Global Energetics of Solar Flares. II.

Global Energetics of Solar Flares: II. Thermal Energies

Markus J. Aschwanden and Paul Boerner Lockheed Martin, Solar and Astrophysics Laboratory, Org. A021S, Bldg. 252, 3251 Hanover St., Palo Alto, CA 94304, USA; e-mail: aschwanden@lmsal.com Daniel Ryan Royal Observatory of Belgium, Solar-Terrestrial Centre for Excellence, Avenue Circulaire 3, 1180 Uccle, Brussels, Belgium; e-mail: ryand5@tcd.ie Amir Caspi Planetary Science Directorate, Southwest Research Institute, Boulder, CO 80302, USA; e-mail: amir.caspi@swri.org James M. McTiernan Space Sciences Laboratory, University of California, Berkeley, CA 94720, USA; e-mail: jimm@ssl.berkeley.edu Harry P. Warren Space Science Division, Naval Research Laboratory, Washington, DC 20375, USA; e-mail: harry.warren@nrl.navy.mil
Abstract

We present the second part of a project on the global energetics of solar flares and coronal mass ejections (CMEs) that includes about 400 M- and X-class flares observed with the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO) during the first 3.5 years of its mission. In this Paper II we compute the differential emission measure (DEM) distribution functions and associated multi-thermal energies, using a spatially-synthesized Gaussian DEM forward-fitting method. The multi-thermal DEM function yields a significantly higher (by an average factor of ), but more comprehensive (multi-)thermal energy than an isothermal energy estimate from the same AIA data. We find a statistical energy ratio of between the multi-thermal energy and the magnetically dissipated energy , which is an order of magnitude higher than the estimates of Emslie et al. 2012. For the analyzed set of M and X-class flares we find the following physical parameter ranges: cm for the length scale of the flare areas, K for the DEM peak temperature, K for the emission measure-weighted temperature, cm for the average electron density, cm for the DEM peak emission measure, and erg for the multi-thermal energies. The deduced multi-thermal energies are consistent with the RTV scaling law , which predicts extremal values of erg for the largest flare and erg for the smallest coronal nanoflare. The size distributions of the spatial parameters exhibit powerlaw tails that are consistent with the predictions of the fractal-diffusive self-organized criticality model combined with the RTV scaling law.

Sun: Flares — plasmas — radiation mechanisms: thermal — Sun: UV radiation

1 Introduction

While we measured the magnetic energy that is dissipated in large solar flares in Paper I (Aschwanden, Xu, and Jing 2014a), the goal of this paper II is the determination of thermal energies of the heated flare plasma, in order to study the energy partition of the input (magnetic) energy into various output (thermal and other) energies. A crucial test is the thermal to the magnetic energy ratio, which is expected to be less than unity for magnetic energy release processes (such as magnetic reconnection). Ratios in excess of unity would indicate either inaccurate energy measurements of either magnetic or thermal energies, or would challenge standard flare scenarios where the source of dissipated energy is entirely of magnetic origin. In the standard CSHKP magnetic reconnection model (Carmichael 1964; Sturrock 1966; Hirayama 1974; Kopp and Pneuman 1976), magnetic reconnection drives the nonlinear dissipation of magnetic energy, which is then converted partially into particle acceleration and (precipitation-driven and conduction-driven) flare plasma heating, for which the thermal energy is naturally expected to be a fraction of the total dissipated magnetic energy only. Thus, statistical measurements of the thermal to magnetic energy ratio provide crucial tests for theoretical flare scenarios as well as on the accuracy of observational flare energy measurement methods.

The problematics of determining magnetic energies has been discussed extensively in Paper I. There are three forms of magnetic energies: the potential energy, the free energy (or excess of nonpotential over potential energy), and the dissipated energy, which corresponds to the negative change of free energy during a flare event. Therefore, the measurement of dissipated magnetic energies requires methods that accurately can detect deviations from the potential magnetic field, which are difficult to achieve, as a quantitative comparison of 12 nonlinear force-free field (NLFFF) extrapolation methods of the photospheric magnetic field demonstrated (DeRosa et al. 2009). Alternative NLFFF methods that use the geometry of (automatically traced) coronal loops as constraints appear to be more promising for this task (Paper I). There exists only one study that attempts to compare dissipated magnetic energies with thermal energies in a set of (large eruptive) flare events (Emslie et al. 2012), but the dissipated magnetic energy could not be determined in that study and instead was estimated to amount to of the potential energy, leading to a rather small thermal/magnetic energy ratio, in the order of . Since the ratio of the dissipated magnetic energy to the potential magnetic energy has been found to have a substantially smaller value in Paper I, in the range of for a representative set of M- and X-class flares, we suspect that the thermal/magnetic energy ratio is systematically underestimated in the study of Emslie et al. (2012). As a consequence, we will see in the present study that the thermal/magnetic energy ratio in large solar flares is indeed significantly higher than previously inferred in Emslie et al. (2012).

Even if we have an accurate method to determine the dissipated magnetic energy in solar flares, there are also large uncertainties in the determination of the thermal energy due to the inhomogeneity and multi-thermal nature of the solar flare plasma. In principle, an accurate measure of the multi-thermal energy could be determined if the full 3D distribution of electron temperatures and electron densities are known, such as produced in 3D magneto-hydrodynamic (MHD) simulations (e.g., Testa et al. 2012). In practice, we have only 2D images in multiple wavelengths available to determine the thermal energy. While the lateral extent (in the [x,y]-plane) of flare-related emission in EUV and soft X-rays can be accurately measured for instruments with high spatial resolution, such as with AIA/SDO, the line-of-sight column depth (in -direction) is subject to geometric models. Moreover, the differential emission measure distribution can only be determined as an integral along any line-of-sight, and thus the thermal inhomogeneity and filling factors along the line-of-sight add additional uncertainties. Nevertheless, the presently available high-resolution and multi-wavelength capabilities of AIA/SDO provide unprecedented possibilities to model the 3D flare plasma distribution with much higher fidelity than previous instruments from the the Solar Maximum Mission (SMM), the Solar and Heliospheric Observatory (SOHO), the Transition Region and Coronal Explorer (TRACE), and the Solar-Terrestrial Relationship Observatory (STEREO) missions. It is therefore timely to attempt a statistical study of magnetic and thermal energies using AIA and HMI data from SDO.

The content of this Paper II includes a description of the data analysis methods to determine multi-thermal flare energies (Section 2 and Appendix A), a presentation of observations and results (Section 3 and Tables 1 and 2), discussions of problems pertinent to the determination of thermal energies (Section 4), and conclusions about thermal and magnetic flare energies (Section 5).

2 Data Analysis Methods

2.1 AIA/SDO Temperature Filters

The temperature and density analysis carried out here uses EUV images from the Atmospheric Imaging Assembly (AIA) (Lemen et al. 2012; Boerner et al. 2012) onboard the Solar Dynamics Observatory (SDO) spacecraft (Pesnell et al. 2012). AIA contains 10 different wavelength channels, three in white light and UV, and seven EUV channels, whereof six wavelengths (94, 131, 171, 193, 211, 335 Å) are centered on strong iron lines (Fe viii, ix, xii, xiv, xvi, xviii), covering the coronal range from MK to MK. The 304 Å (He II) filter was not used because it is mostly sensitive to chromospheric temperatures of , which is outside of the range of interest for the flare study here. The calibration of the response functions has changed somewhat over time. Early on in the mission, the response of the 94 and 131 Å channels was underestimated (see Fig. 10 in Aschwanden and Boerner 2011). Here we will use the currently available calibration, which was updated with improved atomic emissivities according to the CHIANTI Version 7 code, distributed in the Solar SoftWare (SSW) Interactive Data Language (IDL) on 2012 February 13.

