Long tails on thermonuclear X-ray bursts from neutron stars: a signature of inward heating?

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Table 2:

Summary of measurements.
Burst source	Mean burst duration (s)^a			Tail/prompt ratio		Ref.^b
	time scale^c	$\tau_2^d$	tail^e	in time^f	in fluence^g
Sources discussed here
GS 1826-24	$39.4\pm0.2$	44.6	$1252\pm25$	32/28	0.03 (300 s)
			(600-5500 s)
			$\chi^2/\nu$ = 16.9/15
4U 1728-34	$5.85\pm0.02$	12.6	$313\pm17$	53/25	0.09 (100 s)
			(200-800 s)
			$\chi^2/\nu$ = 13.4/11
EXO 0748-676	$13.7\pm0.1$	36.3	$300\pm42^h$	22/8	0.01 (300 s)
			(400-1200 s)
			$\chi^2/\nu$ = 141/44
Literature cases
GX 3+1	$3\pm1$	6	1110 $\pm$ 170	370/185	40 (10 s)	1
M 28		7.5	800-3250	$\sim$ 100	>1.4ⁱ (90 s)	2
Aql X-1	18.4		$627\pm100$	34		3
OSO-8 long burst	44.8		215.7	5	0.01 (150 s)	4

^a Averaged over the bursts cataloged by Galloway et al. (2008); ^b references: 1 - Chenevez et al. (2006); 2 - Gotthelf & Kulkarni (1997); 3 - Czerny et al. (1987); 4 - Swank et al. (1977); ^c the time scale is defined as the burst fluence divided by the peak flux; ^d $\tau_2$ is the e-folding decay time of the final part of the prompt burst; ^e the time range in parentheses refers to the interval in which the fit was carried out; ^f the two numbers refer to division by the mean time scale and $\tau_2$ , respectively; ^g fluences for GS 1826-24 and 4U 1728-34 were determined from data averaged over multiple bursts; that for EXO 0748-676 from the RXTE triple burst. The time between parentheses refers to the interval for the prompt emission; ^h this value applies to the triple burst only and excluding times for the second burst; ⁱ based on counts of 0.8-12 keV photons in ASCA-GIS (Table 1 in Gotthelf & Kulkarni 1997).

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