Fig. 1. Relationships between mass and radius of neutron stars in NL3, GM1 and TMA model.在NL3, GM1和TMA模型下中子星的质量和半径的关系
Fig. 2. Relationship of moment of inertial I to mass M and radius R for magnetars in TMA models.
在TMA模型中磁星的转动惯量I随质量m和半径R的关系
Fig. 3. Normalized magnetic field components of the crustal confined for the force-free field:
(red line),
(blue line), and
(yellow line) vs. normalized radial coordinate x. Here we assume the parameter μ = 1.676, corresponding to M = 1.45M⊙, R = 11.77 km and I = 1.45 × 1045 g·cm2 in the TMA model.
在无力磁场结构位型下壳层归一化磁场分量
(红线),
(蓝线), 及
(黄线)与归一化径向坐标x的关系(选取μ = 1.676, 对应在TMA模型下的M = 1.45M⊙, R = 11.77 km及I = 1.45 × 1045 g·cm2)
Fig. 4. Relationship of σ to ρ, Τ and Q in the inner crust for magnetar: (a) The conductivity due to electron-phonon scattering; (b) the conductivity due to electron-impurity scattering. The EOS of BBP model is used.
磁星壳层电导率随密度、温度及不纯净度参数的变化 (a)电导率由电子-声子散射主导; (b)电导率由电子-杂质散射主导; 物态方程一律采用BBP 模型
Fig. 5. Numerical fitting of Ohmic decay for magnetars: (a) The poloidal magnetic field, Bp, as a function of t at x = 1; (b) the toroidal magnetic field, Bt, as a function of t when at x = 1; (c) the poloidal magnetic field decay rate, dBp/dt, as a function of t when at x = 1; (d) the toroidal field decay rate, dBt/dt, as a function of t when at x = 1; (e) the poloidal field energy decay rate, Lp, as a function of t; (f) the toroidal filed energy decay rate, Lt, as a function of t. The red and blue lines in (a)−(f) indicate
and
, respectively.
磁星磁场欧姆衰变的数值模拟 (a) 在x = 1处极向磁场Bp随时间t的变化; (b) 在x = 1处极向磁场Bt随时间t的变化; (c) 在x = 1处极向磁场衰减率dBp/dt, 随时间t的变化; (d) 在x = 1处环向磁场衰减率dBt/dt, 随时间t的变化; (e) 极化磁场的能量衰减率Lp随时间t的变化; (e) 环向磁场的能量衰减率Lt随时间t的变化; 在(a)−(f)图中红色和蓝颜色的线分别表示
和
Fig. 6. The
-
plot for our magnetars and selected objects in isotropic heating models.
在各向同性加热模型下磁星及相关致密天体
-
的关系图
Fig. 7. Fitting relationship between the soft X-ray luminosity and rotational energy loss rate of magnetars in the isotropic heating model.在各向同性加热模型下拟合得到的磁星的旋转能损率与软X射线光度的关系
| RMF模型 | ${\rho _0}$![]() ![]() /fm–3 | ${E_0}$![]() ![]() /MeV
| ${K_0}$![]() ![]() /MeV
| m*
| K′/MeV
| J/MeV
| ${L_0}$![]() ![]() /MeV
| $K_{{\rm{sym}}}^0$![]() ![]() /MeV
| $Q_{{\rm{sym}}}^0$![]() ![]() /MeV
| $K_{\tau ,V}^0$![]() ![]() /MeV
| | NL3 | 0.148 | –16.24 | 271.53 | 0.60 | –202.91 | 37.40 | 118.53 | 100.88 | 181.31 | –698.85 | | TMA | 0.147 | –16.33 | 318.15 | 0.635 | 572.12 | 30.66 | 90.14 | 10.75 | –108.74 | –367.99 | | GM1 | 0.153 | –16.02 | 300.50 | 0.70 | 215.66 | 32.52 | 94.02 | 17.98 | 25.01 | –478.64 |
|
Table 1. Saturation properties of nuclear matter in the parameterizations for NL3, GM1 and TMA models.