2.2 Gaussian Differential Emission Measure Distribution Function

The measurement of the thermal energy of an (isothermal) flare plasma requires the determination of the electron density , the electron temperature , and the flare volume . From multi-wavelength observations it is customary to calculate the differential emission measure (DEM) distribution function, which can be integrated over the coronal temperature range and yields a total emission measure , providing a mean electron density (for unity filling factor) and a mean DEM peak temperature . The inference of the DEM can be accomplished either by inversion of the observed fluxes using the instrumental response functions, or by forward-fitting of a suitable functional form of a DEM distribution function. DEM inversion methods are often unstable (Craig and Brown 1976; Judge et al. 1997; Testa et al. 2012; Aschwanden et al. 2015), while forward-fitting methods are generally more robust, but require a suitable parameterization of an analytical function that has to satisfy an acceptable goodness-of-fit criterion. A comparison of 10 DEM inversion and forward-fitting methods has been conducted in a recent study with simulated DEMs, using AIA, the EUV Variability Experiment (EVE), the Ramaty High Energy Solar Spectroscopic Imager (RHESSI, and the Geostationary Orbiting Earth Satellite (GOES) response functions (Aschwanden et al. 2015), where the performance of recent DEM methods is discussed in more detail.

One of the most robust choices of a DEM function with a minimum of free parameters is a single Gaussian (in the logarithm of the temperature), which has 3 free parameters only and is defined by the peak emission measure , the DEM peak temperature , and the logarithmic temperature width , where the DEM parameter has the cgs-units of [cm K],

(1)

where the line-of-sight emission measure is the temperature integral over the Gaussian DEM (in units of [cm],

(2)

The Gaussian DEM (Eq. 1) can be forward-fitted to the preflare background-subtracted observed fluxes in multiple wavelengths ,

(3)

where are the observed fluxes (in units of DN/s) in the wavelengths Å, are the observed background fluxes, are the background-subtracted fluxes, integrated over the entire flare area, is the instrumental response function of each wavelength filter (in units of [DN s cm] per pixel), and the temperature integration is using discretized temperature intervals , which generally are chosen to be equidistant bins of the logarithmic temperature range.

In our DEM forward-fitting algorithm we use a temperature range of MK that is subdivided equi-distantly into 36 logarithmic temperature bins , and a Gaussian temperature width range with 10 values in the range of . At the same time, the DEM peak emission measure value is evaluated from the median ratio of the observed to the model (background-subtracted) fluxes,

(4)

where cm K is the unity emission measure. The best-fitting values of the peak emission measure , the peak temperature and temperature width are found by a global search in the 2-parameter space and by adjustment of the peak emission measure value . The best-fit solution is then evaluated by the goodness-of-fit criterion (e.g., Bevington and Robinson 1992),

(5)

where are the 6 observed flux values, are the flux values of the fitted Gaussian DEM (Eq. 1), are the estimated uncertainties, is the number of degrees of freedom, which is for the number of wavelength filters and the number of model parameters.

In recent studies it is found that the dominant uncertainty in fitting fluxes observed with AIA/SDO comes from the incomplete knowledge of the AIA response functions, which concerns missing atomic lines in the CHIANTI code as well as uncertainties whether photospheric or coronal abundances of chemical elements are more appropriate. The combined uncertainty is estimated to be of the observed AIA fluxes in each wavelength (Boerner et al. 2014; Testa et al. 2012; Aschwanden et al. 2015). This is much more than the typical uncertainty due to photon count statistics, which is of order for typical AIA count rates ( DN s) during flares (Boerner et al. 2014; O’Dwyer et al. 2010). We thus perform the DEM forward-fitting to the 6 wavelength fluxes by using the empirical 10% error of the response functions as an estimate of the flux uncertainties due to calibration and background subtraction errors,

(6)

2.3 Spatial Synthesis of Gaussian DEM Fitting

The choice of a suitable DEM function in forward-fitting methods is almost an art. A Gaussian function (in the logarithm of the temperature) appears to be a good approximation near the peak temperature of most DEM functions, but cannot represent “shoulders” of the primary peak, or secondary peaks at lower or higher temperatures. This is particularly a problem for EUV images that have many different temperature structures with competing emission measures in different areas of the image, such as multiple cores of hot flaring regions, surrounded by peripheral cooler regions. Therefore it is a sensible approach in the DEM parameterization to subdivide the image area of a flare into macropixels or even single pixels, and then to perform a forward-fit of a (single-Gaussian) DEM function in each spatial location separately, while the total DEM distribution function of the entire flare area can then be constructed by summing all DEM functions from each spatial location, which we call the “Spatial Synthesis DEM” method. This way, the Gaussian approximation of a DEM function is applied locally only, but can adjust different peak emission measures and temperatures at each spatial location. Such a single-pixel algorithm for automated temperature and emission measure analysis has been developed for the 6 coronal AIA wavelength filter images in Aschwanden et al. (2013), and a SSW/IDL code is available online (http://www.lmsal.com/aschwand/software/aia/aiadem.html). The flux is then measured in each pixel location and time , and the fitted DEM functions are defined at each location and time separately,

(7)

and are forward-fitted to the observed fluxes at each location and time separately,

(8)

The synthesized differential emission measure distribution can then be obtained by summing up all local DEM distribution functions (in units of cm K),

(9)

and the total emission measure of a flaring region is then obtained by integration over the temperature range (in units of cm),

(10)

Note that the synthesized DEM function (Eq. 9) generally deviates from a Gaussian shape, because it is constructed from the summation of many Gaussian DEMs from each pixel location with different emission measure peaks , peak temperatures , and thermal widths . This synthesized DEM function can be arbitrarily complex and accomodate a different Gaussian DEM function in every spatial location .

Typically we process images with a field-of-view of solar radius, which corresponds to about 520 AIA pixels. Subdividing these images into macropixels with a bin size of 4 full-resolution pixels, we have a grid of 130130 macropixels and perform single-Gaussian DEM fits per time frame, per wavelength set, and per event. We illustrate the spatial synthesis procedure with single-Gaussian DEMs in Fig. 1, where we can see that the local temperature discrimination yields a higher temperature contrast for increasingly smaller macropixels, from down to 2 image pixels. The convergence of the DEM with decreasing bin size is depicted in Fig. 2, for three different times of a flare. The initial single-Gaussian DEM function fitted to the fluxes of a pixel area (blue curves in Fig. 2) converges to a double-peaked DEM at the flare peak time (red curve in middle panel of Fig.2), synthesized from macropixels, which evolves then into a broad single-peaked DEM in the postflare phase (red curve in bottom panel of Fig. 2).

2.4 Flare Geometry

The total emission measure EM of a flaring active region, such as defined for a single Gaussian DEM (Eq. 2) or for a spatially synthesized DEM as defined in Eq. (10), yield the product of the squared mean electron density times the flare volume. If we can estimate the flare volume from the imaging information, we can then infer the mean electron density (for unity filling factor). There are many ways to measure a flare area. Two major problems are the choice of a suitable wavelength (in multi-temperature data), and secondly the choice of a threshold, especially in flares that have a large dynamic range of fluxes over several orders of magnitude.

In order to eliminate the choice of wavelengths, we use the emission measure maps (Eq. 7), where we find a range of cm K for the peak values. We choose an emission measure threshold near the lower bound of this range, i.e., cm K, unless this threshold exceeds the 50% level of the peak emission measure, in which case we use the 50% level. This way, a flare area is always defined, even for flares with low emission measures. We measure then the flare area of thermal emission by counting the number of macropixels above the threshold in an emission measure map , which multiplied with the macropixel size yields an area (in units of cm), a length scale , and a flare volume .

One problem that we encountered in our analysis is that the flare area at the peak time is sometimes largely inflated due to saturation of the EUV CCD, pixel bleeding, and diffraction patterns, and thus no reliable flare area can be measured at the flare peak time . Since the automated exposure control alternates between short and long exposure times during saturation, an over-exposed time frame (with flare area at the peak time ) is interpolated from the preceding time step (with flare area at time ) and the following time step (with flare area at time . In the derivation of geometric parameters in this study we use the maximum flare area measured during the flare duration interval.

