieder, B., & Aulanier, G. 2010, Space Sci. Rev., 151, 333
  36. Maričić, D., Vršnak, B., Stanger, A. L., & Veronig, A. 2004, Sol. Phys., 225, 337
  37. Moore, R. L., & Roumeliotis, G. 1992, IAU Colloq. 133: Eruptive Solar Flares, 399, 69
  38. Nishizuka, N., Shimizu, M., Nakamura, T., et al. 2008, ApJ, 683, L83
  39. Öhman, Y. 1969, Sol. Phys., 9, 427
  40. Okamoto, T. J., Tsuneta, S., Berger, T. E., et al. 2007, Science, 318, 1577
  41. Okamoto, T. J., Tsuneta, S., Lites, B. W., et al. 2009, ApJ, 697, 913
  42. Okamoto, T. J., Antolin, P., De Pontieu, B., et al. 2015, ApJ, 809, 71
  43. Oliver, R. 2009, Space Sci. Rev., 149, 175
  44. Orozco Suárez, D., Asensio Ramos, A., & Trujillo Bueno, J. 2012, ApJ, 761, L25
  45. Panasenco, O., Martin, S. F., & Velli, M. 2014, Sol. Phys., 289, 603
  46. Panesar, N. K., Innes, D. E., Tiwari, S. K., & Low, B. C. 2013, A&A, 549, A105
  47. Pereira, T. M. D., Leenaarts, J., De Pontieu, B., Carlsson, M., & Uitenbroek, H. 2013, ApJ, 778, 143
  48. Pevtsov, A. A., Canfield, R. C., & Metcalf, T. R. 1995, ApJ, 440, L109
  49. Pneuman, G. W. 1983, Sol. Phys., 88, 219
  50. Priest, E. R., Hood, A. W., & Anzer, U. 1989, ApJ, 344, 1010
  51. Rust, D. M., & Kumar, A. 1994, Sol. Phys., 155, 69
  52. Schmieder, B., Tian, H., Kucera, T., et al. 2014, A&A, 569, A85
  53. Shimizu, T., Nagata, S., Tsuneta, S., et al. 2008, Sol. Phys., 249, 221
  54. Soler, R., Oliver, R., & Ballester, J. L. 2009, ApJ, 699, 1553
  55. Su, Y., Gömöry, P., Veronig, A., et al. 2014, ApJ, 785, L2
  56. Suematsu, Y., Tsuneta, S., Ichimoto, K., et al. 2008, Sol. Phys., 249, 197
  57. Terradas, J., Arregui, I., Oliver, R., & Ballester, J. L. 2008, ApJ, 678, L153
  58. Tsuneta, S., Ichimoto, K., Katsukawa, Y., et al. 2008, Sol. Phys., 249, 167
  59. van Ballegooijen, A. A., & Martens, P. C. H. 1990, ApJ, 361, 283
  60. Vial, J.-C., & Engvold, O. 2015, Solar Prominences (Astrophysics and Space Science Library, Vol. 415; Dordrecht: Springer)
  61. Vial, J.-C., Pelouze, G., Heinzel, P., Kleint, L., & Anzer, U. 2016, Sol. Phys., 291, 67
  62. Vršnak, B., Maričić, D., Stanger, A. L., & Veronig, A. 2004, Sol. Phys., 225, 355
  63. Wedemeyer, S., Fleck, B., Battaglia, M., et al. 2016, arXiv:1601.00587
  64. Williams, D. R., Harra, L. K., Brooks, D. H., Imada, S., & Hansteen, V. H. 2009, PASJ, 61, 493
  65. Yurchyshyn, V. B. 2002, ApJ, 576, 493
  66. Zhang, Q. M., Chen, P. F., Xia, C., & Keppens, R. 2012, A&A, 542, A52
  67. Zirker, J. B., Engvold, O., & Martin, S. F. 1998, Nature, 396, 440
Comments 0
Request Comment
You are adding the first comment!
How to quickly get a good reply:
  • Give credit where it’s due by listing out the positive aspects of a paper before getting into which changes should be made.
  • Be specific in your critique, and provide supporting evidence with appropriate references to substantiate general statements.
  • Your comment should inspire ideas to flow and help the author improves the paper.

The better we are at sharing our knowledge with each other, the faster we move forward.
The feedback must be of minimum 40 characters and the title a minimum of 5 characters
Add comment
Loading ...
This is a comment super asjknd jkasnjk adsnkj
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters

You are asking your first question!
How to quickly get a good answer:
  • Keep your question short and to the point
  • Check for grammar or spelling errors.
  • Phrase it like a question
Test description