1. Giant Radio Pulses Radio Properties Mechanism High Energy Properties With Astrosat & LOFT

2. Giant Radio Pulses Flux density > M Jy T b > 10 37 K! Highly variable polarisation Scales ~ 1 m Crab

3. Giant Radio Pulses Crab Mickaliger et al. 2012 Giant pulses in different Radio frequencies are simultaneous GPs occur only at the normal pulse Phases MP and IP

4. Giant Radio Pulses First observed in the Crab pulsar - discovered through its giant pulses! Intense narrow pulses (~10 ns) Brightness Temp: upto 5 x 10^39 Random in occurrence, at certain pulse phases Pulse energy many times that of an average pulse One or more power-law distribution of pulse energies Highly polarizeded/variable

5. Giant Radio Pulses Crab Popov et al. 2007 Karuppusamy et al. 2010

6. Giant Radio Pulses Crab Majid et al. 2011 Pulse width up to 100  s 50-90% of total pulse Flux energy is in the Giant pulses

7. Giant Radio Pulses PSR B1937+21 Kinkhabwala et al. 2000

8. Giant Radio Pulses PSR B1937+21 Kinkhabwala et al. 2000

9. Giant Radio Pulses PSR B1937+21 Soglasnov et al. 2004 Width: < 15 ns T_B : 5 x 10^39 K Discharges in the polar cap region

10. Giant Radio Pulse: Mechanism Conversion of electrostatic turbulence in the pulsar magnetosphere by the mechanism of spatial collapse of nonlinear wave packets (Hankins et al.,2003) Electric discharge due to the magnetic reconnection of field lines connecting the opposite magnetic poles (Istmin Ya. N., 2004) Coherent curvature radiation of charged relativistic solitons associated with sparking discharge of the inner gap potential drop above the polar cap (Gil, J & Melikadze G., 2004) Induced Compton scattering of pulsar radiation off the particles of the plasma flow (Petrova S. A. 2004) Cyclotron line at the light cylinder during reconnection events (Lyutikov 2013)

11. (Knight et al. 2006) PSR J0218+4232 (Cusumano et al. 2003) PSR B1937+21 Giant Pulses from MSPs Large magnetic field at the light cylinder Pulsed non-thermal X-ray emission X-ray emission at the same phase of GP RXTE BeppoSAX Radio Chandra 0.1-10kev GBT 850 MHz

12. (Shearer et al. 2003) Giant Pulses and High Energy emission: Crab Optical Flux enhancement: 3% Enhancement of electron positron plasma

13. (Strader et al. 2013) Giant Pulses and High Energy emission: Crab Optical Peak flux enhancement: 11% for Giant Pulses near the peak of the optical pulse, 3% otherwise Flux enhancement: 3% for Giant Pulses at the Main Pulse

14. (Bilous et al. 2012) Giant Pulses and High Energy emission: Crab Chandra HRC: 1.5 - 4.5 keV Chandra HCR: 1.5 - 4.5 keV Upper limit of flux enhancement in pulses with GPs: 10% for MP GPs and 30% for IP GPs Upper limit of flux enhancement during the GPs: 2 for MP GPs and 5 for IP GPs Due to changes in coherent radio emissiom

15. (Mikami et al. 2014) Giant Pulses and High Energy emission: Crab Suzaku HXD, 15-75 keV and 35-315 keV 1 σ upper limit of flux enhancement: 70%

16. (Bilous et al. 2011) Giant Pulses and High Energy emission: Crab Fermi: 100 MeV - 5 GeV 95% confidence upper limit of flux enhancement: 4 times for all GPs and 12 for IP GPs Due to changes in coherent radio emissiom and not due to enhanced particle density

17. Aliu et al. 2012 Giant Pulses and High Energy emission: Crab Veritas: > 150 GeV Upper limit of flux enhancement: 5 times for pulses with GP Upper limit of flux enhancement: 2 times for 8s window around GP

18. Cusumano et al. 2003, Nicastro et al. 2004 Giant Pulses and High Energy emission: 1937+21 X-ray emission is at the same phase as the Giant Pulses

19. Giant Pulses and High Energy emission S/N = sA*T/sqrt((sA+bA)T)= sqrt(AT)*s/sqrt(s+b) s T Chandra RXTE-PCA/ASTROSAT-LAXPC Crab: 10 hrs  10000 bursts  0.2 sec, 400 photons,  100 photons (5 sigma)  sensitivity of 0.01 photon per GP  10^33 erg per GP in X-rays

20. Stability of X-ray Pulse Profiles: Crab ISRO HQ - 22 Apr 2014 Jain and Paul 2011