2.5 Multi-Thermal Energy

If we substitute the expression of the total emission measure at the peak time of the flare, , into the expression for the thermal energy , we have the relationship

(11)

This expression is accurate only if the DEM function is a delta-function with a small thermal width , which can then be characterized by the peak emission measure at the DEM peak temperature .

For every broad temperature DEM distribution , as it is the case for most solar flares, it is more accurate to perform the temperature integral (or summation over discrete temperature increments , which may be logarithmically binned). In the discretized form, the emission measure is integrated over the temperature interval is , and the thermal energy can be written as a summation of partial thermal energies from each temperature interval (see Appendix A),

(12)

While the DEM peak temperatures were determined within the parameter space of MK, the temperature integral of the thermal energy (Eq. 12) was calculated in an extended range of , in order to fully include the Gaussian tails of the DEM fits in each macropixel. This yields a more accurate value of the total multi-thermal energy, since it avoids a truncation at the high-temperature tail of the composite DEM distribution. Note that we defined the thermal energy in terms of the volume-integrated total emission measure ( (in units of cm), in contrast to the column depth integrated emission measure per area, (in units of cm) used in the spatial synthesis method (Eq. 7), where the emission measure is quantified per unit area or per image pixel (see detailed derivation in Appendix A). We find that the more accurate expression of Eq. (12) typically yields a factor of higher values for the thermal energies than the single-temperature approximation of Eq. (11), and thus represents a very important correction for broad multi-temperature DEMs.

Considering the more complex DEM functions obtained from spatial synthesis with Eq. (9), we will see that the DEM function often has multiple peaks, and thus it does not make any sense anymore to talk about a single peak emission measure and single peak temperature . In order to characterize such complex DEM functions with a characteristic temperature value, it makes more sense to define an emission measure-weighted temperature , which we define as,

(13)

and approximately characterizes the “centroid” of the DEM function.

3 Observations and Results

3.1 AIA Observations

The dataset we are analyzing for this project on the global energetics of flares includes all M- and X-class flares observed with SDO during the first 3.5 years of the mission (2010 June 1 to 2014 Jan 31), which amounts to 399 flare events, as described in Paper I (Aschwanden, Xu, and Jing 2014a). The catalog of these flare events is available online, see http://www.lmsal.com/aschwand/RHESSI/flareenergetics.html. We attempt to calculate the thermal energies in all 399 catalogued events, but we encountered 8 events with incomplete or corrupted AIA data, so that we are left with 391 events suitable for thermal data analysis.

AIA provides EUV images from four detectors with a pixel size of , corresponding to an effective spatial resolution of . We generally use a subimage with a field-of-view of . AIA records a full set of near-simultaneous images in each temperature filter with a fixed cadence of 12 seconds, while our analysis of the flare evolution is done in time increments of hrs. This cadence may underestimate the maximum thermal energy during a flare in some cases, but is estimated to be less than a factor of 2.

3.2 Example of DEM Analysis

An example of our DEM analysis is summarized in Fig. 3, which applies to the first event (# 1) of our list, a GOES M2.0 class flare in active region NOAA 11081 at N23 W47, observed with AIA/SDO on 2010 June 12, 00:00-01:30 UT. The GOES 1-8 Å light curve is shown in Fig.3a, with GOES flare start time at =00:30 UT, peak time at =00:58 UT, and flare end time at =01:02 UT, according to the NOAA event list. The flare end time is defined when the GOES flux drops down to 50% of the peak value, according to NOAA convention, but flare-related EUV emission always lasts significantly longer. In our thermal analysis we add margins of hr before and after the NOAA flare start and end times, which covers the time interval of 00:00-01:32 UT in this event. We use a cadence of hr, which yields 14 time frames for this event. The 6 AIA flux profiles are shown in Fig. 3b, which show a very simple evolution of a single peak in all 6 EUV wavelengths, coincident with the SXR peak in GOES time profiles. The peak time occurs in time frame , at 00:58 UT. Flare background fluxes have been subtracted in every spatial macropixel ( image pixels) separately (according to Eq. 8). Because every macropixel has a different background value , the summation of all background subtracted profiles leaves residuals that amount to a fraction of of the peak flux (see preflare time profile of spatially-summed fluxes in Fig. 3b).

For the DEM analysis we read 14 (time frames) times 6 (wavelength) AIA images, extract subimages within a solar radii, which amount to a size of about 522 pixels, we rebin the images into macropixels, yielding a spatial 2D array of macropixels, subtract in each macropixel a temporal minimum flux background, forward-fit a Gaussian DEM function in each macropixel, which yields the 3 Gaussian parameters: the DEM peak emission measure , DEM peak temperature , and thermal width , or a Gaussian DEM function (Eq. 7) for each macropixel. Summing the single-Gaussian DEMs yields then a spatially synthesized DEM function that is shown in Fig. 3f for each time step . The evolution of the DEM peak starts from a DEM peak temperature of MK and peaks at a value of MK, and decreases again to the preflare value. The evolution of this peak temperature is also shown in Fig. 3c, along with the evolution of the mean temperature , the mean electron density , and the thermal energy (Eq. 12), in normalized units. The spatial distribution of the emission measure map is shown in Fig. 3e, where instrumental diffraction patterns (diagonal features) and pixel bleeding (vertical feature) are visible also at the flare peak time. Since these instrumental effects are mostly a spatial re-distribution of photons inside the FOV of the observed image, we expect that they do not affect much the obtained DEM function after spatial integration. The emission measure maps serve to measure a wavelength-independent flare area at the flare peak time (above some threshold; Section 2.4), which yields the equivalent length scale . The physical parameters obtained for this event at the flare peak time are listed in Fig. 3 (bottom right). Note that the peak temperature is only MK, while the emission measure-weighted temperature MK (Eq. 13) is substantially higher. The flare length scale (indicated with a square in Fig. 3e) is Mm, the electron density is cm, and the thermal energy is erg for this event.

The goodness-of-fit or reduced -criterion of the DEM fit yields a mean and standard deviation of for the 14 DEM fits of this particular event #1 (Fig. 3). As mentioned before (Section 2.2), the calculation of the reduced -criterion is based on the estimated uncertainty of the observed AIA fluxes, which is dominated by the incomplete knowledge of the instrumental response functions, estimated to be of order (Boerner et al. 2014; Testa et al. 2012). Although the -value found for this particular event is relatively low, compared with the mean statistical expectation, it fits into the broad range of the obtained overall statistical distribution. In Fig. 6g we plot the distribution of the -values of the 391 fitted flare events, where the value of each flare event is a time average, as well as a spatial average (using the spatial synthesis method). The peak of this distribution is near and the median is (Fig. 6g), which indicates that the chosen model of the DEM parameterization (Eq. 1) yields a best fit that is consistent with the empirical estimates of uncertainties in the flux or response functions (Eq. 6). Of course, the Gaussian DEM parameterization, even when individually fitted in each pixel, may not always represent the best functional form of observed DEMs, which may explain some -values significantly larger than unity. A more accurate goodness-of-fit test would require a more complex parameterization of the DEM function and a physical model of the flux uncertainties , which should include systematic uncertainties due to the AIA flux calibration, the atomic (coronal and photospheric) abundances, the atomic transitions (computed with the CHIANTI code here), and the background subtraction method, which is not attempted here.

3.3 DEM Functions of Extreme Events

In Fig. 4 we show the differential emission measure distributions of 12 extreme events among the 391 analyzed M and X-class flare events. These 12 events were selected by the minimum and maximum values in the parameters of the length scale (Fig. 4a,b), the DEM peak temperature (Fig. 4c,d), the emission measure-weighted temperature (Fig. 4e,f), the electron density (Fig. 4g,h), the DEM peak emission measure ( Fig. 4i,j), and flare duration (Fig. 4k,l). This selection of extreme events demonstrates the variety and diversity of DEM functions we encountered among the analyzed flare events. It shows also the versatility and adequacy of the DEM parameterization using spatially synthesized (single-Gaussian) DEM functions.

