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Дата изменения: Thu Apr 6 09:09:10 2000
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Recent Progress In Magnetars
D. L. Kaplan - Caltech
S. R. Kulkarni - Caltech
D. A. Frail - NRAO
R. E. Rotschild - UCSD
et al.
Arecibo Pulsar Workshop
March 2000

Introduction
 Magnetars: highly magnetized (B >
 10 14 G  B PSR
) neutron
stars
 = Soft Gamma-ray Repeaters?
 4 (maybe 5) known
 Hard (kT  100 keV), highly super-Eddington bursts
 Softer (kT = 1{10 keV) quiescent emission
 Bursts likely associated with out ow of particles | transient
radio nebulae
 All (?) associated with SNRs
 Long periodicities seen in bursts and quiescence
 Implied ages may not be related to actual ages
 Signi cant \glitches," but not like PSRs
 Related to AXPs?

SGR 0526 66
History:
 5 March 1979 burst
 Located in SNR N49 in LMC
 No optical/radio counterparts (Dickel et al. 1995)
 X-ray counterpart: RX J0525 6607 (Marsden et al. 1996)
 8 s periodicity (burst only)
Fig. 1.| ROSAT image of N49/SGR 0526 66, from Marsden et al. 1996.

SGR 0526 66
HST
 HST WF/PC2 in four bands (F300W, F380W, F547M, F814W)
 Goal: nd companion to SGR or surrounding plerion
(from 5 March 1979 burst)
 Source: faint; blue; elongated? (from motion through SNR)
 No obvious source found
CXO
 Imaged with CXO ACIS, to:
{ Improve position (ROSAT/Marsden et al. 1996 give 5 00
uncertainties) ! uniquely identify counterparts
{ Uniquely determine spectrum (ROSAT & EINSTEIN have
ambiguities, leading to R e
/T e
degeneracy)
{ Search for periodicity
 Point source
 No evidence for X-ray plerion
 CXO data still being analyzed | calibration issues

A
B
C D
E
F SGR0526­66
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ARCSEC
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ARCSEC
HST F547M ( V ) image of RX J0525 6607, with 2 00 error circle indicated.
­3 ­2 ­1 0 1 2 3 4
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B­V
V
Color­Magnitude Diagram for Stars in SGR 0526­66 Field
­3 ­2 ­1 0 1 2 3
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U­B
B­V
Color­Color Diagram for Stars in SGR 0526­66 Field
Plots of Stars in HST image, with sources above indicated.

SGR 1900+14
History:
 27 August 1998 burst | brightest recorded.
 Found fading radio plerion ! particle emission (Frail, Kulkarni,
& Bloom 1999)
 Periodicity in burst & quiescence, with detected _
P
 Age from P , _
P may not agree with SNR age (Marsden, Rotschild,
& Lingenfelter 1999)
 Signi cant changes in _
P (MRL 1999, Thompson et al. 1999)
 If associated with SNR G42.8+0.6, v  10 3 km s 1 , oldest SGR
(Vashist et al. 1994)
 Radio pulsar nearby

SGR 1900+14
 Imaged with VLA at 1.4 GHz and 327 MHz
 Goal: search for faint fossil nebula powered by bursts
 1.4 GHz map: possible (but still very uncertain) indication of
second SNR, much closer to SGR 1900+14 and PSR J1907+09
 Con rmation of second SNR: lessen constraints on space
velocity/age of SGR (if associated), or provide origin of PSR
(if associated with that)
 Still preliminary | reducing 327 MHz data to con rm
DECLINATION
(J2000)
RIGHT ASCENSION (J2000)
19 07 14.8 14.6 14.4 14.2 14.0 13.8 13.6 13.4
09 19 30
25
20
15
10
1998 June 25
DECLINATION
(J2000)
RIGHT ASCENSION (J2000)
19 07 14.8 14.6 14.4 14.2 14.0 13.8 13.6 13.4
09 19 30
25
20
15
10
1998 September 03
(Left) Before 27 Aug '98 burst. (Right) After 27 Aug '98 burst, showing plerion

BOTH: SGR1900 IPOL 1425.000 MHZ SGR1900.MA.1
PLot file version 1 created 21­JAN­2000 12:24:49
Grey scale flux range= 0.00 30.00 MilliJY/BEAM
Cont peak flux = 2.8182E­01 JY/BEAM
Levs = 3.500E­03 * (­1.41, ­1, 1, 1.414, 2, 2.828,
4, 5.657, 8, 11.31, 16, 22.63, 32, 45.25, 64, 90.51)
0 10 20 30
DECLINATION
(J2000)
RIGHT ASCENSION (J2000)
19 08 00 07 45 30 15 00 06 45 30 15
09 25
20
15
10
05
PSR J1907+09
SGR 1900+14
Possible New SNR Shell???
Old SNR Shell

RX J0720.4 2135
 Imaged with VLA (D-array) to search for faint, di use emission.
 Nothing found: S 1:4 GHz < 0:64 mJy arcmin 2 .

Future
 Soon: calibrated CXO images of RX J0720.4 2135,
SGR 0526 66, and others | determine positions and spectra
to high accuracy
 Searching through all CXO data | looking for neutron stars
 Optical followup of new neutron star candidates with
Palomar/Keck
 VLA imaging | search for plerions