A&A 405, 769-777 (2003)
S. W. McIntosh1 - B. Fleck1 - P. G. Judge2
1 - European Space Agency, Research and Scientific Support Department, NASA Goddard Space Flight Center, Greenbelt, MD 20772, USA
2 - High Altitude Observatory, National Center for Atmospheric Research, PO Box 3000, Boulder, CO 80307, USA
Received 10 February 2003 / Accepted 15 April 2003
We present the results of an investigation into the interaction of the topographic structure of the solar chromospheric plasma with the wave modes manifesting themselves in the UV continua formed there. We show that there is a distinct correlation between the inferred plasma topography, the phase-differences between and suppression of oscillations in different levels of the solar atmosphere. We interpret these factors as evidence of interaction between the oscillations and the extended magnetic "canopy''. This work is based on the analysis of joint observations made by the Solar and Heliospheric Observatory (SOHO) spacecraft and the Transition Region and Coronal Explorer (TRACE).
Key words: Sun: chromosphere - Sun: oscillations - Sun: UV radiation
The question still exists as to the exact evolutionary path, from generation to extinction, of the ubiquitous oscillations observed in the quiet solar photosphere and chromosphere. The underlying goal of this quest is to assess whether or not there is a sufficient wave flux to supply energy, through some as yet unidentified mechanism, to the ambient chromospheric and coronal plasmas. Recent publications, in a concerted bid to answer this question, have resulted in the focus being placed on the understanding and analysis of multi-spacecraft, multi-wavelength, observations of chromospheric oscillations (see, e.g., Judge et al. 2001, hereafter JTW).
In this Paper we will take a closer look at one subset of those data, described in JTW, from the Solar and Heliospheric Observatory (Fleck et al. 1995, SOHO) Joint Observing Plan (JOP72). Specifically, we will study the time-series of the Ultraviolet (UV) continua (at 1550, 1600 and 1700 Å) acquired by the Transition Region and Coronal Explorer (Handy et al. 1999, TRACE) and the longitudinal magnetic field measured by the Michelson Doppler Imager (Scherrer et al. 1995, MDI) of SOHO on February 26, 1999 between 23:00 and 00:00 UT on February 27, 1999.
The work presented in McIntosh et al. (2001) and McIntosh & Judge (2001) utilised SOHO/SUMER (Wilhelm et al. 1995) time-series data to investigate the relationship between the extrapolated plasma topographies and the effect on the observed spectroscopic signatures. This work was limited to one spatial dimension, that of the SUMER slit. We demonstrate that there is a clear extension of this previous work to more than the one spatial dimension presented by the SUMER spectrometer. That is, we show that there is a direct correlation between reduced oscillatory power in the TRACE UV continua and the transition to a low plasma- (ratio of gas pressure to magnetic pressure) regime in the formation heights of the TRACE continua. Further, we suggest that the TRACE time-series data can be used as a diagnostic of the plasma topography and conditions in the mid-chromosphere through the signatures of the wave-modes present; a form of "chromo-seismology'', see Sect. 2.1.
|Figure 1: Coaligned context SOHO/MDI (left panel; B||) and TRACE (right panel; 1600 Å) images from JOP72 data-cubes of February 26, 1999. These images represent of the averages of one hour of time-series, 60 and 240 frames respectively.|
We analyse a
sub-region of the JOP72 TRACE data of February 26, 1999 (see discussion in JTW). The
observations were made of a near disc-center region of dimension
with 15 s between frames of the
same bandpass. We have employed the data reduction method outlined in
Sect. 2 of Krijger et al. (2001) to investigate the time-series
of the three UV TRACE bandpasses at 1550 Å, 1600 Å and 1700 Å.
This method allows us to form data-cubes for the TRACE and MDI
with each frame coaligned with
the previous one, until all are coaligned to that at t=0 with
sub-pixel accuracy (Tarbell 2002, Private Communication, employing the
TRACE Interactive Data Language routine "tr_get_disp_2d.pro'').