在NL3, GM1和TMA模型下饱和核物质特性.
| m/M⊙ | R/km
| Rcore/R | $\mu $![]() ![]() | I/g·cm2 | | 注: *在TMA模型下由物态方程给出的最大中子星质量. | | 1.20 | 11.42 | 0.915 | 1.678 | 1.03(1) × 1045 | | 1.45 | 11.77 | 0.917 | 1.676 | 1.47(2) × 1045 | | 1.72 | 12.05 | 0.919 | 1.675 | 1.87(2) × 1045 | | 2.03* | 11.25 | 0.914 | 1.679 | 2.09(2) × 1045 |
|
Table 2. Partial values of m, R, Rcore/R, μ and I for magnetars in TMA model.
在TMA模型中磁星的m, R, Rcore/R, μ和I的部分值
| T = 1 × 108 K
| | T = 2 × 108 K
| | T = 3 × 108 K
| $Q = 1$![]() ![]() | $Q = 5$![]() ![]() | $Q = 10$![]() ![]() | $Q = 1$![]() ![]() | $Q = 5$![]() ![]() | $Q = 10$![]() ![]() | $Q = 1$![]() ![]() | $Q = 5$![]() ![]() | $Q = 10$![]() ![]() | | $\rho $![]() ![]() /g·cm–3 | Z | A | $\sigma $![]() ![]() /1023 s–1 | $\sigma $![]() ![]() /1023 s–1 | $\sigma $![]() ![]() /1023 s–1 | $\sigma $![]() ![]() /1023 s–1 | $\sigma $![]() ![]() /1023 s–1 | $\sigma $![]() ![]() /1023 s–1 | $\sigma $![]() ![]() /1023 s–1 | $\sigma $![]() ![]() /1023 s–1 | $\sigma $![]() ![]() /1023 s–1 | | Bp = 5 × 1014 G
| 4.66 × 1011 | 40 | 127 | 0.455 | 2.15 | 0.752 | | 1.69 | 1.15 | 0.591 | | 0.998 | 0.821 | 0.490 | | 6.61 × 1011 | 40 | 130 | 0.641 | 2.58 | 0.865 | 2.24 | 1.45 | 0.703 | 1.18 | 0.982 | 0.592 | | 8.79 × 1011 | 41 | 134 | 0.928 | 3.22 | 0.991 | 2.97 | 1.54 | 0.822 | 1.31 | 1.20 | 0.702 | | 1.20 × 1012 | 42 | 137 | 1.26 | 3.72 | 1.15 | 3.88 | 2.21 | 0.953 | 2.08 | 1.49 | 0.787 | | 1.47 × 1012 | 42 | 140 | 1.97 | 4.63 | 1.23 | 4.89 | 2.50 | 1.04 | 2.43 | 1.69 | 0.867 | | 2.00 × 1012 | 43 | 144 | 2.62 | 4.78 | 1.42 | 6.31 | 3.10 | 1.22 | 3.18 | 2.11 | 1.03 | | 2.67 × 1012 | 44 | 149 | 2.67 | 5.59 | 1.68 | 7.82 | 3.75 | 1.41 | 4.08 | 2.59 | 1.29 | | 3.51 × 1012 | 45 | 154 | 3.42 | 6.41 | 1.85 | 10.30 | 4.52 | 1.62 | 5.20 | 3.14 | 1.40 | | 4.54 × 1012 | 46 | 161 | 4.20 | 7.26 | 2.08 | 15.60 | 5.24 | 1.89 | 6.53 | 3.78 | 1.65 | | 6.25 × 1012 | 48 | 170 | 5.58 | 8.56 | 2.37 | 17.50 | 6.42 | 2.18 | 8.60 | 4.68 | 1.96 | | 8.38 × 1012 | 49 | 181 | 6.95 | 9.67 | 2.66 | 22.20 | 7.46 | 2.49 | 10.90 | 5.55 | 2.23 | | 1.10 × 1013 | 51 | 193 | 8.58 | 11.40 | 2.99 | 27.90 | 8.75 | 2.81 | 13.70 | 6.60 | 2.55 | | 1.50 × 1013 | 54 | 211 | 10.80 | 12.90 | 3.45 | 35.60 | 10.40 | 3.24 | 17.30 | 7.95 | 2.95 | | 1.99 × 1013 | 57 | 232 | 13.00 | 14.90 | 3.95 | 43.60 | 12.10 | 3.73 | 21.20 | 9.37 | 3.12 | | 2.58 × 1013 | 60 | 257 | 15.20 | 16.90 | 4.46 | 51.20 | 13.80 | 4.22 | 24.90 | 10.80 | 3.88 | | 3.44 × 1013 | 65 | 296 | 17.70 | 19.70 | 5.22 | 59.60 | 16.20 | 4.93 | 28.90 | 12.50 | 4.53 | | 4.68 × 1013 | 72 | 354 | 20.40 | 23.50 | 6.23 | 67.70 | 19.10 | 5.87 | 32.60 | 14.60 | 5.37 | | 5.96 × 1013 | 78 | 421 | 21.70 | 26.50 | 7.08 | 69.00 | 21.10 | 6.63 | 33.80 | 15.90 | 6.02 | | 8.01 × 1013 | 89 | 548 | 22.10 | 31.20 | 8.48 | 69.80 | 23.80 | 7.82 | 34.70 | 17.20 | 6.95 | | 9.83 × 1013 | 100 | 683 | 23.20 | 35.30 | 9.78 | 69.80 | 25.40 | 8.83 | 36.00 | 17.50 | 7.64 | | 1.30 × 1014 | 120 | 990 | 25.50 | 40.30 | 11.80 | 70.80 | 26.50 | 10.10 | 38.20 | 18.10 | 8.20 | | | Bp = 3 × 1015 G
| 4.66 × 1011 | 40 | 127 | 0.463 | 2.21 | 0.764 | | 1.70 | 1.18 | 0.603 | | 1.04 | 0.830 | 0.505 | | 6.61 × 1011 | 40 | 130 | 0.649 | 2.67 | 0.873 | 2.29 | 1.50 | 0.721 | 1.36 | 1.04 | 0.605 | | 8.79 × 1011 | 41 | 134 | 0.943 | 3.30 | 1.09 | 3.05 | 1.71 | 0.842 | 1.42 | 1.29 | 0.723 | | 1.20 × 1012 | 42 | 137 | 1.32 | 3.77 | 1.19 | 3.98 | 2.32 | 1.01 | 2.21 | 1.59 | 0.854 | | 1.47 × 1012 | 42 | 140 | 1.70 | 4.76 | 1.36 | 5.09 | 2.84 | 1.19 | 2.66 | 1.87 | 0.937 | | 2.00 × 1012 | 43 | 144 | 2.00 | 4.85 | 1.65 | 6.41 | 3.29 | 1.30 | 3.40 | 2.28 | 1.12 | | 2.67 × 1012 | 44 | 149 | 2.66 | 5.66 | 1.81 | 7.99 | 3.79 | 1.43 | 4.18 | 2.65 | 1.31 | | 3.51 × 1012 | 45 | 154 | 3.48 | 6.49 | 1.91 | 11.30 | 4.58 | 1.64 | 5.20 | 3.17 | 1.45 | | 4.54 × 1012 | 46 | 161 | 4.20 | 7.32 | 2.11 | 15.80 | 5.31 | 1.92 | 6.56 | 3.81 | 1.69 | | 6.25 × 1012 | 48 | 170 | 5.58 | 8.64 | 2.44 | 17.90 | 6.49 | 2.24 | 8.65 | 4.74 | 1.99 | | 8.38 × 1012 | 49 | 181 | 6.94 | 9.74 | 2.69 | 23.10 | 7.53 | 2.52 | 11.20 | 5.61 | 2.27 | | 1.10 × 1013 | 51 | 193 | 8.58 | 12.00 | 3.06 | 28.80 | 8.80 | 2.86 | 13.80 | 6.65 | 2.68 | | 1.50 × 1013 | 54 | 211 | 10.90 | 13.20 | 3.50 | 35.70 | 10.80 | 3.29 | 17.40 | 7.98 | 2.97 | | 1.99 × 1013 | 57 | 232 | 13.10 | 15.10 | 3.98 | 43.70 | 12.60 | 3.77 | 21.30 | 9.40 | 3.45 | | 2.58 × 1013 | 60 | 257 | 15.30 | 17.00 | 4.48 | 51.30 | 14.00 | 4.24 | 25.00 | 11.10 | 3.90 | | 3.44 × 1013 | 65 | 296 | 17.70 | 19.90 | 5.25 | 59.70 | 16.40 | 4.95 | 28.90 | 12.70 | 4.55 | | 4.68 × 1013 | 72 | 354 | 20.50 | 23.70 | 6.25 | 67.70 | 19.30 | 5.89 | 32.70 | 14.70 | 5.38 | | 5.96 × 1013 | 78 | 421 | 21.80 | 26.70 | 7.10 | 69.00 | 21.30 | 6.65 | 33.80 | 16.00 | 6.03 | | 8.01 × 1013 | 89 | 548 | 22.10 | 31.30 | 8.49 | 69.80 | 23.90 | 7.83 | 34.70 | 17.30 | 6.96 | | 9.83 × 1013 | 100 | 683 | 23.20 | 35.40 | 9.79 | 70.30 | 25.50 | 8.85 | 36.10 | 17.70 | 7.65 | | 1.30 × 1014 | 120 | 990 | 25.50 | 40.30 | 11.80 | 70.80 | 25.50 | 10.10 | 28.20 | 18.10 | 8.20 |
|
Table 3. Partial values of electrical conductivity for different temperatures and impurity parameters in the crust of magnetars. Here we use the equation of station (EOS) of BBP model.
在不同温度和不同纯净度参数下磁星壳层电导率的部分值(采用BBP模型)
$\sigma $![]() ![]() /s–1 | t/a
| ${B_{\rm{p}}}$![]() ![]() /G
| ${{{\rm{d}}B_{\rm{p}}^{}}/{{\rm{d}}t}}$![]() ![]() /G·a–1 | ${L_{\rm{p}}}$![]() ![]() /erg·s–1 | ${B_{\rm{t}}}$![]() ![]() /G
| ${{{\rm{d}}B_{\rm{t}}^{}}/{{\rm{d}}t}}$![]() ![]() /G·a–1 | ${L_{\rm{t}}}$![]() ![]() /erg·s–1 | ${L_B}$![]() ![]() /erg·s–1 | | 8.75 × 1024 | 5.0 × 102 | 1.995 × 1015 | –5.92 × 109 | 1.57 × 1034 | 1.965 × 1016 | –5.84 × 1010 | 6.28 × 1035 | 6.44 × 1035 | | 2.0 × 103 | 1.981 × 1015 | –4.65 × 109 | 1.15 × 1034 | 1.953 × 1016 | –4.58 × 1010 | 4.59 × 1035 | 4.70 × 1035 | | 2.0 × 104 | 1.954 × 1015 | –1.37 × 108 | 3.61 × 1033 | 1.927 × 1016 | –1.35 × 1010 | 1.44 × 1035 | 1.48 × 1035 | | 2.0 × 105 | 1.844 × 1015 | –5.91 × 108 | 1.63 × 1033 | 1.818 × 1016 | –5.84 × 1010 | 6.52 × 1034 | 6.68 × 1034 | | 2.0 × 106 | 1.373 × 1015 | –8.61 × 107 | 1.56 × 1032 | 1.354 × 1016 | –8.48 × 108 | 6.24 × 1033 | 6.40 × 1033 | | 2.0 × 107 | 6.865 × 1014 | –4.36 × 107 | 7.85 × 1031 | 6.772 × 1015 | –4.29 × 108 | 3.14 × 1033 | 3.22 × 1033 | | 2.52 × 1024 | 5.0 × 102 | 1.990 × 1015 | –1.51 × 1010 | 3.98 × 1034 | 1.96 × 1016 | –1.49 × 1011 | 1.59 × 1036 | 1.63 × 1036 | | 2.0 × 103 | 