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	Figure 1: The soft X-ray flux from the low energy channel (1-8 Å) from GOES 9 showing (enumerated) flares observed near the time of radio spike burst emission observed on 1997 November 14. This shows the overall context of the series of overlapping flares, Flares 0-4, possibly related, directly or indirectly to the radio spike bursts.
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In the text

	Figure 2: The soft-ray flux for the low energy channel (1-8 Å - the higher flux curve) and the high energy channel (0.5-4 Å - the lower flux curve) from GOES 9 showing the times of SXT full-frame images (FFIs) and partial-frame images (PFIs); EIT 195 and 304 Å images; and LASCO C1, C2, and C3 images. Also shown are the time intervals of the enumerated flares and Yohkoh satellite night.
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In the text

Figure 3: An AIP spectrogram showing radio emission associated with Flare 1 in the form of the time derivative of the spectrum (to enhance faint features). There was a group of type III bursts between 80 and 40 MHz (09:07.30-09:14 UT). The first decimetric features occurred between 200 and >400 MHz as faint positively and negatively drifting features at about 09:10 UT, and as broadband pulsations after 09:22 UT. There was ongoing NS activity, enhanced with the pulsations, between 100 and 170 MHz.

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In the text

	Figure 4: An AIP spectrogram showing radio emission associated with Flares 2 and 3. The dominant feature is a group of intense type III bursts around 09:42 UT. In this paper we focus on the three continuum enhancements with embedded spike bursts between 200-800 MHz from 09:37-09:39 UT. Spuriously repeated spikes occurred later, too. There were ongoing NS features between 100-170 MHz.
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In the text

	Figure 5: An AIP spectrogram, enlarged from Fig. 4, showing the spike clouds superposed on continuum emission. The radio emission in this range, 332-400 MHz, was averaged to obtain the radio flux plot shown in Fig. 7.
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In the text

	Figure 6: An AIP spectrogram showing a slowly-drifting radio continuum burst associated with Flare 4.
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In the text

	Figure 7: Hard X-ray fluxes as observed by the HXT L channel (14-23 keV) and BATSE DISCLA channel 1 (25-50 keV) and channel 2 (50-100 keV) for the radio spike burst-associated flare, Flare 2. Also shown in the top panel is the frequency-integrated AIP radio flux for the spike bursts associated with Flare 2.
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In the text

	Figure 8: Portions of corrected SXT partial-frame images (PFIs) showing an overview of the development of the sequence of flares on 1997 November 14. The images have been scaled to show the brightest features in each image (i.e., relative differences between images are not retained). Note Flare 3 was not observed by SXT but SOHO EIT data show it originated from the same region as Flare 2.
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In the text

	Figure 9: Portions of corrected SXT partial-frame images (PFIs) showing faint soft X-ray emitting features which appear to be in the form of ejecting and expanding loops associated with Flare 1.
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In the text

Figure 10: Portions of SXT full-frame images (FFIs). Rows 1 and 3 show corrected raw data, while rows 2 and 4 show difference images. For the lower portion of row 4, we superposed difference images truncated over a narrower data number (DN) difference range (absolute value 20 as opposed to 400). The images show the expanding and ejecting soft X-ray loops and the compression of soft X-ray emitting magnetic field structures.

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In the text

Figure 11: Portions of running difference EIT images showing large-scale compression of magnetic field structures (indicated by arrows). Dimming of the EIT images in the vicinity of the soft X-ray ejection region seen in Fig. 9 is also apparent. Also show on two of the panels are the 60% and 90% contour levels for the NRH 327.0 MHz source (dashed lines) and 410.5 MHz source (solid lines) of the radio spike burst at 09:38:30 UT.

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In the text

Figure 12: The left-hand panel shows a difference image from Fig. 11 with superposed white + marks indicating points clicked along the arcs, interpolated points between them (black x [which are not resolved in the figure and appear as thick black lines]), and the subset of shortest distance line segments (white lines) used to estimate the speed between arcs. The right-hand panel shows the mean of the speeds between successive arcs estimated from the line segments, with the error bars indicating the standard deviation of the values. The overall average speed is indicated by the dotted line.

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In the text

Figure 13: An SXT PFI taken at 09:37:00 UT showing the bright arcade of Flare 1 and the small flaring structures of Flare 2, superposed on a portion of an FFI taken at 09:32:32 UT (with saturated portions covered with an FFI taken at 09:39:10 UT). Shown in black contours are the HXT L channel (14-23 keV) sources constructed by accumulating counts over the interval 09:36:45-09:38:50 UT. The dashed white contours show the 60% and 90% contour levels for the NRH 327.0 MHz source of the radio spike burst at 09:38:30 UT. Similarly the solid white contours show the NRH 410.5 MHz source of the radio spike burst at 09:38:30 UT.

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In the text

Figure 14: The graph at the top shows the GOES soft X-ray fluxes for the decay phase of Flare 4, identifying and enumerating subsidiary flare-like brightenings, which we refer to as soft X-ray blips. The bottom part of the figure shows SXT images of some of the soft X-ray blips. In each image we replaced the ordinate label with a label identifying the enumerated soft X-ray blip (as given in the graph).

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In the text