This image correlation process ensures that the data-cubes are as
"stable'' as possible to the effects of solar rotation. The need to
have each of these data-cubes aligned with one another required that
the initial TRACE and MDI frames must be carefully correlated to one
another. Figure 1 provides some
context for the observations through the temporal averages of the MDI line-of-sight magnetic field B|| and TRACE (the 1600 Å
bandpass) time-series and demonstrates that they are indeed well
|Figure 2: In panel A we show the spatial variation in the altitudes at which the plasma- is of order unity in the TRACE field of view, the TH. We have included solid contours for reference and each is separated by 0.25 Mm. panels B through D show one example of the integrated oscillatory power in the 3-8 mHz band of the 1700, 1600 and 1550 Å TRACE UV bandpasses respectively. On each panel we have overplotted the contours of panel A. Note the clear correlation between the reduced power and the contours.|
The critical component of the analysis presented by McIntosh et al. (2001) was the correlation between continuum signal formation height and the region of the atmosphere where the plasma- is of order unity. This correlation was represented by a considerable drop in the integrated oscillatory power in the 3-8 mHz frequency band when the SUMER signal was formed in the low regime. So, to draw comparison between the two-dimensional TRACE data and the one-dimensional SUMER data we must form an extrapolation of the underlying magnetic field. Since the coaligned MDI magnetograms show very little signature of emerging flux over the hour of the time-series, we can assume that the region under observation was very static. Therefore, in an effort to build a picture of the chromospheric plasma topography we employ the simplest approach to extrapolate the magnetic field, a potential extrapolation, of the time-averaged MDI B||. Once the three dimensional field B(x,y,z) is extrapolated from B||(x,y,0) we compute the magnetic pressure and the plasma- ( ; where is the model gas pressure). We make use of the Vernazza et al. (1981, VAL3C) model values of interpolated onto the same vertical scale as that of the magnetic field extrapolation.
To search for locations where the oscillatory power drops in the TRACE
bandpasses they are further decomposed, using a Fast Fourier Transform
at each spatial pixel, so that we have
|Figure 3: The two-dimensional histograms of TRACE oscillatory power and TH derived from panels B through D of Fig. 1. The colour scale in each panel indicates the number of image pixels with that particular combination of oscillatory power and TH. We see that, in each panel, there are two distinct correlations present, the "tail'' to the lower-left indicating the correlation of low oscillatory power and low TH and the broad power correlation of the "canopy'' at a TH of around 1.75 Mm.|
Now, it is straightforward to estimate the height at which the plasma- is of order unity, five say, in the two-dimensional TRACE field-of-view (FOV). This height we call, for the sake of brevity, the transition height, or TH. In panel A of Fig. 2 we show the colour-coded spatial variation of the TH. As a visual aid we have added contours with a spacing of 0.25 Mm. The presence of the network elements, where TH is blue-violet in colour, is perhaps the most striking feature. We can also get a feeling, albeit a very rough one given that this is from a potential field extrapolation, about the topographical form of the chromospheric "canopy'' field and its connectivity. In the inter-network regions of panel A it is clear that the TH is far higher than that in the network regions. In the other panels of Fig. 2, B through D, we have included the maps of 3-8 mHz power for the three TRACE UV bandpasses with the same TH contours overplotted. Obviously, there is a striking correspondence between the TH contours and the dearth of oscillatory power and that is far extended from the network elements, cf. panel B of Fig. 1 (Krijger et al. 2001 reported the drop of the 3-8 mHz power and called this a "network shadow''; quite different from the "shadow'' defined by McIntosh & Judge 2001). The clear extension of the drop beyond the the network element makes it all the more likely that the drop in signal is more than just an issue related to regions where there is a large intensity contrast in that particular continuum bandpass.
