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Dynamic fibrils in H-alpha and C IV

Aim: To study the interaction of the solar chromosphere with the transition region, in particular active-region jets in the transition region and their relation to chromospheric fibrils. Methods: We carefully align image sequences taken simultaneously in C IV with the Transition Region and Coronal Explorer and in H-alpha with the Swedish 1-m Solar Telescope. We examine the temporal evolution of"dynamic fibrils", i.e., individual short-lived active-region chromospheric jet-like features in H-alpha. Results: All dynamic fibrils appear as absorption features in H-alpha that progress from the blue to the red wing through the line, and often show recurrent behavior. Some of them, but not all, appear also as bright features in C IV which develop at or just beyond the apex of the H-alpha darkening. They tend to best resemble the H-alpha fibril at +700 mA half a minute earlier. Conclusions: Dynamic chromospheric fibrils observed in H-alpha regularly correspond to transition-region jets observed in the ultraviolet. This correspondence suggests that some plasma associated with dynamic fibrils is heated to transition-region temperatures.


Introduction
In this paper, we study active-region fibrils in the solar chromosphere and transition region. The context is the dynamical structure of the transition region as the interface between the chromosphere and the corona. It is highly complex due to the fine structure of the chromosphere, which is dominated on small scales by jet-like features observed in Hα as spicules at the limb, and as active-region fibrils and quiet-sun mottles on the disk. They bring cold (∼10 4 K), dense plasma up to greater heights than expected from hydrostatic equilibrium (e.g., Suematsu et al. 1995). The understanding of the formation and behavior of these structures is limited, although they appear to be key agents in the momentum and energy balances of the outer solar atmosphere . Even the relationships between these different features remain in debate (see the still valid observational reviews by Beckers (1968Beckers ( , 1972, the theoretical review by Sterling (2000), and the more recent analyses by Tziotziou et al. (2003Tziotziou et al. ( , 2004 and references therein). Solar images taken in EUV lines also show jet-like structures in the chromosphere and transition region. Some EUV jets extend much further out from the limb than Hα spicules, and have much longer lifetimes. However, it has been established that many EUV and Hα features tend to have similar lengths and dynamics (e.g., Withbroe 1983;Dere et al. 1983Dere et al. , 1986Dere et al. , 1987Budnik et al. 1998;Wilhelm 2000;Xia et al. 2005). The similarities between a class of EUV and Hα features suggests that they are different manifestations of the same phenomenon, possibly with EUV jets being hot sheaths around cool Hα interiors. However, a direct one-to-one correspondence has not yet been established.
In the present analysis, we concentrate on short-lived activeregion fibrils observed in Hα. These have lifetimes of only a few minutes. We call them "dynamic fibrils". Longer and more static fibrils are not the subject of this study. De Pontieu et al. (2003) reported spatial coincidence of emission features in C  lines and dynamic Hα fibrils observed in the red wing at ∆λ = 700 mÅ from line center. The dynamic fibrils in Hα correspond well with dark inclusions observed in the Fe / EUV passband around 171 Å of the Transition Region and Coronal Explorer (TRACE, Handy et al. 1999) in so-called mossy plage, where "moss" describes the finely textured and dynamical appearance of such plage in 171-Å image sequences De Pontieu et al. 1999. Here, we expand on De Pontieu et al. (2003) by examining the temporal evolution of the dynamic Hαfibrils and their C  counterparts. The data are described in Sect. 2, the analysis in Sect. 3, and the results are discussed in Sect. 4 and summarized in Sect. 5.

Observations and data reduction
We analyze image sequences of NOAA active region 10380 recorded simultaneously in Hα and in C on June 16 2003 between 8:02 and 9:07 UT at a viewing angle of 48 degrees (µ = 0.66). AR10830 was a sizable active region that decayed rapidly during its transition over the disk, appearing as a large complex of sunspots and disappearing as mostly plage. It still contained several small sunspots at the time of observation. The Swedish 1-m Solar Telescope (SST, Scharmer et al. 2003) was used to take images at four wavelengths in Hα, while co-pointed imaging was performed by TRACE in its three ultraviolet (UV) passbands at 1550, 1600, and 1700 Å. The SST field of view is indicated by the solid contour. It contains active region AR10380 with a few small sunspots. The dashed contour specifies the cutout used in Fig. 2.
