2000ApJ...543..340T


Query : 2000ApJ...543..340T

2000ApJ...543..340T - Astrophys. J., 543, 340-350 (2000/November-1)

Physical mechanisms for the variable spin-down and light curve of Sgr 1900+14.

THOMPSON C., DUNCAN R.C., WOODS P.M., KOUVELIOTOU C., FINGER M.H. and VAN PARADIJS J.

Abstract (from CDS):

We consider the physical implications of the rapid spin-down of soft gamma repeater SGR 1900+14 reported by Woods and colleagues in 1999. During an 80 day interval between 1998 June and the large outburst on 1998 August 27, the mean spin-down rate increased by a factor of 2.3, resulting in a positive period offset of ΔP/P=10–4. A radiation-hydrodynamical outflow associated with the August 27 event could impart the required torque, but only if the dipole magnetic field is stronger than ∼1014 G and the outflow lasts longer and/or is more energetic than the observed X-ray flare. A positive period increment is also a natural consequence of a gradual, plastic deformation of the neutron star crust by an intense magnetic field, which forces the neutron superfluid to rotate more slowly than the crust. Sudden unpinning of the neutron vortex lines during the August 27 event would then induce a glitch opposite in sign to those observed in young pulsars, but of a much larger magnitude as a result of the slower rotation.

The change in the persistent X-ray light curve following the August 27 event is ascribed to continued particle heating in the active region of that outburst. The enhanced X-ray output can be powered by a steady current flowing through the magnetosphere, induced by the twisting motion of the crust. The long-term rate of spin-down appears to be accelerated with respect to a simple magnetic dipole torque. Accelerated spin-down of a seismically active magnetar will occur when its persistent output of Alfvén waves and particles exceeds its spin-down luminosity or if particle flows modulate the ratio of conduction to displacement currents in the outer magnetosphere. We suggest that SGRs experience some episodes of relative inactivity, with diminished P{dot}, and that such inactive magnetars are observed as anomalous X-ray pulsars (AXPs). The reappearance of persistent X-ray emission from SGR 1900+14 within one day of the August 27 event provides strong evidence that the persistent emission is not powered by accretion.


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Journal keyword(s): Stars: Pulsars: General - Stars: Individual: Alphanumeric: SGR 1900+14 - X-Rays: Bursts

Simbad objects: 13

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Number of rows : 13
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026
#notes
1 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 19090 0
2 PSR B0525-66 Psr 05 26 00.7 -66 04 35           ~ 569 1
3 M 1 SNR 05 34 31.8 +22 01 03           ~ 6516 1
4 V* CM Tau Psr 05 34 31.9474694616 +22 00 52.153698024           ~ 5476 0
5 NAME Vela Pulsar Psr 08 35 20.65525 -45 10 35.1545     15.10     ~ 2446 1
6 2E 2336 HXB 10 50 08.93 -59 53 19.9           Be 419 0
7 3FHL J1746.2-2852 LXB 17 44 33.09 -28 44 27.0           ~ 559 0
8 PSR J1808-2024 Psr 18 08 39.32 -20 24 40.1           ~ 1316 2
9 SNR G027.3+00.0 SNR 18 41 17.8 -04 56 12           ~ 345 3
10 GBS 1900+14 gB 19 07 13 +09 19.6           ~ 906 0
11 SNR G042.8+00.6 SNR 19 07 41.890 +09 07 17.29           ~ 134 1
12 2E 4673 HXB 23 01 08.14 +58 52 44.5           ~ 673 1
13 SNR G109.1-01.0 SNR 23 01 35 +58 53.0           ~ 362 0

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