The length scales of thermal emission vary from Mm (#256; Fig. 4a) to Mm (#132; Fig.4b). What is striking between the evolution of these two events is that the flare with the smallest size shows very little increase in the emission measure at any temperature, while the largest flare exhibits a large increase in the high-temperature emission measure.

For the peak temperatures we find a range from MK (#305; Fig. 4c) to MK (#67; Fig. 4d), which is not necessarily coincident with the emission measure-weighted temperature . This is clearly shown in the case with the smallest peak temperature, which is far below the emission measure-weighted temperature of peaks in the DEM, which can make the peak temperature to jump around wildly as a function of time, as long as their associated DEM peak emission measures are comparable. This is a major reason why the DEM peak temperature should not be used in the estimate of thermal energies, but rather the emission measure-weighted temperature that is a more stable characteristic of the DEM function.

For the emission measure-weighted DEM function we find a range from MK for the coldest flare (#102; Fig. 4e) to MK for the hottest flare (#316; Fig. 4f), which is close to the upper limit of the temperature range where AIA is sensitive. The coldest flare in our selection with MK is a M1.3 GOES class, while the hottest flare with MK is a M3.5 GOES class. The GOES class does not necessarily correlate with the flare temperature, which is expected since the GOES class is mostly defined by the emission measures (in soft X-rays) rather than by the temperature.

For the electron density we find a range from cm (#396; Fig. 4g) to cm (#375; Fig. 4h), which corresponds to a variation by a factor of . The lowest density corresponds to a low peak temperature ( MK), while the highest density yields a high peak temperature temperature ( MK). For a fixed loop length, a correlation between the electron density and the electron temperature is expected according to the RTV scaling law, i.e., (Eq. 21).

For the DEM peak emission measure we find a variation from cm (# 241; Fig. 4i) to cm (# 147; Fig. 4j), which varies by a factor of . The corresponding GOES classes are M1.3 and X5.4, which are both near the limits of the GOES class range (M1.0 - X6.9) found in our selection. The event with the largest emission measure represents the second-largest GOES class (X5.4) in our selection, and thus the GEOS class is indeed a good proxy to estimate the emission measure of flares.

The time range of flare durations is found to vary from hr (#56; Fig. 4k) to hr (#130; Fig. 4l). The longest duration event, however, does not have extreme values in temperature, emission measure, or length scale.

3.4 Statistics of Physical Parameters

We provide some statistics on the derived thermal parameters, such as the length scale , the thermal volume , the DEM peak temperature , the emission measure-weighted temperature , the electron density , the total emission measure , and the thermal energy , in form of scatterplots (Fig. 5) and size distributions (Fig. 6). The inferred physical parameters are listed for the 28 X-class flares in Table 1, and for all 391 M and X-class flares in the machine-readable Table 2. The ranges of these physical parameters have already been discussed in terms of extreme values in Section 3.3. The scatterplots shown in Fig. 5 reveal us which parameters are correlated and indicate simplified scaling relationships, while the size distributions shown in Fig. 6 reveal us the powerlaw tails that are typical for dissipative nonlinear systems governed by self-organized criticality (SOC).

The scatterplots shown in Fig. 5 indicate that the thermal energy is correlated with the length scale by the scaling relationship (Fig. 5a),

(14)

and consequently is correlated with the volume (Fig. 5b) also,

(15)

and is correlated also with the total emission measure (Fig. 5f)

(16)

but strongly anti-correlated with the electron density (Fig. 5e), and is not correlated with the temperatures (Fig. 5c) and (Fig. 5d).

Regarding the size distributions, the fractal-diffusive self-organized criticality (FD-SOC) model provides predictions for the size distributions (Aschwanden 2012; Aschwanden et al. 2014b). The most fundamental parameter in the FD-SOC model is the length scale , which according to the scale-free probability conjecture is expected to have a size distribution for Euclidean space dimension . We find agreement between this theory and the data within the uncertainties of the fit (Fig. 6a),

(17)

For the volume of thermal emission, the FD-SOC model predicts a powerlaw slope of , and we find good agreement (Fig. 6b),

(18)

For the energy , using the observed scaling, i.e., with (Eq. 15), we expect then a size distribution of , which predicts a powerlaw slope of , which is indeed consistent with the observed slope,

(19)

We have to keep in mind that the FD-SOC model is a very generic statistical model that predicts a universal scaling law for spatial parameters, based on the scale-free probability conjecture, i.e., (Aschwanden 2012), while the scaling of other physical parameters, such as the energy, , requires a physical model that is specific to each SOC phenomenon. In the next Section we will discuss the RTV scaling law, which we apply to model the otherwise unknown scaling of the energy with the volume, .

3.5 The Rosner-Tucker-Vaiana Scaling Law

A well-known physical scaling law between hydrodynamic parameters of a coronal loop is the Rosner-Tucker-Vaiana law (Rosner et al. 1978), which is derived under the assumption of energy balance between the energy input by a volumetric heating rate (in units of [erg cm s]) and the radiative and the conductive loss rates , i.e., , which yields two scaling laws between the loop length , loop apex electron temperature , average electron density , and heating rate . While this original derivation applies to a steady-state of a heated coronal loop, it turned out that the same scaling laws apply also to solar flares at the heating/cooling turnover point (Aschwanden and Tsiklauri 2009). Solar flares are generally not heated under steady-state conditions, except at the turning point of maximum temperature, when the heating rate and the radiative and conductive losses are balanced for a short instant of time. Before reaching this turning point, heating dominates the cooling losses, while the cooling dominates after this turning point.

We can express the RTV scaling laws explicitly for the parameters (Aschwanden and Shimizu 2013),

(20)
(21)
(22)
(23)
(24)

We can then compare the observed parameters with these theoretically predicted parameters , which is shown in Fig. 7. Note that we use the weighted temperature and the emission measure and density measured at the peak time of the flare here. While the original RTV scaling law has no free parameters, the scaling between the average loop half length (required for the RTV scaling law) and the average length scale (measured here during the flare duration) requires a geometric model, as well as information on filling factors and fractal geometry. Since detailed modeling of the 3D geometry of flare loop configurations is beyond the scope of this study, we determine the average scaling ratio empirically and find that a relationship of yields a satisfactory match between the observed and the theoretically predicted physical parameters of the RTV scaling law (indicated with the dotted diagonal line expected for equivalence in Fig. 7).

We see now that the 3-parameter RTV scaling laws (Fig. 7) retrieve the relationships obtained from 2-parameter correlations (Fig. 5). The correlation of the thermal energy with length scale, (Eq.14; Fig. 5a) is similar to the RTV relationship (Eq. 24), which is equivalent to the relationship with the volume, i.e., (Eq.15; Fig. 5b) and the RTV relationship (Eq. 24). Combining the RTV relationships between (Eq. 24) and (Eq. 23) we obtain , which is similar to the observed 2-parameter correlation . Thus the 2-parameter correlations are approximations of the 3-parameter (RTV) scaling laws, and thus can be explained by a physical model, although they are less accurate because of the neglected third parameter. Comparing the observed and RTV-predicted values (as shown in Fig. 7), we find that the (multi-)thermal energies , emission measures , and length scales are correlated with the observed values within a standard deviation, while the temperature and density deviate more than a standard deviation, which is likely to be caused by their smaller ranges of values and the associated truncation effects (e.g., see calculation of truncation effects in Fig. 8 of Aschwanden and Shimizu 2013).