These TRACE continua are formed at heights of 400-700 km above (JTW), we see that the TH contours corresponding to significantly reduced oscillatory power in the TRACE continua are at 1.0 Mm or less. In an effort to quantify this correspondence we show, in Fig. 3, the two-dimensional correlation histogram of oscillatory power and TH for each of the three TRACE bandpasses. There are two correlations that are clearly present in each of the histograms:
|Figure 4: In panel A we show the spatial variation in the altitudes at which the plasma- is of order unity in the SOHO/MDI field of view, the TH. We have included solid contours for reference and each is separated by 0.25 Mm. panels B through D show one example of the integrated oscillatory power in the 3-8 mHz band of the B||, V|| and continuum intensity (I) MDI filtergrams respectively. These filtergrams are formed significantly lower in the atmosphere than those of Fig. 2 (0.2 Mm). On each panel we have overplotted the contours of panel A. Careful inspection of panel D shows that the only significant drops in oscillatory power occur in the very darkest, deepest, regions of the TH.|
There is an extension of the TRACE continua analysis that can help us to differentiate between the correlation between "canopy'' interactions with oscillations (i.e., TH and oscillatory power suppression) and the suppression of oscillations in regions of magnetic plage (see, e.g., Title et al. 1992). In Fig. 4, we have duplicated the TRACE UV continuum analysis for the concurrent MDI filtergram time-series in B||, the line-of-sight Doppler velocity V|| and continuum intensity I; all of which are formed significantly lower (0.2 Mm) than the TRACE UV continua. The rationale being that, at these lower formation heights, we should see very little, or no, oscillatory power suppression in V|| and Iexcept in regions where the TH gets low enough, i.e. in concentrated, strong, regions of network or plage magnetic fields, not the extended regions shown in Fig. 2. Panels B through D of Fig. 4 show, again, the integrated power in the 3-8 mHz range for the three MDI filtergram time-series. Other than the dark regions of low power in panel B (such deficits of B||Fourier power have been discussed previously in the literature, see, e.g., Jain & Haber 2002), a cursory look at panels C and D shows the reader little, or no, correlation to the overplotted TH contours. However, careful examination of panel D shows that the lowest oscillatory powers are located in the very core of the network elements; the darkest regions in panel A. The localisation of these oscillatory power minima in the network element cores is consistent with the results found in the TRACE UV continua analysis. This adds further weight to the assertion that the observed oscillatory power suppression is related to the topographic structure of the plasma as interpreted through the TH.
Using the evidence presented in Figs. 2, 3 and 4 we deduce that the reduction in the oscillatory power of the TRACE continua, MDI I continuum and their close correlation to the structure of the TH is the two-dimensional analogue of the effect reported by McIntosh et al. (2001).
An obvious extension of the work discussed in this paper is to study
the spatial variation of the phase-difference between the three TRACE
bandpasses at as high a spatial resolution as possible. The
investigation of phase-differences in TRACE, SUMER and ground based
observations of chromospheric oscillations has been performed before
(see, e.g., Deubner & Fleck 1990; Krijger et al. 2001; Lites et al. 1982, JTW and many more references
therein). These previous analyses spatially summed phase-spectra and sought only
to differentiate between network and inter-network regions (ensuring a
large signal-to-noise level), not to investigate the full range of
spatial features. Here, we compute the TRACE bandpass
phase-differences (as outlined in Sect. 3 of
Krijger et al. 2001) directly
from the full spatial resolution complex frequency cube of
Eq. (1). To compute the phase-difference spectrum we
must first compute the cross-power spectrum
for any two of the three bandpasses i and j, say. This is simply
To investigate the spatial variation of , we form a scatter plot of versus for each pixel in the spatial pixel region. Additionally, each of these points has a weight (given by its corresponding cross-spectrum power values) and we use these weights to perform a linear least-squares fit to the scatter plot between 3 and 8 mHz. A sample fit of from the scatter plot is illustrated in Fig. 5 for a typical internetwork aggregate pixel. The dots indicate the scatter in the , space (notice the tight behaviour and growth from about 3-10 mHz and the break to almost random phase-differences beyond 15 mHz) and the size indicates the magnitude of the cross-power (largest have the highest cross-powers), or the weights of the fit. This example fit has a of . A more in-depth discussion of this procedure, and the associated fitting error, can be found in McIntosh et al. (2003).
|Figure 5: Sample linear fit of the phase-difference gradient, , between 3 and 8 mHz at position coordinates [-170, 35] and a region around that point for the 1700-1600 Å bandpass pair. The dots mark the positions, in ( , ) space, of every point in the spatially degraded cube (we also show the variation of mean and mean plus/minus 1- of at each -indicated by the dash-dot and solid lines respectively). Of these points, about 10% lie between 3 and 8 mHz with a net cross-power greater than, or equal to, ten. This latter set are indicated by triangles and their size indicates the net cross-power, the quantity used to weight the linear fit. The solid line indicates the fit to the triangles and has a gradient of .|
Performing this analysis for each aggregate pixel of the three bandpass combinations we can construct the panels of Fig. 6. Again, for reference, in panel A, we show the TH map and its contours. In panels B through D we show the spatial dependence of for each of the bandpass pairs; 1700-1600 Å, 1700-1550 Å, and 1600-1550 Å respectively. We see that there is a variation of from about 0 in the network regions to about 10 in the farthest reaches of the internetwork. As noted above, for this degree of spatial binning, there is an associated mean error in of 1 . We note that, at full TRACE spatial resolution, the error is 10 and it is straightforward to see that any spatial pattern is lost in the noise attributed to the poorly constrained fit (as mentioned above). As a test of our methodology we have performed a "closure test'' (cf. Sect. 5 of Krijger et al. 2001) involving the comparison of the 1700-1550 map to the sum of the other two; the resulting difference should be zero. For our level of approximation, using as a measure of the phase-difference variation, we are close to zero (mean difference of ).
