SGRs and AXPs: Evidence for Delayed Amplification of Magnetic Field after Neutron Star Formation?
Table 1
SGRs/AXPs data mainly from Gaensler et al. [5], Marsden et al. [4], the atnf pulsar catalog [12], and Camilo [13]; with updates as indicated by footnotes. Spin-down ages, , and SNR ages, , in years.
Source
Assoc.
(km/s)
(km/s)
SGR180620
281
3500
30000
10300
(1%)
100
3800
SGR190014
1050
9600
30000
17000
(4%)
7
2000
32000
SGR052566
1960
5000
16000
8940
S (0.2–0.7%)
50
800
3600
SGR162741
N/A
2600
30000
8830
(5%)
11
460
N/A
AXP1E1841045
4510
500
2500
1120
S (0.01%)
7
890
220
AXP18450258
N/A
600
30000
4240
S (0.2%)
20
870
N/A
AXP1E2259586
228000
3000
17000
7140
S (0.05%)
360
11
AXP1E10485937
N/A
N/A
N/A
N/A
N/A
N/A
N/A
AXPRXS17084009
8960
N/A
N/A
N/A
N/A
N/A
N/A
N/A
TAXPXTEJ1810197
N/A
N/A
N/A
N/A
N/A
N/A
N/A
TAXPJ01007211
6760
N/A
N/A
N/A
N/A
N/A
N/A
N/A
AXP15475408
1400
N/A
N/A
N/A
N/A
N/A
N/A
N/A
AXP4U0142615
70200
N/A
N/A
N/A
N/A
N/A
N/A
N/A
Frail et al. [14]; McClure-Griffiths and Gaensler [15]; Vasisht et al. [16]; Lorimer and Xilouris [17]; Smith et al. [18]; based on prior to 2002 outburst [19]; Camillo et al. [20]; Kothes et al. [21]. S for secure and A for ambiguous association (random association probability given in brackets);unconfirmed AXP.