3.6 Comparison of Magnetic and Thermal Energies

The main goal of the global flare energetics project is the comparison and partitioning of various flare energies. In Paper I we calculated the dissipated magnetic energies in 172 M and X-class flares, based on the (cumulative) decrease of free energies during each flare, which were found to have a range of erg. In this study we calculated the thermal energy at the peak time of the total emission measure and find a range of erg. A scatterplot between the magnetic and thermal energies is shown in Fig. 8a. From this diagram we see that the average ratio is , with a standard deviation by a factor of 4.8, which defines a typical range of . Thus, the thermal energy amounts generally only to a fraction of of the dissipated magnetic energy, as determined with the coronal NLFFF method.

We show also a scatterplot of the thermal energy with the dissipated magnetic energy as computed with the photospheric NLFFF method, which could be performed only for 12 events (Fig. 8b). In this small dataset, the average ratio is , with a scatter by a factor of 6.5, or a range of . In four out of the 12 events the thermal energy exceeds the dissipated magnetic energy, which is likely to be a false result due to underestimates of the dissipated magnetic energy, since the PHOT-NLFFF code seems to be less sensitive in measuring decreases of the free energy than the COR-NLFFF code, possibly due to a smoothing effect caused by the preprocessing procedure.

We compare the new results also with the previous study by Emslie et al. (2012), where the thermal energy could be determined for 32 large eruptive flares, while the magnetically dissipated energy was estimated to be 30% of the potential energy. In that study, the average ratio of the thermal to the magnetically dissipated energy is found to be with a scatter by a factor of , which yields a range of 0.2%-1.0% (Fig. 8c). Since the thermal energies have a similar median value ( erg) as we find in this study ( erg), the discrepancy is most likely attributed to an overestimate of the magnetically dissipated energies, as well as to a selection effect of larger flares. The median value of the magnetically dissipated energy is erg in Emslie et al. (2012), while we find a median value of erg, which is about an order of magnitude lower, and goes along with our finding that the free energy is about 1%-25% of the potential free energy, rather than 30% as assumed in the study of Emslie et al. (2012).

4 Discussion

4.1 Previous Measurements of Thermal Flare Energies

Most previous studies estimated thermal flare energies by using the isothermal relationship, i.e., , which requires a DEM analysis (to obtain the peak emission measure and peak temperature ) and imaging observations (in order to obtain the flare area or volume ), measured at the flare peak time. A DEM analysis requires multiple temperature filters, and thus thermal flare energies can only be obtained from instruments with multi-wavelength imaging capabilities. Statistics of thermal energies was gathered for large flares, nanoflares, and impulsive brightenings in EUV and soft X-rays from Skylab S-054 (Pallavicini et al. 1977), Yohkoh/SXT (Shimizu 1997; Aschwanden and Benz 1997; Shimojo and Shibata 2000), SoHO/EIT (Krucker and Benz 2000); TRACE (Aschwanden et al. 2000; Aschwanden and Parnell 2002), RHESSI (Emslie et al. 2004, 2005, 2012; Caspi et al. 2014), and AIA/SDO (Aschwanden and Shimizu 2013).

How consistent are the thermal energies determined here with previous measurements ? We compile some statistics on thermal energy measurements in large flares in Table 3, by listing the instruments, the number of events, and the parameter ranges of the spatial scale , the peak electron temperature , the peak electron density , the peak emission measure , and the thermal energy . A scatterplot of thermal energies versus the flare volumes measured in large flares is shown in Fig. 9. In particular, statistics on large flares (approximately GOES M- and X-class) has been analyzed in 31 events from Skylab S-054 (Pallavicini et al. 1977), in 32 events from RHESSI (Emslie et al. 2012), in 155 events from AIA/SDO (Aschwanden and Shimizu 2013), and in 391 events from AIA/SDO in the present study. Table 3 provides the ranges of reported physical parameters, but we have to be aware that different event selections have been used in the different datasets.

4.2 Isothermal Versus Multi-Thermal Energies

The most striking discrepancy appears between the isothermal and multi-thermal energies, which is measured for the first time in this study. We overlay the thermal energies as a function of the flare volume for the same four studies in Fig. 9. In the present study we calculate both the isothermal energy (Eq. 11) and the multi-thermal energy (Eq. 12) and find a systematic difference of (Fig. 9, 10). Note the offset of the linear regression fits between isothermal energies (black line and diamonds in Fig. 9) and multi-thermal energies (orange line and diamonds in Fig. 9). The multi-thermal flare energy definition has to our knowledge not been applied in the calculation of thermal flare energies in all previous studies, but is very important, because it boosts the thermal energy produced in flares statistically by an average factor of , as measured from the energy offset in cumulative size distributions (Fig. 10). This is related to the incompatibility of iso-thermal temperatures inferred from GOES, AIA, and RHESSI data, investigated in a recent study (Ryan et al. 2014), which can only be ameliorated with broadband (multi-temperature) DEM distributions. The systematic underestimate of the thermal energy, when the isothermal approximation is used, may also be the reason why a very low value of (Fig. 8c) was found for the thermal/magnetic energy ratio in Emslie et al. (2012), compared with our range of (Fig. 8a) calculated in the present study.

4.3 Flare Volume Measurements

The thermal energy depends on the volume , and thus the measurement of flare areas or volumes are crucial to obtain an accurate energy value. Since we can directly observe in 2D images the flare area only, the definition of a flare volume is subject to modeling. The simplest definition is the Euclidean relationship and , but more complicated definitions involve the fractal dimension (Aschwanden and Aschwanden 2008a,b), 3D filling factors (Aschwanden and Aschwanden 2008b), or other geometric concepts to characterize the inhomogeneity of flare plasmas. One prominent modeling concept is the hydrostatic density scale height , which depends on the flare plasma temperature and can be used to estimate the vertical height above the solar surface. The detailed geometry of the flare plasma often appears to have the geometry of an arcade of loops, which can be highly inhomogeneous, depending on the spatial intermittency of precipitating electrons along the flare ribbons. Nevertheless, regardless how complicated the spatial topology of a flare is, the thermal energy is a volume integral and thus should be rotation-invariant to the aspect angle or heliographic location (assuming that we measure correct DEMs along each line-of-sight). This argument justifies isotropic geometries such as hemispheric flare volumes (Aschwanden and Shimizu 2013), or the related Euclidean relationship . Moreover, the height of semi-circular flare loops is about half of the footpoint separation , and thus the volume can be approximated with a cube . Hence, we use the simple Euclidean relationships and in this paper. Detailed geometric 3D modeling of the flare volume at different temperatures is beyond the scope of this study.

How consistent is the flare volume measurement in the present work with previous studies? Most flare area measurements are done using a flux threshold, which is chosen above the data noise level and lower than the maximum flux in an image, but is arbitrary within this range. The volume of limb flares from Skylab data (Pallavicini et al. 1977) was calculated from measuring the height and size of bright soft X-ray emission in photographs and yields a remarkable good match for the isothermal energy with our present study (blue line and crosses in Fig. 9). The previous study of 155 M- and X-class flares with AIA/SDO data (Aschwanden and Shimizu 2013) involved multiple flux threshold levels and was combined from 6 different wavelength filters, but is consistent with the area measurements in this study within a factor of . This uncertainty translates into a factor of for volumes, total emission measures, and thermal energies.

4.4 Spatial-Synthesized DEM Analysis

DEM analysis is a prerequisite tool for determining thermal energies. The thermal width of the DEM distribution is the most crucial parameter to discriminate between isothermal and multi-thermal cases. Numerical integrations of the DEM temperature distribution show that multi-thermal DEMs yield in the average 14 times higher (multi-)thermal energies than isothermal (delta-function-like) DEM distributions (Fig. 10). Thus, the fidelity of the DEM reconstruction is important for the accurate determination of thermal flare energies.