As in Sect. 2, we notice that there is a striking correspondence between regions of low and the lower TH contours, predominantly in the network regions. In the internetwork regions, far away from the network elements, we see the largest values of . In Fig. 7, as in Fig. 3, we show the correlation histograms of for each of the bandpass pairs and TH. Again, the two correlations discussed above are evident in each panel. We note this correspondence here and leave a brief discussion for the following section.
|Figure 6: As in Fig. 2, in panel A, we show the model-derived altitudes at which the plasma- is of order unity in the TRACE field of view. In panels B through D we show the fitted phase-difference gradient ( ) maps as discussed in the text. Again, we note more than a passing correspondence between the overplotted contours and the darker regions of the maps.|
|Figure 7: The two-dimensional histograms of phase-difference gradient ( ) and TH derived from panels B through D of Fig. 6. The colour scale in each panel indicates the number of image pixels with that particular combination of and TH. As for Fig. 3, we see that, in each panel, there are two distinct correlations present. The "tail'' to the lower-left indicating the correlation of low and low TH and the broader correlation of the "canopy'' at a TH of around 1.75 Mm. In this case, the "resolution'' of the histograms are degraded compared to those of Fig. 3 but this is due to the spatial degradation necessary to compute from the full resolution TRACE image.|
We have shown that there is a distinct correlation between the inferred solar plasma topography, the phase-differences between and suppression of oscillations in different levels of the outer solar atmosphere. The suppression of the TRACE signal, near network elements, is reported by Krijger et al. (2001) but the extension of the suppression far beyond the network region and its connection to the TH was not made. The fact that this extension of the suppressed power is not observed in the lower photosphere (the MDI time-series) we interpret as evidence of interaction between oscillations and the TH "canopy'', i.e., the two-dimensional analogue of the 3-min oscillation suppression reported by McIntosh et al. (2001).
We acknowledge that there are drawbacks associated with the use of a potential field extrapolation and the incorporation of the VAL3C atmospheric model in building the plasma topography (e.g., concentrated flux regions). For example, the slight discrepancy between the TRACE formation heights and those attributed from the TH can most likely be attributed to the application of the VAL3C to regions of the atmosphere where it would typically be invalid. In any further analysis the use of a lookup table to associate model atmosphere type and, say, magnetic field strength may provide more accurate predictions of the TH interface.
In a future paper (McIntosh et al. 2003) we investigate, in depth, the spatial patterns of presented in the panels of Fig. 6. To this end we consider the two significant components that we have mentioned in Sect. 2.1, discussed at greater length in Deubner & Fleck (1990); Lites et al. (1982), that can produce these patterns in imaging observations:
The work presented in this paper (and in Bogdan et al. 2002,2003; McIntosh et al. 2001; Rosenthal et al. 2002; McIntosh & Judge 2001) demonstrates that understanding the position and role of the TH may provide a critical link into the understanding of wave mode conversion, dissipation and ultimately the heating mechanism of the chromosphere, maybe even the ambient solar corona itself. However, for the time being, the investigation of these effects will be limited to the complex, though not impossible (cf. JTW), combination of spectroscopic slit (SUMER) and passband imaging (TRACE) observations which lack Doppler velocity information. Indeed, that will be the case until we are able to perform some form of imaging spectroscopy. Such a platform will allow the study of multiple line profiles simultaneously, spanning the vertical domain of the solar atmosphere in a less discrete fashion. This advance will accurately allow the diagnosis and mapping of the important region where the plasma- is of order unity.
SWM acknowledges the support of a External Fellowship from the European Space Agency at GSFC and the European Solar Magnetometry Network (ESMN) under contract ERBFMRXCT980190. The authors wish to thank Guiseppe Severino, Mark Rast and Karel Schrijver for their careful reading of the manuscript and the comments that have greatly improved its content and clarity. SWM also wishes to acknowledge the support and assistance of Tom Bogdan, Mats Carlsson and Viggo Hansteen in the work that has lead up to this publication.