1.977 × 1015 | –5.43 × 1010 | 1.65 × 1034 | 1.95 × 1016 | –5.36 × 1010 | 6.61 × 1035 | 6.77 × 1035 | | 2.0 × 104 | 1.931 × 1015- | –1.86 × 109 | 4.74 × 1033 | 1.905 × 1016 | –1.83 × 1010 | 1.90 × 1035 | 1.94 × 1035 | | 2.0 × 105 | 1.745 × 1015 | –7.21 × 109 | 1.69 × 1033 | 1.721 × 1016 | –7.11 × 1010 | 6.76 × 1034 | 6.93 × 1034 | | 2.0 × 106 | 8.712 × 1014 | –3.87 × 109 | 4.46 × 1032 | 8.592 × 1015 | –3.82 × 1010 | 1.78 × 1034 | 1.83 × 1034 | | 2.0 × 107 | 2.749 × 1013 | –1.33 × 107 | 4.82 × 1029 | 2.711 × 1014 | –1.31 × 108 | 1.93 × 1031 | 1.98 × 1031 |
|
Table 4. Partial values of Bp, dBp/dt, Lp, Bt, dBt/dt, Lt and LB when Bp(0) = 2.0 × 1015 G. Here we assume a medium-mass magnetar M = 1.45M⊙, R = 11.77 km, Rc = 0.97 km, corresponding to I = 1.47I45 and
, respectively. The top and bottom parts correspond to
and
, respectively.
当Bp(0) = 2.0 × 1015 G时Bp, dBp/dt, Lp, Bt, dBt/dt, Lt和LB的部分值(假定一个中等质量的磁星M = 1.45M⊙, R = 11.77 km, Rc = 0.98 km, 对应着I = 1.47I45和
; 表格上和下半部分分别对应着
和
)
| Source | P/s
| $\dot{ P}$![]() ![]() /10–11 s–1 | ${\tau _{\rm{c}}}$![]() ![]() /ka
| Age Est/ka | Associa. | Method | $L_{\rm{X}}^\infty $![]() ![]() /erg·s–1 | Lrot./erg·s–1 | Refs. | | SGR 0418+5729 | 9.07839 | 0.0004(1) | 36000 | 550 | SMC | 磁热模拟 | 9.60 × 1029 | 3.1 × 1029 | [46,48,49]
| | 1E 2259+586 | 6.97904 | 0.04837 | 230.0 | 10—20 | SNR CTB109 | SNR年龄 | 1.70 × 1034 | 7.37 × 1031 | [50—52]
| | 4U 0142+61 | 8.68870 | 0.2022(4) | 68.0 | 68.0 | SMC | 特征年龄 | 1.05 × 1035 | 1.85 × 1032 | [49,50,53]
| | CXOU J164710 | 10.61 | < 0.04 | > 420.0 | > 420 | Cluster Wdl | 特征年龄 | 4.50 × 1032 | < 1.88 × 1031 | [54,55]
| | 1E 1048–5937 | 6.45787 | 2.250 | 4.5 | 4.5 | GSH 288.3–0.5–28 | 特征年龄 | 4.90 × 1034 | 4.65 × 1033 | [56—58]
| | CXOU J010043 | 8.02039 | 1.88(8) | 6.8 | 6.8 | SMC | 特征年龄 | 6.50 × 1034 | 2.33 × 1033 | [49,59]
| | 1RXS J170849 | 11.00502 | 1.9455(13) | 9.0 | 9.0 | MC 13A | 特征年龄 | 4.20 × 1034 | 7.37 × 1032 | [50,55]
| | 1E 1841–045 | 11.78898 | 4.092(15) | 4.70 | 0.5—1.0 | SNR Kes73 | SNR年龄 | 1.84 × 1035 | 1.47 × 1033 | [50,60]
| | SGR 0501+4516 | 5.76206 | 0.594(2) | 16.00 | 4—6 | SNR HB9 | SNR年龄 | 8.10 × 1032 | 1.85 × 1033 | [61—63]
