Restless quiescence: thermonuclear flashes between transient X-ray outbursts

E. Kuulkers; J. J. M. in 't Zand; J.-P. Lasota

doi:10.1051/0004-6361/200810981

Home

All issues

Volume 503 / No 3 (September I 2009)

A&A, 503 3 (2009) 889-897

Full HTML

Free Access

Table 1:

Overview of the properties¹ of the observed flashes discussed in this paper.
Source	$F_{\rm bb,peak}$ (10^-8		$F_{\rm pers}$		$F_{\rm pers,bol}/F_{\rm bb,peak}$	$L_{\rm x,bol}$ (10³⁶	$\Delta t_{\rm last}$		$\Delta t_{\rm next}$
	erg cm^-2 s^-1)		(10^-10 erg cm^-2 s^-1)		$\equiv$ $L_{\rm x,bol}/L_{\rm Edd}$	erg s^-1)	(days)		(days)
Cen X-4	$\sim$ 120	[1]	<20^a (2-10 keV)	[1]	$\lesssim$ 0.0033	$\lesssim$ 0.7	>40	[1,2]	$\simeq$ 2	[1,3]
2S 1711-339	$3.0 \pm 1.0^b$	[4]	<0.7 (2-28 keV)	[4]	$\lesssim$ 0.0047	$\lesssim$ 1	$\sim$ 340	[4]	$\simeq$ 1440	[5]
GRS 1747-312	$\simeq$ 2.5^c	[6]	<0.6 (0.1-200 keV)	[6]	$\lesssim$ 0.0024	$\lesssim$ 0.5	$\simeq$ 26	[6]	$\simeq$ 28	[6]
IGR J17473-2721	$\simeq$ 11^d	[7]	<1.7 (2-10 keV)	[8]	$\lesssim$ 0.0031	$\lesssim$ 0.4	$\sim$ 960	[9,10]	$\simeq$ 2	[8,11]
2S 1803-245	$3.1 \pm 0.7$	[12]	<2^e (2-28 keV)	[4]	$\lesssim$ 0.013	$\lesssim$ 3	$\sim$ 7990	[13]	$\simeq$ 7	[12]
SAX J1808.4-3658	$25 \pm 2^c$	[14]	<3 (2-28 keV)	[14]	$\lesssim$ 0.0024	$\lesssim$ 0.5	$\simeq$ 17	[14]	$\simeq$ 543	[15]

^a Vela 5B 56 h upper limit; ^b highest peak flux among the flash sample in [4]; ^c photospheric radius-expansion flash; ^d peak flux observed during another flash reported by [7]; ^e no limits are quoted in [12]; we, therefore, assume the highest BeppoSAX/WFC flux upper limit from [4].
Note 1. In the first two columns we give the observed flash bolometric peak fluxes ( $F_{\rm bb,peak}$ ) and the 3 $\sigma$ upper limits on the flux around the flashes ( $F_{\rm pers}$ ). From these we infer the flash peak luminosities in terms of the Eddington luminosity ( $L_{\rm Edd}$ ), assuming $L_{\rm x,bol}/L_{\rm Edd} \equiv F_{\rm pers,bol}/F_{\rm bb,peak}$ (see Sect. 3), where $F_{\rm pers,bol}$ and $L_{\rm x,bol}$ are the bolometric pre-flash source flux and luminosity, respectively. Assuming $L_{\rm Edd} = 2 \times 10^{38}$ erg s (see Sect. 2) we derive an upper limit on $L_{\rm x,bol}$ . In the last two columns we provide the time since the last and to the next detected X-ray outburst with respect to the time of the flash, $\Delta t_{\rm last}$ and $\Delta t_{\rm next}$ , respectively. References are given in brackets: [1] this paper; [2] Conner et al. (1969); [3] Belian et al. (1972); [4] Cornelisse et al. (2002a); [5] Markwardt & Swank (2004); [6] in 't Zand et al. (2003b); [7] Altamirano et al. (2008); [8] Markwardt et al. (2008); [9] Grebenev et al. (2005); [10] Markwardt & Swank (2005); [11] Del Monte et al. (2008); [12] Cornelisse et al. (2007); [13] Jernigan (1976); [14] in 't Zand et al. (2001); [15] Marshall (1998).

Source LaTeX | All tables | In the text

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.