In this study we employed the spatial synthesis DEM method (Section 2.3 and Aschwanden et al. 2013), which approximates the DEM in every (macro-)pixel with a 3-parameter Gaussian DEM function, which is then synthesized for the entire flare volume by adding all partial DEM distributions from each pixel. In Fig. 2 we demonstrated that this method converges to a unique DEM solution by iterating from large macro-pixels to smaller sizes, down to a single image pixel. We find that this method converges rapidly, when iterating macro-pixel sizes , , on an image with full size (Figs. 1 and 2). This means that macropixels with a size of a few pixels isolate hot flare areas and ambient cooler plasma areas sufficiently to be characterized with a single-peaked DEM function. The fast convergence to a unique DEM function is very fortunate and relieves us from more sophisticated DEM modeling.

We find that the largest uncertainty in DEM modeling comes from uncertainties of the instrumental response functions, including missing atomic lines, chemical abundance variations, and preflare-background subtraction, which all combined are estimated to be of order (Boerner et al. 2014; Testa et al. 2012; Aschwanden et al. 2015), which is also confirmed from DEM inversions applied to synthetic data generated with 3D magneto-hydrodynamic (MHD) simulations (Testa et al. 2012).

4.5 Scaling Law and Extreme Events

In Section 3.5 we derived a physical scaling law for the thermal energy, (Eq. 24), based on the RTV scaling law of 1-D hydrostatic loops that are in steady-state energy balance between heating and cooling processes. The observational measurements of (multi-thermal) energies were found indeed to match this predicted relationship closely (see correlation between theoretically predicted and observed thermal energies in Fig. 7e).

Let us consider the parameters of the most extreme events. For the largest flare in our dataset, we found a length scale of Mm solar radius, the hottest flare has an (emission measure-weighted) temperature of MK, and the most energetic flare has a multi-thermal energy of erg. The upper limit for thermal energies is of particular interest for predictions of the most extreme (and worst events for space weather and astronauts). Based on the largest flare events observed in history, with a GOES-class of X10 to X17, an even larger maximum flare energy of erg was estimated, while stellar flares may range up to erg (see Fig. 3 in Schrijver et al. 2012).

On the other extreme, the RTV scaling law (Eq. 24) may also be applied to predict the magnitude of the smallest coronal flare events. An absolute lower limit of flare temperatures is the temperature of the ambient solar corona, which is approximately MK. For a lower limit of the spatial size of a flare event we can use the size of the smallest loop that sticks out of the chromosphere, which has a height of Mm and a semi-circular loop length of Mm. The apex segment that sticks out of the chromosphere can have a projected length scale as short as Mm. The extrapolated thermal energy of the smallest flare is then estimated to be erg, which is about 9 orders of magnitude smaller than the largest flare, and thus called a nanoflare. This is consistent with the smallest observed nanoflares, which have been found to have a thermal energy of erg (Krucker and Benz 2000; Parnell and Jupp 2000; Aschwanden et al. 2000; Aschwanden and Parnell 2002). Note that these predictions are based on our calculations of the multi-thermal energy, which amounts to an average correction factor of .

4.6 Self-Organized Criticality Models

The statistics of nonlinear dissipative events often follows a scale-free powerlaw distribution, in contrast to (linear) random processes (such as photon statistics of a steady source), which follow a Poisson distribution (or its exponential approximation). The powerlaw function in occurrence frequency distributions (or size distributions) has been declared as a hallmark of nonlinear systems governed by self-organized criticality (SOC; Bak et al. 1987). A quantitative derivation of the powerlaw distribution function of SOC processes has been derived in the framework of the fractal-diffusive self-organized criticality model (FD-SOC: Aschwanden 2012, Aschwanden et al. 2014b), which predicts universal values for the powerlaw slopes of spatio-temporal parameters, based on the scale-free probability conjecture, , the fractal geometry of nonlinear dissipative avalanches, and diffusive transport of the avalanche evolution. We measured the size distributions of spatio-temporal physical parameters in solar flares (length , area , volume , durations ) and found indeed agreement with the predictions of the standard FD-SOC model (Fig. 6). The size distributions of the other physical parameters (, , , ), however, are not universal, but depend on the underlying physical process of the SOC phenomenon. For solar flares in particular, we found that the RTV scaling law is consistent with the observed parameter correlations and size distributions. Most of the physical scaling laws are expressed in terms of powerlaw exponents (such as the thermal energy, i.e., ), which has the consequence that all size distributions of physical parameters are also predicted to have a powerlaw shape, except for finite-size effects (that produce a steep drop-off at the upper end) and incomplete sampling due to limited sensitivity (which produces a turnover at the lower end), as manifested in the size distributions shown in Fig. 6. What the observed size distributions show, is the scale-free parameter range (also called inertial range) of SOC processes over which an identical physical process governs nonlinear energy dissipation. The size distributions shown in Fig. 6 exhibit no indication of multiple or broken powerlaws in the inertial range of M- and X-class flares. Note that such powerlaw distributions occur only for statistically complete samples (above some threshold value). Datasets with “hand-selected” events (such as the 37 eruptive flare events sampled in Emslie et al. 2012) do not exhibit powerlaw-like size distributions.

Various flare energy size distributions have been compared in previous studies (e.g., see composite size distribution in Fig. 10 of Aschwanden et al. 2000, based on size distributions published by Shimizu 1997; Crosby et al. 1993; Krucker and Benz 2000; Parnell and Jupp 2000; and Aschwanden et al. 2000). Such composite size distributions have been used to characterize the overall size distributions from the smallest nanoflare to the largest X-class flare. However, the construction of a synthesized flare energy size distribution requires a consistent definition of energy, which is not the case in most of the published studies, since they contain thermal as well as nonthermal energies. In order to illustrate this discrepancy we show the cumulative size distributions of isothermal, multi-thermal, and magnetic flare energies in Fig. 10, where we sample an identical event list, which is the common subset of the three energy forms and contains 171 events. In Fig. 10 we show a cumulative size distribution of these events, constructed with the inverse rank-order plot. Note that the three different forms of energy differ by an approximate amount of and . It is therefore imperative to derive the same form of energy when comparing the occurrence probabilities from the size distributions of different datasets.

4.7 Thermal/Magnetic Energy Ratios

One key result of this study is the thermal/magnetic energy ratio, for which we found a range of . We consider this result to be a substantial improvement over previous estimates, where isothermal instead of multi-thermal temperature distributions were used and no measurements of magnetically dissipated energies were available, resulting into a much lower estimate of the thermal energy content in the order of (Emslie et al. 2012). The thermal energy is smaller than the magnetically dissipated energy for essentially all events (Fig. 8a), while the few mavericks can be explained by inaccurate energy measurements, either on the thermal or magnetic part. This result is certainly consistent with most magnetic reconnection models (where magnetic energy is converted into acceleration of particles) and the thick-target model (where the accelerated particles lose their energy by precipitation down to the chromosphere and heat up the chromospheric plasma). The amount of energy that goes into chromospheric and coronal plasma heating may well be larger than the thermal energy measured here, because we measured only the thermal energy content at the peak time of the flare, while multiple heating phases may occur before and after the flare peak. Even if we would add up all thermal energies from every flare episode that shows a subpeak in the soft or hard X-ray time profile, we would still underestimate the thermal energy because (radiative and conductive) cooling processes are not considered in the calculation of the thermal energy content here. Thus, the multi-thermal energy content calculated here represents only a lower limit of the heating energy that goes into flare plasma heating during a flare. A complete calculation of the multi-thermal flare energy would require a forward-fitting method of the evolution of the heating rate that fits the observed conductive and radiative energy loss rate , which is beyond the scope of this study, since this would require realistic geometric 3D models of flare loop arcades also.

5 Conclusions

As part of a global flare energetics study that encompasses all forms of energies that are converted during solar flares (with or without CMEs) we calculated the dissipated magnetic energy of 172 GOES M- and X-class events (in Paper I), and the multi-thermal energy at the peak time of 391 flare events (in this Paper II here). The catalog of these flare events is available online, see http://www.lmsal.com/aschwand/RHESSI/ flareenergetics.html. The major results of this study are:

  1. We computed the differential emission measure (DEM) distribution function of all 391 flares in time steps of hr using the spatially-synthesized Gaussian DEM forward-fitting method, which yields a detailed shape of the multi-thermal DEM distribution. This method is found to be robust and converges as a function of the macro-pixel size to a unique DEM solution, subject to uncertainties in terms of the instrumental response function and subtracted background fluxes in the order of . The multi-thermal DEM function yields a significantly higher (typically by a factor of , but comprehensive, (multi-)thermal energy than the isothermal energy estimated from the same data.

