Masuda's discovery of a compact hard X-ray impulsive source at the apex of a flaring coronal loop has received a great deal of recent attention in the solar physics community. The Masuda flare, which occurred on 1992 January 13, exhibited evidence of energy deposition in a compact region some distance above the soft X-ray loop, suggesting, to some authors, a flare process similar to the classical model for two-ribbon flares proposed by Shibala et al. These conclusions were made on the basis of a maximum entropy method (MEM) reconstruction of the Yohkoh Hard X-Ray Telescope (HXT) observations. Recently, a new approach has been developed for reconstructing the spatial information from the HXT: that of pixon reconstruction, proposed by Metcalf et al. In this paper, we apply the pixon reconstruction technique to the event of 1992 January 13 and determine the temporal and spectral characteristics of the loop-top source. While our emphasis here is on the spectral properties of the Masuda flare, we also provide a brief comparison between the pixon reconstruction and that of MEM for the hard X-ray loop top. In carrying out the comparison between the methods, we have applied recent improvements to the instrument response functions and reconstruction algorithms. We have also identified a previously unknown effect of weak source suppression that was inherent in previous analyses and that significantly compromised the ability to study weak sources of hard X-ray emission in the presence of strong sources. The improved response functions and the better flux estimation used in this paper reduce (but do not eliminate) the effects of this suppression, and consequently, it should be noted that the MEM analysis presented in this paper is quite distinct from any that have been carried out previously. Our conclusions are that (a) a compact loop-top hard X-ray source exists with an impulsive temporal profile spanning the peak: of the flare; (b) the loop-top source is nonthermal in nature at the peak of the Bare; (c) there is a distinct dearth of HXT LO channel emission, relative to the higher energy channels, from the loop-top region, indicating either a very hard spectrum or the presence of a low-energy cutoff in the energetic electron spectrum; (d) the footpoint and loop-top emission during the impulsive phase of the flare are produced by two distinct particle populations; (e) following the main phase of this flare, the loop top is clearly thermal in nature with a peak temperature of similar to 40 MK that decreases with time as the event proceeds; and (f) the disparity between the present pixon results and previous MEM results is primarily due to the intrinsically better photometry achieved by the pixon method and the avoidance of suppression effects in the present analysis. These conclusions therefore support, in part, those made in previous works, confirming the existence of an impulsive source of hard X-rays In the corona above a Baring loop. Our analysis does, however, allow for a more comprehensive understanding of the temporal and spectral development of this event In the context of an alternative reconstruction technique.