At the SST, the SOUP tunable Lyot filter (Solar Optical Universal Polarimeter, Title et al. 1986) was used for narrowband imaging at ∆λ = −700, −350, +350, and +700 mÅ from the Hα line center with 130-mÅ FWHM bandwidth. These passbands sample the chromosphere, though there is a contribution from the photosphere at least in the ±700-mÅ passbands due to the double-peaked contribution function of the Hα line wing (Leenaarts et al. 2006). The images consist of 1534×1032 square pixels of 0.0655 ′′ size. Bursts of images were recorded at each sampling wavelength during seven seconds before tuning the SOUP filter to the next wavelength. The frame rate was 1.6 fps at ±700 mÅ with 115-ms exposure, and 1.2 fps at ±350 mÅ with 200-ms exposure. Thanks to the use of the SST's adaptive-optics system, the data quality does not suffer too much from these long exposure times. The three images of each burst with the highest contrast were stored to disk.
In the post-processing all stored images were first corrected for wavelength-dependent dark current and flat field. In order to reduce seeing effects caused by the Earth's atmosphere, each set of three images was subsequently processed with the multi-frame blind deconvolution technique developed by Löfdahl (2002) using the implementation of Van Noort 1 (cf. van Noort et al. 2005). The resulting images reach better than 0.25 ′′ resolution. The four Hα sequences have a cadence of 55 ± 5 s, with an average time delay of 12 ± 2 s between successive wavelength positions, and 18 ± 5 s from the last red back to the first blue position. They were rotated to the same orientation as the TRACE images with solar north up. Image displacements were then measured in multiple steps described below. These displacements were subsequently used to re-sample the de-rotated images onto an aligned grid in a single step in order to avoid repeated spatial interpolation. We began by computing the displacements between successive images per wavelength. Next, we corrected the −700-mÅ sequence for residual linear drift by aligning the first and last images, and adjusting the com-1 http://www.solarphysics.kva.se/mfbd puted displacements between these two. The first and last images of the other passbands were then aligned to the −700-mÅ ones using the wavelet technique of De . Finally, we used the computed offsets to shift the de-rotated images using cubic-spline interpolation to create four accurately aligned sequences of 78 images each.
Visual inspection of the sequences shows rapid changes in the mean full-field intensity. We suspect that the SOUP filter was not always precisely tuned to the wavelength specified. Since we study the morphology of structures here, this amplitude variation and the small tuning error do not affect our results.
The TRACE UV bandpasses labeled 1550, 1600, and 1700 Å together sample the low and upper chromosphere as well as the transition region. In these observations TRACE was programmed to record images sequentially in these three wavelengths at a cadence of 20 ± 1 s. The angular resolution is 0.5 ′′ per pixel, the image size 640 × 512 square pixels. The images were corrected for dark current and were flat-fielded with the SolarSoft procedure trace prep described in the TRACE Analysis Guide 2 . The images were subsequently aligned with high precision using Fourier cross-correlation in three steps. In the first step, the 1600-Å images were aligned in consecutive pairs, and each 1550 and 1700-Å image was subsequently aligned with the 1600-Å image that is closest in time. The second step involves alignment of each of the resulting images with respect to a running average over nine images. The latter were selected from the output of the first step for 1550, 1600, and 1700 Å combined such as to be closest in time, and smoothed with a 5 × 5-pixel spatial averaging. This procedure avoids copying alignment errors from one sequence to another, as would occur when aligning to a single "master" image sequence (De Wijn et al. 2005). Finally, each original image was re-sampled to the aligned grid. The single interpolation step ensures minimal degradation of the image quality.
