Advances in Astronomy / 2009 / Article / Tab 1

Research Article

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)

SGR1806 20 281 3500 30000 10300 ( 1%) 100 3800
SGR1900 14 1050 9600 30000 17000 (4%) 7 2000 32000
SGR0525 66 1960 5000 16000 8940 S (0.2–0.7%) 50 800 3600
SGR1627 41 N/A 2600 30000 8830 (5%) 11 460 N/A
AXP1E1841 045 4510 500 2500 1120 S (0.01%) 7 890 220
AXP1845 0258 N/A 600 30000 4240 S (0.2%) 20 870 N/A
AXP1E2259 586 228000 3000 17000 7140 S (0.05%) 360 11
AXP1E1048 5937 N/A N/A N/A N/A N/A N/A N/A
AXPRXS1708 4009 8960 N/A N/A N/A N/A N/A N/A N/A
TAXPXTEJ1810 197 N/A N/A N/A N/A N/A N/A N/A
TAXPJ0100 7211 6760 N/A N/A N/A N/A N/A N/A N/A
AXP1547 5408 1400 N/A N/A N/A N/AN/A N/A N/A
AXP4U0142 615 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.

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