| | SGR 0526–66 | 8.054(2) | 3.8(1) | 3.400 | 4.8 | SNR N49 | SNR年龄 | 1.89 × 1035 | 4.22 × 1033 | [64,65]
| | SGR 1900+14 | 5.19987 | 9.2(4) | 0.900 | 3.98—7.9 | Massive star Cluster | 自行年龄 | 9.00 × 1034 | 3.79 × 1034 | [66—68]
| | SGR 1806–20 | 7.54773 | 49.5000 | 0.240 | 0.63—1.0 | W31, MC13A | 自行年龄 | 1.63 × 1035 | 6.68 × 1034 | [68,69]
| | XTE J1810–197 | 5.54035 | 0.777(3) | 11 | 11 | W31, MC13A | 特征年龄 | 4.3 × 1031 | 2.93 × 1035 | [69,70]
| | IE 1547–5408 | 2.07212 | 4.77 | 0.69 | 0.63 | SNR G327.24–013 | SNR年龄 | 1.3 × 1033 | 3.11 × 1035 | [71,72]
| | 3XXMJ185246 | 11.5587 | < 0.014 | > 1300 | 5—7 | SNR Kes 79 | SNR年龄 | < 4.0 × 1038 | < 4.8 × 1038 | [73,74]
| | CXOU J171405 | 3.82535 | 6.40 | 0.95 | 5 | CTB 37B | SNR年龄 | 5.6 × 1034 | 6.13 × 1034 | [45,75]
| | SGR 1627–41 | 2.59458 | 1.9(4) | 2.2 | 5.0 | SNR G337.0–0.1 | SNR年龄 | 3.6 × 1033 | 5.87 × 1034 | [76,77]
| | Swift J1822–1606 | 8.43772 | 0.0021(2) | 6300 | 6300 | HII region | 特征年龄 | < 4.0 × 1029 | 2.0 × 1030 | [78,79]
| | Swift J1834–0864 | 2.4823 | 0.796(12) | 4.9 | 60200 | SNR W41 | SNR年龄 | < 8.4 × 1030 | 3.1 × 1034 | [80,81]
| | PSR J1622–4950 | 4.326(1) | 1.7(1) | 4.0 | ≤ 6.0 | SNR G33.9+0.0 | SNR年龄 | 4.40 × 1032 | 1.18 × 1034 | [63,82]
| | SGR J1745–2900 | 3.7636 | 1.385(15) | 4.30 | 4.30 | Galaxy Center | 特征年龄 | 1.10 × 1032 | 1.47 × 1034 | [83,84]
| | PSR J1846–0258 | 0.32657 | 0.71070 | 0.73 | 0.9-4.3 | SNR Kes75 | SNR年龄 | 1.90 × 1034 | 8.10 × 1036 | [49,85]
|
|
Table 5. The persistent timing, ages and emission characteristics for 22 magnetars with observed soft X-ray flux.
具有软X射线辐射的22颗磁星的到达时间及其辐射特性
| Source | Bp(0)/G
| PL Ind. | $T_{BB}^{\infty} $![]() ![]() /keV
| D/kpc
| $F_{\rm{X}}^\infty $![]() ![]() /erg·s–1·cm2 | $L_{\rm{X}}^\infty $![]() ![]() /erg·s–1 | $L_B^{\rm{a}}$![]() ![]() /erg·s–1 | $\eta _{}^{\rm{a}}$![]() ![]() /%
| $L_B^{\rm{b}}$![]() ![]() /erg·s–1 | $\eta _{}^{\rm{b}}$![]() ![]() /%
| Ref. | 注: a表示
$\sigma = 2.52 \times {10^{24} }\; { {\rm{s} }^{ {\rm{ - 1} } } }$![]() ![]() 的情况; b表示
$\sigma = 8.75 \times {10^{24} } \;{ {\rm{s} }^{ {\rm{ - 1} } } }$![]() ![]() 的情况; PL Ind. 表示幂率指数.