The 1550 and 1600-Å passbands include the C  lines at 1548 and 1550 Å that are formed at temperatures around 60-250×10 3 K and sample the transition region. There are also considerable contributions from the surrounding continuum because of the broad passbands (20 and 275 Å, respectively). The 1700-Å passband has a width of 200 Å, but does not include the C  lines. In this analysis, which focuses on the C  contribution, we employ the technique of Handy et al. (1998) to construct an image sequence in the C  lines through linear combination of the three bandpasses. Because TRACE takes images sequentially, we used temporal interpolation of the 1600 and 1700-Å images to match the 1550-Å images. We prefer to use interpolation over the more usual nearest-neighbor selection, because the averaging inherent to interpolation reduces the noise. Comparison between the two techniques shows only small differences.
The final step of the reduction is cross-alignment of the sequences of Hα and C  images. This was done using several small bright points visible in Hα −700 mÅ as well as the UV continua. The resulting C  image sequence was scaled and cut out to match the Hα images. Since the cadence of the C  sequence is much faster than that of the Hα sequences, and since the four Hα sequences are staggered in time, we produced four C  sequences for each of the Hα sequences by nearest-neighbor sampling. Visual inspection shows good alignment (< 0.5 ′′ ) between the C  and Hα sequences.   Figure 1 shows a cutout of an example 1600-Å image to illustrate the common field of view between TRACE and the SST. The solid rectangle outlines the SST field of view, the dashed rectangle outlines the cutout in Fig. 2. The latter contains activeregion plage which appears as mossy plage in a TRACE 171-Å sequence taken an hour earlier. It harbors many small, dark Hα features that are best visible in the ±700-mÅ panels. They are also present at the inner-core wavelengths but with more confusion rising from feature crowding. Closer to the limb, such confusion would be much worse due to projection effects and also affect the outer wing panels, but at µ = 0.66 single features are well identifiable in these data. Most of these features display very dynamic behavior in the Hα sequences. We call these "dynamic fibrils" because they come and go on timescales of a few minutes only; they are the subject of this study. Fibrils that are more stable in appearance and tend to be longer are not the subject of this paper.

C  emission from dynamic fibrils
We searched for spatio-temporal coincidence of enhanced C  emission and the occurrence of dynamic Hα fibrils by detailed inspection of the image sequences. Often, C  brightness enhancements do not have obvious counterparts in Hα, but some of them clearly correspond closely to dark dynamical features in the red wing of Hα, not only by appearing at the same location and close in time, but also by having morphological similarity. This has earlier been noticed by De Pontieu et al. (2003). It is present in all Hα images, but best visible in the blue wing at first, and later in the red wing. The C  panels show diminishing brightness at its location.
We identified 16 cases in which the correspondence between a dynamic fibril in Hα and C  emission is particularly evident. Their locations are marked by the white diamonds in the leftmost panel of Fig. 2. Five examples are shown in Fig. 3. The morphological correspondence is obviously imperfect, which in part can be attributed to noise in the UV images (the TRACE CCD has lost considerable sensitivity since its launch), to the relatively poor angular resolution of the C  construct, to residual seeing in Hα, and to intrinsic difference in shape. However, the number of paired features, their morphological similarities, and the fact that they tend to track each other in their temporal evolution give confidence that their identification as pairs is correct. The intrinsic shape differences are discussed below.
