Variability of cosmic Gamma-Ray Burst (II)

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Presentation transcript:

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

Aperiodic variability (I) Coherent variability (II)

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

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)

Dec.27 2004 Giant Flash of SGR1806-20 RHESSI, INTEGRAL, Konus-Wind, Swift, Geotail, Helicon-Coronas-F …

Dec.27 2004 Giant Flash of SGR1806-20 RHESSI, K.Hurley et al.

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

Dec.27 2004 Giant Flash of SGR1806-20

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

Short duration GRB …

Short GRB time profiles in different energy bands…

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?

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

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!

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)

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

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

BATSE 2514 (930905) time profile

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

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

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

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

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