Patterns of variability in Be/X-ray pulsars during giant outbursts

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Table 4

Pearson’s correlation coefficients for the various samples.

Source name	L_X − Γ	Γ − E_cut	L_X − I_Fe	L_X − ν₁	Γ − ν₁
	HB/DB	HB/DB	all	all	HB/DB	spectra	power spectra

4U 0115+63	–0.96/0.94	0.89/–0.49^f	0.98	0.85	–0.80^f/0.46^f	1.5 ± 0.4	1.4 ± 0.3
EXO 2030+375	–0.85/0.89	0.80/0.98	0.96	0.88	–0.82/0.37^f	1.1 ± 0.1	2.0 ± 0.8
V 0332+53	–0.97/–0.52	–/0.86	0.95	0.83	0.63^f/–0.48	1.6 ± 0.5	1.3 ± 0.4
KS 1947+300	–0.80/0.97	0.67/0.97	0.90	0.95	–0.48^f/0.77	1.1 ± 0.4	1.8 ± 0.7
1A 0535+262	–0.90/–	0.05^g/–	0.98	0.92	–0.91/–	0.7 ± 0.2	1.3 ± 0.3
1A 1118–616	–0.96/–	0.88/–	0.99	0.96	–0.86/–	1.2 ± 0.2	1.2 ± 0.3
Swift J1626.6–5156	–0.95^a/–	0.93^b/–	0.94	0.45^d	0.02^g/–	0.9 ± 0.2	1.6 ± 0.6
XTE J0658–073	–0.89^e/–	0.88^b/–	0.99	0.96^e	–0.85^e/–	1.1 ± 0.3	1.9 ± 0.8
GRO J1008–57	–0.84/–	0.94^c/–	0.96	0.80	–0.29^g/–	0.8 ± 0.2	1.3 ± 0.3

Notes. All correlations are significant at > 99%, unless stated otherwise. The L_X − ν₁ and L_X − I_Fe relationships were fitted with a power law function (linear correlation in log −log scale). A “–” indicates that no data points exist. Also shown (Cols. 7 and 8) is the mean and standard deviation of the reduced χ² of the fits. In 4U 0115+63, quoted value corresponds to the POWER × HIGHECUT model. Using the “bump” model the reduces to 1.0 ± 0.2 for this source.

^(a)

For L_X/L_Edd > 0.05;

^(b)

for L_X/L_Edd > 0.1;

^(c)

for L_X/L_Edd > 0.01;

^(d)

For L_X/L_Edd < 0.2;

^(e)

for L_X/L_Edd < 0.1;

^(f)

95% confidence level;

^(g)

<80% confidence level.

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