In Figs. 4-6, we present the samples of the first three columns of Fig. 3 in detail. Figure 4 shows the temporal evolution of the leftmost case in Fig. 3. The fibril appears as a dark structure especially in Hα −700 and −350 mÅ (second and third panel in the top row). It consists of a slender feature extending from (663 ′′ , −236 ′′ ) to (668 ′′ , −234 ′′ ), and a smaller squarish feature around (662 ′′ , −237 ′′ ). There is already a brightening in the C  construct (top row, first panel) appearing just to the right of the square feature around (664 ′′ , −237 ′′ ). In the middle row of Fig. 4, the elongated feature has largely disappeared in the blue wing, but has become more clearly visible in the red one. The square feature is still visible in the blue wing and does not have an appreciable signature in the +700-mÅ passband. The lower part of the C  brightening shrinks slightly, but the upper part coincident with the left side of the elongated Hα feature remains bright, while the other end around (669 ′′ , −234 ′′ ) brightens. The bottom row shows the scene about one minute later. The elongated Hα feature has mostly disappeared, the square feature is now evident throughout Hα, and the left C  brightening has shrunk further. Figure 5 similarly details the example in the second column of Fig. 3. In this case, a small fibril appears in Hα −700 and −350 mÅ around (672 ′′ , −207 ′′ ) (second and third panel, top row). A brightening in C  develops quickly at the same location. The fibril is visible in all Hα passbands in the middle row. A minute later (bottom row) it is still clearly visible in the far red wing (fifth panel), and appears somewhat more clearly in Hα −700 mÅ (second panel), indicative of recurrent behavior. It remains clearly visible in the C  image. Despite its small size in Hα, there is considerable brightening in C . Figure 6 shows the example in the third column of Fig. 3. The Hα ±350 mÅ panels (third and fourth column) suffer much from feature crowding that makes precise identification of features difficult. However, the similarity between, e.g., the absorption in the Hα +700 mÅ in the top row and the C  emission in the mid-  Fig. 3, in the same format as Fig. 4. The central brightening in the C  panels corresponds to darkening in Hα that progresses from the blue wing (top row, second and third panel) to the red wing (middle and bottom row, fourth and fifth panel). In the middle row, the dark structure around (676 ′′ , −212 ′′ ) expands in the blue wing of Hα, and migrates toward the red wing while brightening markedly in C  (bottom row). Some other structures visible in Hα are not identifiable in C , such as the dark feature around (678 ′′ , −210 ′′ ) in the middle Hα +700 mÅ image. dle row is striking. A small feature around (690 ′′ , −220 ′′ ) is first clearly visible in the far blue wing (top row, second panel), and later at the same location with similar morphology in the far red wing (bottom row, fifth panel). It appears at the same location as the absorption in Hα +700 mÅ in the top row (fifth panel), pointing to recurrent behavior. It also shows associated C  emission in the middle row. Another fibril around (693 ′′ , −215 ′′ ) develops C  brightening more slowly and less obviously. In this case, the C  emission is offset by about 1 ′′ from the rightmost edge of the absorption in Hα +700 mÅ.
The remaining thirteen cases not detailed here all exhibit similar evolution: a dark absorption feature first appears in the blue wing of Hα and then migrates to the red wing, while corresponding brightening appears in C . We emphasize, however, that there are many more fibrils in the SST field of view that show such smooth progression through Hα without obvious corresponding C  emission.

Correlations
We computed Pearson correlation coefficients (e.g., Press et al. 1992) for the 16 selected locations between Hα and C  intensity as a function of time delay. They describe the amount of linear correlation between the two intensities, i.e., a correlation coefficient C = 0 indicates a complete lack of linear correlation, while C = 1 and −1 reflect perfect linear correlation and anticorrelation, respectively. In each case, the fibril area was determined by first selecting those pixels in C  that are more than two standard deviations above the average value around the fibril, and dilating the result with a 30 × 30-pixel kernel. These regions are indicated by white outlines in the five examples in Fig. 3. For each Hα wavelength, we next correlated the C  frame in which the feature is best visible to the five Hα frames straddling it in time. As to the correlation coefficients C of bright C  versus dark Hα +700 mÅ derived for the 16 cases, we find that their extremes reach a minimum of −0.7 and a maximum of −0.2, while their average is −0.5. The delay between C  and the best match in Hα +700 mÅ varies between 13 and −109 s with an average value of −33 ± 30 s, where a negative delay indicates that Hα +700 mÅ precedes C . Despite the large error, the negative delay appears significant because it is found in all but two cases. Figure 7 shows the correlations against time for the first three examples of Fig. 3. For all fibrils the anticorrelation is most obvious for the +700-mÅ passband, and varies for the other passbands. The fibrils show a similar time delay of about one minute for the +700-mÅ passband, in the sense that C  brightens later than the red wing darkens. Especially the fibril in the center panel shows temporal progression from blue to red across the line. It also shows recurrent behavior: the correlation drops again at large time difference, at first in the blue wing, and later in the Fig. 6. Temporal evolution of the fibril in the third column of Fig. 3, in the same format as Fig. 4. The bright structure in the C  panels corresponds to darkening in Hα best visible in the ±350 mÅ passbands (third and fourth column). In the top row, only a small feature is present in the far blue wing around (690 ′′ , −220 ′′ ) (second panel). There is already considerable absorption in the far red wing (fifth panel). The C  brightening develops quickly and is most prominent in the middle row. It is morphologically most similar to the absorption in Hα +700 mÅ a minute earlier (top row, fifth panel). In the bottom row it has largely disappeared. The fibril around (690 ′′ , −220 ′′ ) in the Hα −700 mÅ panel has now progressed into the red wing of Hα. Another fibril is present around (693 ′′ , −215 ′′ ). Its associated C  brightening is less clearly seen and offset by about 1 ′′ from the rightmost edge of the absorption in Hα+700 mÅ.