  2. For the overlapping dataset of 171 flare events for which we could calculate both the magnetically dissipated energies and the multi-thermal energies , we find a ratio of . This value is about an order of magnitude higher than previous estimates, i.e., , where isothermal energies from GOES X-ray data rather than multi-thermal energies from EUV AIA data were calculated, and a ratio of was assumed ad hoc (Emslie et al. 2012).

  3. The computed thermal energies are consistent with the RTV scaling law , which applies to the energy balance between the heating and (conductive and radiative) cooling rate at the turning point of the flare peak time. In our analyzed dataset of M and X-class flares we find thermal energies in the range of erg. In comparison, the largest historical flare event has been reported to have an energy of erg, while the smallest coronal nanoflares with a length scale of Mm and coronal temperature of MK are predicted to have values of erg according to the RTV scaling law.

  4. The size distributions of the spatial parameters display a powerlaw tail with powerlaw slopes of for the length scales, for flare volumes, for flare volumes, and are consistent with the predictions of the fractal-diffusive self-organized criticality model combined with the RTV scaling law (; ; ).

After we have established the measurements of magnetically dissipated flare energies (Paper I) and the multi-thermal energies (Paper II here), we plan to measure the non-thermal energies (using RHESSI), the kinetic energies of CMEs (using AIA/SDO and STEREO), and the various radiative energies in gamma-rays, hard X-rays, soft X-rays, EUV, and bolometric luminosity in future studies. The ultimate goal is to quantify and understand the energy partition in a comprehensive set of large flare/CME events, and to identify the physical processes that are consistent with the various flare energy measurements.


We appreciate helpful and constructive comments from an anonymous referee and from a number of participants of the RHESSI-13 workshop. Part of the work was supported by NASA contract NNG 04EA00C of the SDO/AIA instrument and the NASA STEREO mission under NRL contract N00173-02-C-2035.

APPENDIX A: Thermal Energy of a Multithermal DEM

Thermal energies of solar flares are generally estimated by the expression for a homogeneous and isothermal plasma (Eq. 11),

where is the electron density, the electron temperature, and the volume, measured at the peak time of a flare. The values and are generally determined from the peak in a DEM distribution function.

However, since the solar flare plasma is inhomogeneous and multi-thermal, we can calculate a more accurate expression for the total thermal energy when imaging observations are available. Ideally, such as in the case of an MHD simulation, the full 3D distributions of temperatures and electron densities are known, so that the most accurate expression for thermal energies can be computed by volume integration (e.g., Testa et al. 2012),

For numerical computations, we use a discretized 3D volume that is aligned in the z-direction with the line-of-sight, while images in different wavelengths have the 2D coordinate system with pixel size . A DEM analysis yields an inversion of a DEM distribution in every pixel at location . The column depth emission measure is defined by

which yields an average density along the line-of-sight column depth with length at each pixel position ). We can then define a thermal energy for each column depth by summing all contributions from each temperature interval (Eq. 11),

The total thermal energy in the computation box can then be obtained by summing up the partial thermal energies from all pixels,

where we replaced the partial DEM functions per column depths by the total DEM function ,

which leads to the expression given in Eq. (12).

We compare now the thermal energy (Eq. A5) computed in this way for a multi-thermal DEM distribution with the isothermal approximation (Eq. A1) by their ratio in Fig. 11, given for a set of thermal widths in the single-Gaussian DEM function (Eq. 1) that is used for DEM modeling in each pixel. For small values, say , the DEM distributions are almost isothermal, and thus the approximation (Eq. A1) is appropriate and we obtain a ratio near unity ). For broader multi-thermal DEM functions, the ratio increases systematically, up to a factor of . At higher temperatures, the ratio decreases because the temperature range between the peak of the DEM and the upper limit (here at MK) becomes increasingly smaller and thus has less weight in the asymmetric -weighting of the thermal energy contributions. Observed DEM peaks have typically a logarithmic temperature half width of (see Fig. 4 for examples), and thus the multi-thermal energy ratios vary by a factor of for flare peak temperatures in the range of MK (Fig. 11). Since the observed DEM distributions are generally multi-peaked, the ratios tend to be higher than estimated from single-Gaussian DEMs as shown in Fig. (11).

