Table 2.
Results of the NSCOOL model fits to the observed 
evolution in MXB 1659 − 29 after outbursts I and II.
| Model |
 |
Qsh, I | Qsh, II | ρsh, I | ρsh, II | log(ylight, I) | log(ylight, II) | Qimp, 1(a) | Qimp, 2(a) | Qimp, 3(a) | χ2 (d.o.f. (b)) |
|---|---|---|---|---|---|---|---|---|---|---|---|
| (×107 K) | (MeV | (MeV | (×108 | (×108 | (g cm−2) | (g cm−2) | |||||
| nucleon−1) | nucleon−1) | g cm−3) | g cm−3) | ||||||||
| A | 3.1 |
1.2±0.8 | 1.2 |
4.3 |
10.1 |
8.5 |
7.8 |
2.7 |
2.1 |
1.8 |
2.7 (3) |
| B | 3.2 |
1.2±0.7 | 1.0±0.8 | 5.1 |
3.8 |
8.4 |
8.4 |
2.3 |
2.1 |
1.6 |
2.9 (4) |
| C | 3.1 |
1.1±0.8 | 1.1±0.8 | 3.5 |
3.5 |
8.6 |
7.8 |
5.9 |
1.7 |
1.9 |
2.6 (5) |
Notes. The errors are stated for the 90% confidence level. The * indicates that the error is not constrained and corresponds to the maximum or minimum allowed value for the given parameter. The lowest allowed limit for ρsh is ρ = 108 g cm−3 which corresponds to the boundary of the outer crust with the envelope. The highest and lowest allowed ylight in our model is, respectively, log(ylight) = 12 g cm−2 and 5 g cm−2. The lowest allowed Qimp = 0.
The Qimp parameters have been indicated as Qimp, n where n = the layer of the crust (from the outer crust to the inner crust, n = 1, 2, 3). The outer and inner boundaries of the crust are defined by ρ = 108 g cm−3 and ρ = 1.5 × 1014 g cm−3, respectively. The three layers of the crust for which the different Qimp have been modelled are defined by boundaries set at ρ = 6.2 × 1011 g cm−3 and ρ = 8 × 1013 g cm−3, respectively. Thus, the three layers define the outer crust, the neutron drip layer, and the inner crust where the nuclear pasta is expected to occur.
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