Download - Variability of cosmic Gamma-Ray Burst (II)
![Page 1: Variability of cosmic Gamma-Ray Burst (II)](https://reader036.vdocument.in/reader036/viewer/2022062309/568144e8550346895db1b91e/html5/thumbnails/1.jpg)
Variability of cosmic Gamma-Ray Burst (II)
A. Pozanenko*, V. Loznikov* , R. Preece#
*Space Research Institute (IKI)
#Dept. of Physics, Univ. of Alabama in Huntsville
![Page 2: Variability of cosmic Gamma-Ray Burst (II)](https://reader036.vdocument.in/reader036/viewer/2022062309/568144e8550346895db1b91e/html5/thumbnails/2.jpg)
• Aperiodic variability (I)
Coherent variability (II)
![Page 3: Variability of cosmic Gamma-Ray Burst (II)](https://reader036.vdocument.in/reader036/viewer/2022062309/568144e8550346895db1b91e/html5/thumbnails/3.jpg)
Short duration GRB connection with SGR?
• 1982: Mazets, E. P., et al., Ap&SS, 84, 173• 1982 …….. -- ……… 2004• 2004: Boggs, S. et al. SGR1806-20, RHESSI
observations of the 041227 giant flare, GCN Circ. No. 2936
![Page 4: Variability of cosmic Gamma-Ray Burst (II)](https://reader036.vdocument.in/reader036/viewer/2022062309/568144e8550346895db1b91e/html5/thumbnails/4.jpg)
Soft Gamma-ray Repeaters
• Sporadic activity in soft gamma-rays
• 4 SGRs are known (SGR 0526-66, SGR 1900+14, SGR 1627-41, SGR 1806-20)
• Giant Flashes followed long pulsating tail (period 5 – 8 seconds)
• Magnetars = Neutron star with intense magnetic field (> 1014 G)
• Close to the Earth (6-55 Kpc)
![Page 5: Variability of cosmic Gamma-Ray Burst (II)](https://reader036.vdocument.in/reader036/viewer/2022062309/568144e8550346895db1b91e/html5/thumbnails/5.jpg)
Dec.27 2004 Giant Flash of SGR1806-20
• RHESSI, INTEGRAL, Konus-Wind, Swift, Geotail, Helicon-Coronas-F …
![Page 6: Variability of cosmic Gamma-Ray Burst (II)](https://reader036.vdocument.in/reader036/viewer/2022062309/568144e8550346895db1b91e/html5/thumbnails/6.jpg)
Dec.27 2004 Giant Flash of SGR1806-20
RHESSI, K.Hurley et al.
![Page 7: Variability of cosmic Gamma-Ray Burst (II)](https://reader036.vdocument.in/reader036/viewer/2022062309/568144e8550346895db1b91e/html5/thumbnails/7.jpg)
Dec.27 2004 GF of SGR1806-20
Konus-Wind, E.Mazets, et al. Swift, D. Palmer, at al
![Page 8: Variability of cosmic Gamma-Ray Burst (II)](https://reader036.vdocument.in/reader036/viewer/2022062309/568144e8550346895db1b91e/html5/thumbnails/8.jpg)
Dec.27 2004 Giant Flash of SGR1806-20
![Page 9: Variability of cosmic Gamma-Ray Burst (II)](https://reader036.vdocument.in/reader036/viewer/2022062309/568144e8550346895db1b91e/html5/thumbnails/9.jpg)
Short duration GRB
• Duration of T90 less than 2 seconds
• No counterparts
• A separate class of GRBs
• Possible Distant (< 30 Mpc) SGR?
![Page 10: Variability of cosmic Gamma-Ray Burst (II)](https://reader036.vdocument.in/reader036/viewer/2022062309/568144e8550346895db1b91e/html5/thumbnails/10.jpg)
Short duration GRB …
![Page 11: Variability of cosmic Gamma-Ray Burst (II)](https://reader036.vdocument.in/reader036/viewer/2022062309/568144e8550346895db1b91e/html5/thumbnails/11.jpg)
Short GRB time profilesin different energy bands…
![Page 12: Variability of cosmic Gamma-Ray Burst (II)](https://reader036.vdocument.in/reader036/viewer/2022062309/568144e8550346895db1b91e/html5/thumbnails/12.jpg)
Before start:
• Can be Giant Flash from SGR detected from distance about 30 Mpc?
• Is it enough SGRs within 30 Mpc?
• Can be detected Pulsating Tail of distant SGR?