red. The fibril in the rightmost panel displays similar behavior. Figure 8 displays histograms of the delays of best anticorrelation between Hα and C  intensity for each Hα wavelength. It shows a clear peak at negative values for the best anticorrelations between Hα +700 mÅ and C  brightness, indicating that the halfminute negative delay is significant despite a large error, and less so between +350 mÅ and C  brightness. The histograms of delays for the best anticorrelation between Hα blue wing and C  brightness appear featureless. Large positive delays can be interpreted as signs of recurrent behavior.

Discussion
The observations presented here add temporal evolution to the study by De Pontieu et al. (2003). In a one-hour multiwavelength sequence, we have identified 16 dynamic Hα fibrils with associated C  emission. In all cases, the corresponding dark Hα feature progresses in a smooth, continuous fashion from the blue wing to the red one in a few minutes, and only then shows the best correlation with the C  brightness feature. It often also displays recurrent behavior. Many Hα fibrils appear to have some corresponding C  emission, though it is conspicuous in only a few cases.
Another aspect of interest is the width of the Hα line in dynamic fibrils. Inspection of the Hα sequence shows that most, if not all, short-lived Hα fibrils show such progression from the blue to the red wing, but most are not obviously associated with C  brightening. A case in point is the dark feature around (678 ′′ , −210 ′′ ) in Fig. 5. It is present in the ±350 mÅ panels in the top row, and shows progression to the red wing (second row, +350 and +700 mÅ panels) without clear C  brightening.
We interpret the progression as to result from matter first moving up in the direction of the observer, and then back toward the surface. This interpretation agrees well with the description of active-region moss as jets moving upward in the atmosphere and periodically obscuring the hot footpoints of loops De Pontieu et al. 1999;Martens et al. 2000). We do not have concurrent observations in TRACE 171 Å or 195 Å, so we cannot establish that our dynamic Hα fibrils correspond to such obscuration in mossy plage. However, since the relationship between moss and chromospheric jets is wellestablished (e.g., De Pontieu et al. 2003), it is likely that the dy- Fig. 7. Three samples of the correlation between Hα and C  intensity as a function of time delay, corresponding to the first three cases in Fig. 3, respectively. Curve coding: correlation between C  and Hα −700 mÅ (dashed-dotted, circles), Hα −350 mÅ (dashed, triangles), Hα +350 mÅ (dotted, squares), and Hα +700 mÅ (solid, diamonds). namic fibrils described here correspond to the jets that cause moss.
The observation that the C  emission occurs only after the fibril has progressed to the red wing of Hα, i.e., when the matter returns toward the solar surface, implies that the C  emission line itself should be shifted to the red as well. Spectroscopic observations indeed show that this is the case (Dere et al. 1986).
The curves in Fig. 7 show that darkness in Hα +700 mÅ correlates well with C  brightness occurring half a minute later. The disappearance of the Hα absorption at that time may be due to the narrow width of the SOUP passband (130 mÅ), which registers only a narrow range of velocities. If the fibril still accelerates downward while being heated, it may reach the temperature needed for C  emission while shifting out of the SOUP passband.
