Документ взят из кэша поисковой машины. Адрес оригинального документа : http://www.naic.edu/~pulsar/y2kws/talks/dave/talk.ps
Дата изменения: Thu Apr 6 09:09:10 2000
Дата индексирования: Sun Dec 23 01:10:14 2007
Кодировка:
Поисковые слова: спрайты

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
Signicant \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
0
1
2
3
4
5
1
2
3
4
5
ARCSEC 0
1
2
3
4
5
1
2
3
4
5
ARCSEC
0
1
2
3
4
5 1 2 3 4 5
ARCSEC
0
1
2
3
4
5 1 2 3 4 5
ARCSEC
HST F547M ( V ) image of RX J0525 6607, with 2 00 error circle indicated.
3 2 1 0 1 2 3 4
19
20
21
22
23
24
25
26
27
1
2
3
4
5
6
7
8
9
10
11
12
13
14
15 16
17
18 19
20
21
22
23
24
25
26
27 29
30
31
32
33
34
35
36
37
38
39
40
41
42
44
45
46
47
48
49
50
51
52
53
54
55
56
58
59
60
61
62
63
64
66
67
68
69
70
71
72
73
74
75 76
78
79
80
82
83
84
85
86
87
88
89
90
91
92
93 94
95 96
97
98
99
100
101
102
103
104
105
106
107
108
109
110
111
112
113
115
116
117
118
119
120
121
122
123
124
125
126
127
128
129
130
131
132
133
134
135 136
137
138
139
140 141
142
143
144
145
146
147
148
149
150
151
152
153
154
155
156
157
158
159
160
161
162
163
164
166
167
168
169
170 171
172
174
175
177
178
179
180
181
182
183
184
185
186
187
188
189
190
191
192
193
194
196
197
198
199
200
201
202
203
204
205
207
208
209
210
211
212
213
214
215
216
217
218
219
220
221
224
225
227
228 229
230
232
233
234
BV
V
ColorMagnitude Diagram for Stars in SGR 052666 Field
3 2 1 0 1 2 3
2.5
2
1.5
1
0.5
0
0.5
1
1.5
2
2.5
1 2
3
5
6
7 9
10
11
12
13
14
15
16
17
18
19
20
21
22
24
25
27
29
30
31
32
33
34
35
36
37
38
39
40
41
42
44
45
46
47
48
49
50
51
52
53
54
55
56
58
59
60
61
62
63
64
66
67
68
69
70
71
72
73
74
75
76
78
79
83
84
85
86
87
88 90
92
93
95
96
97
98
99
101
102
103
104
105
106
107
110
111
112
113
115
118
119
120
121
122
124
125
126
127
128
129
130
131
132
133
134
135
138
139
140
141
142
143
144
145
146
147
149
150
151
152
153
154
155
157
158
159
160 162
163
164
166
167
168
169
170
171
172
174
177
179 180
182
183
184
185
186
187
188
190
191
193
194
196 198
199
200
201
202
203
205
207
208
209
210
211
212
214
215
216
217
218
219
221
227
228
230
232
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)
Signicant 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
Conrmation 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 conrm
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, diuse 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