Table 3.
Spectral results.
| Model | NH | Γ | PL normalization |
 |
χ(a) | ξ(a) | Teff | Rem |  /d.o.f. |
nhp |
|---|---|---|---|---|---|---|---|---|---|---|
| (1021 cm−2) | (10−6 pho cm−2 s−1 keV−1) | (1012 G) | (°) | (°) | (MK) | (km) | ||||
| Phase averaged | ||||||||||
| PL+BB |
 |
1.2 ± 0.2 |
 |
... | ... | ... | 3.1 ± 0.2 |
 |
0.80/32 | 0.78 |
| PL+NSMAXG (b) | 9 ± 1 | 1.1 ± 0.3 |
 |
4 | ... | ... | 1.1 ± 0.1 |
 |
0.86/32 | 0.69 |
| PL+NSMAXG (c) | 9 ± 1 |
 |
 |
2 | η = 0° |
 |
 |
0.84/32 | 0.72 | |
| PL+NSMAXG (c) | 9 ± 1 |
 |
 |
2 | η = 90° |
 |
 |
0.86/32 | 0.69 | |
| PL+NSMAXG (c) | 10.7 ± 0.4 | 1.3 ± 0.2 |
 |
2 | η = 90° | 0.88 ± 0.01 | 13 (a) | 0.76/33 | 0.64 | |
| PL+ATMO north (d) | 8.4 ± 0.4 | 1.0 ± 0.2 |
 |
4 | 90 | 25 | 1 (a) | 5.1 ± 0.2 | 0.96/33 | 0.53 |
| PL+ATMO south (d) | 8.5 ± 0.4 | 1.0 ± 0.2 |
 |
4 | 90 | 25 | 1 (a) | 5.6 ± 0.2 | 0.96/33 | 0.53 |
| Phase resolved | ||||||||||
| PL+ATMO north (d) | 8.3 ± 0.4 | 1.0 ± 0.3 |
 |
4 | 90 | 25 | 1 (a) | 5.1 ± 0.2 | 1.05/44 | 0.38 |
| PL+ATMO south (d) | 8.3 ± 0.4 | 1.1 ± 0.3 |
 |
4 | 90 | 25 | 1 (a) | 5.5 ± 0.2 | 0.94/44 | 0.59 |
| Unpulsed/pulsed | ||||||||||
| PL+BB | 6 ± 1 | 0.92 ± 0.26 |
 /< 0.4 |
… | … | … | 3.6 ± 0.3 |
 |
1.61/7 | 0.13 |
| PL+ATMO north (d) | 8.7 ± 0.6 | 1.0 ± 0.2 |
 /< 0.4 |
4 | 90 | 20 | 1 (a) | 5.5 ± 0.3 | 1.03/9 | 0.41 |
| PL+ATMO south (d) | 8.8 ± 0.6 | 1.1 ± 0.2 |
 /< 0.5 |
4 | 90 | 20 | 1 (a) | 5.7 ± 0.3 | 1.11/9 | 0.35 |
Notes. Temperatures and radii are at the star surface; M = 1.36 M⊙, R = 13 km, d = 1.5 kpc. Errors at 1σ.
NSMAXG model (Ho et al. 2008, 2014) with constant magnetic field and surface temperature.
NSMAXG model with a dipole distribution of the magnetic field and consistent temperature distribution.
Our model of a magnetized atmosphere described in Sect. 2 with a dipole distribution of the magnetic field and consistent temperature distribution, with only either the northern or the southern hemispheres active.
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