| | SGR 0418–5729 | 3.0 × 1014 | — | 0.30 | 2.0 | 2.0 × 10–11 | 9.60 × 1029 | 5.35 × 1032 | 0.31 | 2.26 × 1032 | 0.74 | [48,49,50]
| | 1E 2259+586 | 5.0 × 1014 | 3.75(4) | 0.37(1) | 3.2(2) | 1.41 × 10–11 | 1.70 × 1034 | 6.5(1.0) × 1035 | 22(6) | 1.4(3) × 1035 | 47(8) | [50—52]
| | CXOU J164710 | 3.0 × 1014 | 3.86(22) | 0.59(6) | 3.9(7) | 2.54 × 10–11 | 4.50 × 1032 | 8.65 × 1033 | 9 | 3.62 × 1033 | 21 | [50,54,95]
| | 3XXMJ185246 | 3.0 × 1014 | — | 0.6 | 7.1 | 1.0 × 10–15 | 4.0 × 1033 | 3.53 × 1034 | | 3.11 × 1035 | | [73,74]
| | 4U 0142+61 | 3.0 × 1015 | 3.88(1) | 0.41 | 3.6(4) | 6.97 × 10–11 | 1.0 × 1035 | 1.14 × 1036 | 15 | 4.85 × 1035 | 37 | [50,53,96]
| | 1E1048–5937 | 1.0 × 1015 | 3.14(11) | 0.56(1) | 9.0(1.7) | 5.11 × 10–11 | 4.90 × 1034 | 7.19 × 1035 | 12 | 3.08 × 1035 | 27 | [50,57,58]
| | CXOU J010043 | 1.0 × 1015 | — | 0.30(2) | 62.4(1.6) | 1.40 × 10–11 | 6.50 × 1034 | 6.82 × 1035 | 16 | 3.22 × 1035 | 34 | [50,97]
| | IRXS J170849 | 1.0 × 1015 | 2.79(1) | 0.456 | 3.8(5) | 2.43 × 10–11 | 4.20 × 1034 | 7.65 × 1035 | 9 | 3.23 × 1035 | 21 | [50,53,96]
| | 1E1841–045 | 1.0 × 1015 | 1.9(2) | 0.45(3) | 8.6(1.1) | 2.13 × 10–11 | 1.84 × 1035 | 1.2(2) × 1036 | 26(4) | 5.9(7) × 1035 | 46(4) | [50,98,99]
| | SGR 0526–66 | 3.0 × 1015 | $2.5_{ - 0.12}^{ + 0.11}$![]() ![]() | 0.44(2) | 53.6(1.2) | 5.50 × 10–11 | 1.89 × 1035 | 2.28 × 1036 | 8 | 7.11 × 1035 | 26 | [50,65]
| | SGR1900+14 | 3.0 × 1015 | 1.9(1) | 0.47(2) | 13.0(1.2) | 4.82 × 10–12 | 9.0 × 1034 | 2.2(6) × 1036 | 7(1) | 7.8(8) × 1035 | 19(2) | [50,66]
| | SGR1806–20 | 3.0 × 1015 | 1.6(1) | 0.55(7) | 8.8(1.6) | 1.81 × 10–12 | 1.63 × 1035 | 3.8(4) × 1036 | 7.4(8) | 8.9(9) × 1035 | 26(2) | [50,69]
|
|
Table 6. The X-ray emission characteristics and magnetic field energy decay rates of 12 magnetars with rotational energy loss rates less than their soft X-ray luminosities.
12颗旋转能损率远小于软X射线光度的磁星的辐射特性及磁场能衰变率