References

  • (1)
  • (2) Aschwanden, M.J., and Benz, 1997, ApJ 480, 839.
  • (3) Aschwanden, M.J., Tarbell, T., Nightingale, R., Schrijver, C.J., Title, A., Kankelborg, C.C., Martens, P.C.H., and Warren, H.P. 2000, ApJ 535, 1047.
  • (4) Aschwanden, M.J., and Parnell, C.E. 2002, ApJ 572, 1048.
  • (5) Aschwanden, M.J. and Aschwanden, P.D. 2008a, ApJ 674, 530.
  • (6) Aschwanden, M.J. and Aschwanden, P.D. 2008b, ApJ 674, 544.
  • (7) Aschwanden, M.J. and Tsiklauri, D. 2009, ApJSS 185, 171.
  • (8) Aschwanden, M.J. and Boerner, P. 2011, ApJ 732, 81.
  • (9) Aschwanden, M.J, 2012, A&A 539, A2..
  • (10) Aschwanden, M.J. and Shimizu, T. 2013, ApJ 776, 132..
  • (11) Aschwanden, M.J., Boerner, P., Schrijver, C.J., and Malanushenko, A. 2013, Solar Phys. 283, 5.
  • (12) Aschwanden, M.J,, Xu, Y., and Jing, J. 2014a, ApJ, 797, 50.
  • (13) Aschwanden, M.J., Crosby, N., Dimitropoulou, M., Georgoulis, M.K., Hergarten, S., McAteer, J., Milovanov, A., Mineshige, S., Morales, L., Nishizuka, N., Pruessner, G., Sanchez, R., Sharma, S., Strugarek, A., and Uritsky, V., 2014b, Space Science Reviews, DOI 10.1007/s11214-014-0054-6.
  • (14) Aschwanden, M.J., Boerner, P., Testa, P., Cheung, M., Warren, H.P., McTiernan, J.M., Caspi, A., and Ryan, D. 2015, (to be submitted).
  • (15) Bak, P., Tang, C., and Wiesenfeld, K. 1987, PhRvL 59/4, 381.
  • (16) Bevington, P.R. and Robinson, D.K. 1992, Data reduction and error analysis for the physical sciences. McGraw Hill: Boston.
  • (17) Boerner,P., Edwards, C., Lemen, J., Rausch, A., Schrijver, C., Shine, R., Shing, L., Stern, R., Tarbell, T., Title, A., Wolfson, C.J., Soufli, R., Spiller, E., Gullikson, E., McKenzie, D., Windt, D., Golub, L., Podgorski, W., Testa, P., and Weber, M. 2012, Solar Phys. 275, 41.
  • (18) Carmichael, H. 1964, in ”The Physics of Solar Flares”, Proc. AAS-NASA Symposium, NASA Special Publ. 50, (ed. W.N.Hess), NASA Science and Technical Information Division, Washington DC.
  • (19) Caspi, A., Krucker, S., and Lin, R.P. 2014, ApJ 781, 43.
  • (20) Craig, I.J.D. and Brown, J.C. 1976, A&A 49, 239.
  • (21) Crosby, N.B., Aschwanden, M.J. and Dennis, B.R. 1993, Solar Phys. 143, 275.
  • (22) DeRosa, M.L., Schrijver, C.J., Barnes, G., Leka, K.D., Lites, B.W., Aschwanden, M.J., Amari, T., Canou, A., et al. 2009, ApJ 696, 1780.
  • (23) Emslie, A.G., Kucharek, H., Dennis, B. R., Gopalswamy, N., Holman, G.D., Share, G.H., Vourlidas, A., Forbes, T.G., Gallagher, P.T., Mason, G.M., Metcalf, T.R., Mewaldt, R.A., Murphy, R.J., Schwartz, R.A., and Zurbuchen, T.H. 2004, JGR (Space Physics), 109, A10, A10104.
  • (24) Emslie, A.G., Dennis, B.R., Holman, G.D., and Hudson, H.S., 2005, JGR (Space Physics), 110, 11103.
  • (25) Emslie, A.G., Dennis, B.R., Shih, A.Y., Chamberlin, P.C., Mewaldt, R.A., Moore, C.S., Share, G.H., Vourlidas, A., and Welsch, B.T. 2012, ApJ 759, 71.
  • (26) Judge, P.G., Hubeny, V., and Brown, J.C. 1997, ApJ 475, 275.
  • (27) Hirayama T. 1974, Solar Phys. 34, 323.
  • (28) Kopp R.A. and Pneuman G.W. 1976, Solar Phys. 50, 85.
  • (29) Krucker, S. and Benz, A.O. 2000, Solar Phys. 191, 341.
  • (30) Lemen, J.R., Title, A.M., Akin, D.J., Boerner, P.F., Chou, C., Drake, J.F., Duncan, D.W., Edwards, C.G., et al. 2012, Solar Phys. 275, 17.
  • (31) O’Dwyer, B., DelZanna, G., Mason, H.E., Weber, M.A., and Tripathi,D. 2010, A&A 521, A21.
  • (32) Pallavicini, R., Serio, S., and Vaiana, G.S. 1977, ApJ 216, 108.
  • (33) Parnell, C.E. and Jupp, P.E. 2000, ApJ 529, 554.
  • (34) Pesnell, W.D., Thompson, B.J., and Chamberlin, P.C. 2012, Solar Phys. 275, 3.
  • (35) Rosner, R., Tucker, W.H., and Vaiana, G.S. 1978, ApJ 220, 643.
  • (36) Ryan, D.F., O’Flannagain, A.M., Aschwanden, M.J., and Gallagher, P.T. 2014, Solar Phys. 289, 2547.
  • (37) Schrijver, C.J., Beer, J., Baltensperger, U., Cliver, E.W., Guedel, M., Hudson, H.S., McCracken, K.G., Osten, R.A., Peter, T., Soderblom, D.R., Usoskin, I.G., and Wolff, E.W. 2012, JGR (Space Physics), 117, 8103.
  • (38) Shimizu, T. 1997, PhD Thesis, University of Tokyo.
  • (39) Shimojo, M. and Shibata, K. 2000, ApJ 542, 1100.
  • (40) Sturrock P.A. 1966, Nature 5050, 695.
  • (41) Testa, P., De Pontieu, B., Martinez-Syjkora, J., Hansteen, V., and Carlsson, M. 2012, ApJ 758, 54.
# Flare GOES Helio- Length Peak EM-weighted Electron Emission Thermal
start time class graphic scale temperature temperature density measure energy
position
(Mm) (MK) (MK) (cm (cm erg)
12 20110215 0144 X2.2 S21W12 28.4 15.9 27.9 10.8 49.9 82.2
37 20110309 2313 X1.5 N10W11 34.8 5.6 22.5 10.6 49.7 84.7
61 20110809 0748 X6.9 N14W69 28.9 15.9 28.4 10.9 50.2 128.9
66 20110906 2212 X2.1 N16W15 24.5 15.9 25.4 10.8 49.7 52.2
67 20110907 2232 X1.8 N16W30 37.4 28.2 28.9 10.6 50.0 140.6
107 20111103 2016 X1.9 N21E64 26.2 25.1 33.2 10.8 49.8 76.4
132 20120127 1737 X1.7 N33W85 46.0 6.3 14.8 10.4 49.8 107.3
136 20120305 0230 X1.1 N19E58 29.7 14.1 33.9 10.7 49.8 92.9
147 20120307 0002 X5.4 N18E31 44.9 14.1 21.8 10.6 50.3 208.4
148 20120307 0105 X1.3 N18E29 36.0 4.0 22.7 10.5 49.7 89.8
209 20120706 2301 X1.1 S13W59 20.4 5.6 28.5 10.8 49.5 33.2
220 20120712 1537 X1.4 S15W03 36.3 6.3 24.2 10.6 49.8 105.3
248 20121023 0313 X1.8 S13E58 10.4 15.9 34.1 11.1 49.4 11.5
286 20130513 1548 X2.8 N08E89 23.6 17.8 33.3 10.9 49.9 70.9
287 20130514 0000 X3.2 N08E77 29.9 15.9 28.5 10.8 50.1 109.5
288 20130515 0125 X1.2 N10E68 22.6 5.6 27.1 10.7 49.5 40.8
318 20131025 0753 X1.7 S08E73 11.4 28.2 29.1 11.1 49.3 10.9
320 20131025 1451 X2.1 S06E69 17.0 4.0 30.5 10.9 49.4 24.6
330 20131028 0141 X1.0 N05W72 15.9 15.9 32.0 10.9 49.5 23.3
337 20131029 2142 X2.3 N05W87 23.9 22.4 30.3 10.8 49.8 53.7
344 20131105 2207 X3.3 S08E44 12.0 25.1 32.8 11.1 49.4 14.7
349 20131108 0420 X1.1 S11E11 20.8 25.1 30.2 10.9 49.8 43.0
351 20131110 0508 X1.1 S13W13 22.0 17.8 33.3 10.9 49.8 54.5
358 20131119 1014 X1.0 S13W69 18.3 20.0 30.7 10.9 49.6 31.4
384 20140107 1804 X1.2 S12E08 3.0 1.8 25.1 11.4 48.2 0.4
Table 1: Thermal energy parameters of 28 X-class flare events.
# Flare GOES Helio- Length Peak EM-weighted Electron Emission Thermal
start time class graphic scale temperature temperature density measure energy
position
(Mm) (MK) (MK) (cm (cm erg)
1 20100612 0030 M2.0 N23W47 13.2 6.3 18.6 10.8 48.9 7.0
2 20100613 0530 M1.0 S24W82 12.2 7.1 15.8 10.7 48.6 4.1
3 20100807 1755 M1.0 N13E34 25.1 4.0 6.2 10.4 49.1 8.2
4 20101016 1907 M2.9 S18W26 15.1 14.1 29.9 10.9 49.4 19.2
5 20101104 2330 M1.6 S20E85 13.8 10.0 24.9 10.8 49.0 10.2
6 20101105 1243 M1.0 S20E75 13.3 6.3 19.8 10.8 48.9 7.7
7 20101106 1527 M5.4 S20E58 20.3 4.0 20.9 10.7 49.4 24.6
9 20110209 0123 M1.9 N16W70 8.2 3.2 28.5 11.0 48.7 3.4
10 20110213 1728 M6.6 S21E04 15.9 14.1 23.9 10.9 49.5 20.8
Table 2: Thermal energy parameters of 391 M and X-class flare events. The full list is available from a machine-readable file, from which only the first 10 entries are listed here.
Instrument Number Spatial Electron Electron Emission Thermal
of events scale temperature density measure energy
[Mm] [MK] [cm] [cm] [erg]
Skylab/S-054 31
RHESSI 32
AIA/SDO 155
AIA/SDO 391
AIA/SDO 391
Table 3: Parameter ranges of physical parameters determined from 4 different datasets of large flares: Pallavicini et al. (1977); Emslie et al. (2012); Aschwanden and Shimizu (2013); This study: Isothermal energy; This study: Multi-thermal energy.
Figure 1: The spatial synthesis DEM method is visualized by single-Gaussian DEM fits in a grid ,