![Page 13: Variability of cosmic Gamma-Ray Burst (II)](https://reader036.vdocument.in/reader036/viewer/2022062309/568144e8550346895db1b91e/html5/thumbnails/13.jpg)
Before start:
• Can be Giant Flash from SGR detected from distance about 30 Mpc? YES
• Is it enough SGRs within 30 Mpc? YES
![Page 14: Variability of cosmic Gamma-Ray Burst (II)](https://reader036.vdocument.in/reader036/viewer/2022062309/568144e8550346895db1b91e/html5/thumbnails/14.jpg)
Can be detected Pulsating Tail of distant SGR???
• The tail energy is the same for all Giant Flashes from SGRs registered
• The ratio of Main Spike of Giant Flashes to the amplitude of pulsation in the tail is varying between 40 and 600
• The amplitude of pulsation depends on geometry, and does not depend on Main Spike
For bright short GRB of BATSE the tail may be detected!
![Page 15: Variability of cosmic Gamma-Ray Burst (II)](https://reader036.vdocument.in/reader036/viewer/2022062309/568144e8550346895db1b91e/html5/thumbnails/15.jpg)
Burst Choice
BATSE:
• Short GRBs (T90 < 2 s)
• Bright GRBs (F64 > 25 phot/cm^2/s)
• 64 ms data • Chan1 ( ~ 25 – 50 keV)• Chan2 ( ~ 50 – 100 keV)• Chan3 ( ~ 100 – 300 keV)• Chan4 ( > 300 keV)
![Page 16: Variability of cosmic Gamma-Ray Burst (II)](https://reader036.vdocument.in/reader036/viewer/2022062309/568144e8550346895db1b91e/html5/thumbnails/16.jpg)
BATSE GRB time profile:Resolution, data types and coverage
To – trigger timeBATSE:DISCSC+PREB – 64ms, To-2.048, To+ ~150 s
![Page 17: Variability of cosmic Gamma-Ray Burst (II)](https://reader036.vdocument.in/reader036/viewer/2022062309/568144e8550346895db1b91e/html5/thumbnails/17.jpg)
BATSE Short GRB F64 > 25 phot/cm^2/s
Id Name comments
0298 910609
0444 910626
2514 930905
3152 94090
3412 950211
3736 950805
6293 970704-
6668 980330 telemetry errors
![Page 18: Variability of cosmic Gamma-Ray Burst (II)](https://reader036.vdocument.in/reader036/viewer/2022062309/568144e8550346895db1b91e/html5/thumbnails/18.jpg)
BATSE 2514 (930905)time profile
Time
0 50 100 150 200
Cou
nts
per0.
064s
Time
0 50 100 150 200
Cou
nts
per0.
064s
102
103
104
![Page 19: Variability of cosmic Gamma-Ray Burst (II)](https://reader036.vdocument.in/reader036/viewer/2022062309/568144e8550346895db1b91e/html5/thumbnails/19.jpg)
BATSE 2514 (930905)Power spectrum, Periodogram
0.01 0.1 1 100
5
10
15
20
#3
0.1 0.2 0.3 0.40
1
2
3
4
5
#3
Pow
erR
educ
ed
2
Frequency, Hz
![Page 20: Variability of cosmic Gamma-Ray Burst (II)](https://reader036.vdocument.in/reader036/viewer/2022062309/568144e8550346895db1b91e/html5/thumbnails/20.jpg)
BATSE 2514 (930905)Phase profile in 100-300 keV
P = 6.425 s
Phase
0.0 0.5 1.0 1.5 2.0 2.5
Cou
nts
perbi
n
57500
58000
58500
59000
59500
60000
![Page 21: Variability of cosmic Gamma-Ray Burst (II)](https://reader036.vdocument.in/reader036/viewer/2022062309/568144e8550346895db1b91e/html5/thumbnails/21.jpg)
Anomalous X-ray Pulsars(V. M. Kaspi., F. P. Gavriil, 2004), HXMB
![Page 22: Variability of cosmic Gamma-Ray Burst (II)](https://reader036.vdocument.in/reader036/viewer/2022062309/568144e8550346895db1b91e/html5/thumbnails/22.jpg)
BATSE Short GRB F64 > 25 phot/cm^2/s
Id Name Possible period
0298 910609 -
0444 910626 1.66 +- 0.05 ?
2514 930905 6.425 +- 0.160
3152 94090 4.00 +- 0.11 ?
3412 950211 6.79 +- 0.17 ?
3736 950805 -
6293 970704- -
6668 980330 Data corrupted in telemetry
![Page 23: Variability of cosmic Gamma-Ray Burst (II)](https://reader036.vdocument.in/reader036/viewer/2022062309/568144e8550346895db1b91e/html5/thumbnails/23.jpg)
Conclusions
• First direct connection of SGR and Short GRB
• Bright galaxy with intensive star formation should be searched within error-box of GRB with (pulsating) tail
• One can estimate distances to Short GRBs which manifest the pulsating tail
• Swift will be able to detect pulsating tale of Short GRB >~ three times more efficiently