Table 1
Best-fit parameters obtained with XSPEC of spectra during each time interval.
| Global (a) | Quiescent phases (b) | ||||
|---|---|---|---|---|---|
| Interval | 1 | 4 | 7 | ||
| nH (1020 cm−2) | 0.23 (<0.80) | 0.23 – | 0.23 – | 0.23 (1.0–2.0) | |
| T1 (106 K) | 5.3 ( 5.0–5.9) | 6.5 – | 6.5 – | 6.5 (5.5–7.9) | |
| T2 (106 K) | 10.9 (10.6–11.3) | 11.4 – | 11.4 – | 11.4 (10.6–13.6) | |
| T3 (106 K) | 25.6 (24.4–26.9) | 23.0 – | 23.0 – | 23.0 (21.1–31.7) | |
| Z /Z⊙(c) | 0.30 (0.26-0.33) | 0.22 – | 0.22 – | 0.22 (0.19–0.26) | |
| log EM1 | 52.63 (52.56–52.70) | 52.81 (52.72–52.87) | 52.89 (52.81–52.95) | 52.77 (52.62–53.00) | |
| log EM2 | 52.97 (52.92–53.04) | 53.03 (52.95–53.09) | 52.87 (52.74–52.97) | 53.09 (53.02–53.19) | |
| log EM3 | 53.22 (53.20–53.25) | 52.94 (52.87–53.01) | 53.16 (53.11–53.21) | 53.13 (52.88–53.19) | |
| log LX(d) | 30.58 (30.57–30.59) | 30.46 (30.45–30.47) | 30.52 (30.51–30.53) | 30.55 (30.54–30.56) | |
| χ2 | 1438 | 48.4 | 67.8 | 98.2 | |
| D.o.F. | 1131 | 53 | 51 | 103 | |
| First flare (e) | Second flare (e) | ||||
| Interval | 2 | 3 | 5 | 6 | |
| T4 (106 K) | 111 (86–162) | 39 (32–47) | 63 (44–98) | 53 (32–99) | |
| log EM4 | 53.35 (53.32–53.37) | 53.12 (53.09–53.15) | 53.04 (52.99–53.10) | 52.58 (52.49–52.67) | |
| log LX,Tot (erg/s) | 30.87 (30.86–30.88) | 30.71 (30.70–30.72) | 30.75 (30.74–30.76) | 30.64 (30.63–30.65) | |
| Lx,flare (erg/s) (f) | 6.9 × | 1030 | 3.4 × | 1030 | |
| χ2 | 74.7 | 103.1 | 74.5 | 99.6 | |
| D.o.F. | 68 | 65 | 52 | 65 | |
Notes. (a)Best fit of all EPIC and RGS spectra obtained with 3T VAPEC components. (b)Best fits of the summed MOS+pn spectra in the quiescent phases were obtained with 3T VAPEC models, where nH and element abundance ratios with respect to iron were fixed at the values of the “Global” best fit. For intervals 1 and 4, we also fixed the temperatures and the iron abundance found in phase 7, and varied only the emission measures of the three thermal components. (c)Best-fit value of the iron abundance, linked to the abundances of Al, Ar, and Ni. Abundances of other elements, treated as free parameters, are reported in Sect. 3. (d)Unabsorbed total luminosity for the quiescent phases are given in the band 0.3–10.0 keV. (e)For the flares in phases 2–3 and 5–6 we used a 4T model with three components fixed at the best-fit values found in the pre-flare phases 1 and 4, respectively. (f)The total flare luminosity in phases 2–3 and 5–6 computed as the total luminosity minus the luminosity of the pre-flare phases 1 and 4, respectively.
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