As already noted, not all dynamic Hα fibrils show corresponding C  emission. Some may be missed when they evolve faster than our temporal sampling, which is limited by the ∼1 minute cadence of the Hα sequences. Some others may be missed due to lack of instrument sensitivity.
What precisely is the origin of this C  emission that apparently corresponds to cool Hα structures? The emission may originate from a hot sheath around a cool fibril acting as inter-face to the surrounding corona, as proposed by Withbroe (1983). Such a sheath could be formed through cross-field thermal conduction (Athay 1990), and would be expected to produce C  emission that is cospatial with the Hα absorption. Estimated radiative losses show that only a very thin layer of hot material is required to explain the observed intensity in our TRACE images, so that cross-field conduction cannot be ruled out on grounds of effectiveness or timescale. However, we get the impression from our observations that many of the brightness enhancements in C  are systematically shifted toward the upper end point of the corresponding Hα fibril. This is the case for all 16 fibrils studied here; in some the C  brightening extends as far out as 1 ′′ beyond the apex of the feature in Hα +700 mÅ. Co-spatial correlations have been computed in Sect. 3.2. The temporal delay shown by the curves in Fig. 7 is not invalidated by the observation that the Hα and C  features are not co-spatial. It even serves as confirmation: the offset C  emission is more strongly correlated with the Hα fibril in its appearance of, say, half a minute ago, when it had a larger extent. Dere et al. (1986) also noted that in quiet-sun observations the most intense C  emission is produced just beyond Hα mottles. This finding suggests that there is a large temperature gradient along the structure, with a cold footpoint in the chromosphere and a hot top in the corona. The energy required to heat the tip of the fibril may then be provided by the corona, possibly through parallel heat conduction, or by hot coronal material filling the wake of the descending fibril. Dere et al. (1987) derived extremely small filling factors from HRTS spectra, and concluded that UV fibrils are sparsely filled with numerous hot microscopic structures. Our observations cannot confirm or disprove this, other than that these microscopic structures should develop toward the end of the fibril's life, during or after the descent of the fibril back to the lower atmosphere, in order to reproduce the observed time delay between the appearance in the far red wing and the C  emission.
It is unclear what mechanism may cause heating in such a highly inhomogeneous spatial pattern, or why it would preferentially cause heating during the downward contraction of the fibril.
Another possibility is that a density enhancement occurs when the jet descends, causing brightness enhancements in optically thin conditions, as is the case for the C  lines used here. Lastly, coronal and transition-region EUV radiation may ionize a sheath, causing C  emission through recombination.
Classically, spicular line widths and profiles of Hα and Ca  H&K pose inconsistencies between thermal and nonthermal broadening (e.g., Beckers 1968). Our 16 specimens show that Hα darkening often occurs simultaneously in all four Hα passbands, with the most pronounced darkening progressing from the blue to the red wing. This is also shown by the correlation curves in Fig. 7. It requires large line broadening which may be caused by unresolved structure, non-thermal motions including turbulence, or a high temperature. The latter would be consistent with associated C  emission, though contradicting the common belief of ∼10 4 K temperature with large non-thermal broadening. It is of interest to map chromospheric line widths at high resolution in this context.

Conclusions
We have identified 16 dynamic Hα fibrils in high-resolution image sequences which show corresponding C  emission in the UV. Without exception, these fibrils show a progression of the absorption feature through Hα from the blue to the red wing, often with recurrent behavior. Many, if not all, dynamic fibrils that do not display identifiable C  emission also show this progression. We interpret it as matter flowing first up and then down in the solar atmosphere.
We conclude that some plasma associated with dynamic fibrils is heated to transition-region temperatures. The C  emission appears at the apex of the Hα fibril, sometimes extending beyond it. It best resembles the far red Hα wing of about half a minute earlier. We attribute this apparent delay to the offset of the C  emission beyond the tip of the Hα fibril.
Whichever heating mechanism operates, our observed correlation between Hα and C  fibrils clearly provides constraints on theoretical models. Detailed comparisons with advanced 2D or 3D numerical simulations of the low solar atmosphere will be necessary to determine which effect dominates the heating of fibril plasma to 10 5 K.