1. Variability of cosmic Gamma-Ray Burst (II)
Pozanenko*, V. Loznikov* , R. Preece#
*Space Research Institute (IKI) #Dept. of Physics, Univ. of Alabama in Huntsville

2. Aperiodic variability (I)
Coherent variability (II)

3. Short duration GRB connection with SGR?
1982: Mazets, E. P., et al., Ap&SS, 84, 173
1982 …….. -- ……… 2004
2004: Boggs, S. et al. SGR , RHESSI observations of the giant flare, GCN Circ. No. 2936

4. Soft Gamma-ray Repeaters
Sporadic activity in soft gamma-rays
4 SGRs are known (SGR , SGR , SGR , SGR )
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)

5. Dec Giant Flash of SGR
RHESSI, INTEGRAL, Konus-Wind, Swift, Geotail, Helicon-Coronas-F …

6. Dec Giant Flash of SGR
RHESSI, K.Hurley et al.

7. Dec.27 2004 GF of SGR1806-20 Konus-Wind, E.Mazets, et al.
Swift, D. Palmer, at al

8. Dec Giant Flash of SGR

9. Short duration GRB Duration of T90 less than 2 seconds No counterparts
A separate class of GRBs
Possible Distant (< 30 Mpc) SGR?

10. Short duration GRB …

11. Short GRB time profiles in different energy bands…

12. 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?

13. Before start:
Can be Giant Flash from SGR detected from distance about 30 Mpc? YES
Is it enough SGRs within 30 Mpc? YES

14. 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!

15. 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)

16. BATSE GRB time profile: Resolution, data types and coverage
To – trigger time
BATSE:
DISCSC+PREB – 64ms, To-2.048, To+ ~150 s

17. BATSE Short GRB F64 > 25 phot/cm^2/sId
Name
comments
0298
910609
0444
910626
2514
930905
3152
94090
3412
950211
3736
950805
6293
6668
980330
telemetry errors

18. BATSE 2514 (930905) time profile

19. BATSE 2514 (930905) Power spectrum, Periodogram
Reduced 2
Frequency, Hz

20. BATSE 2514 (930905) Phase profile in 100-300 keV P = 6.425 s

21. Anomalous X-ray Pulsars (V. M. Kaspi., F. P. Gavriil, 2004), HXMB

22. BATSE Short GRB F64 > 25 phot/cm^2/sId
Name
Possible period
0298
910609 -
0444
910626 ?
2514
930905
3152
94090 ?
3412
950211 ?
3736
950805
6293
6668
980330
Data corrupted in telemetry

23. First direct connection of SGR and Short GRB
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