1. Le spectre des GRBs dans le modèle EMBH
Pascal Chardonnet
LAPTH
+ Collaboration Roma La Sapienza
POLAR - January,

2. Discovery of GRBs
GRBs unknown until the end of ‘60 neither predicted by astrophysical or cosmological models
Discovery by chance by Vela satellite (1973)
I revolution (BATSE satellite, ‘90):
isotropy of spatial distribution
II revolution (BeppoSAX, 1997):
discovery of afterglow X
cosmological distance (z order of 1)

3. The EMBH model 1) Spherical symmetry for all the phases.
2) Magnetohydrodynamics and pair equations for the evolution of the plasma in the optically thick phase. Fully radiative condition for the energy emission in the afterglow.
3) nism = 1 particle/cm3 i.e. a constant density interstellar medium.
- “Relative Space Time Transformations” (RSTT) paradigm (Ruffini et al., ApJ 555, L107, 2001)
- “Interpretation of the Burst Structure” (IBS) paradigm (Ruffini et al., ApJ 555, L113, 2001)
- “GRB-supernova Time Sequence” (GSTS) paradigm (Ruffini et al., ApJ 555, L117, 2001)

4. inhomogeneity of interstellar medium
Assumptions
Spherical symmetry
“Fully radiative” condition
Temporal variability of light curve due to
inhomogeneity of interstellar medium
Thermal distribution of energy in comoving frame

5. Parameters of the model
Edya is the total energy emitted by source
B= MBc2/Edya parametrizes baryonic matter protostellar not collapsed
R = Aeff/Atot indicates the porosity of interstellar medium
<nism> is the particle number density of interstellar medium
Edya B

6. Temporal structure of GRB
Collision with baryonic remnant
Increase of opacity of pulse
Conversion of internal energy
in kinetic energy
Edya
Short GRB
Long GRB

7. The bolometric luminosity of the source
Where:
De = internal energy developed in the ABM - ISM collision.
L = g (1 - (v/c) cosJ)
Ruffini, Bianco, Chardonnet, Fraschetti, Xue, ApJ, 581, L19, (2002) Ruffini, Bianco, Chardonnet, Fraschetti, Vitagliano, Xue, “Cosmology and Gravitation”, AIP, (2003)

8. Bolometric light curve
Edya= 4.83 ´1053 erg
B = 3.0 ´10-3

9. GRB 991216 BATSE noise threshold
Ruffini, Bianco, Chardonnet, Fraschetti, Xue, 2001b, ApJ, 555, L113

10. GRB A B C D

11. Temporal substructure of peakD

12. Emitted luminosity
Thermal distribution of energy in comoving system:
Tarris the temperature of radiation emitted by dS and observed on the Earth

13. Luminosity and spectrum:GRB991216
Peak
Afterglow
c2 = 0.497
GRB , , , , ,…

16. Hard-to-Soft evolution
Spectral evolution
Hard-to-Soft evolution
Time integrated spectrum
Non-thermal observed spectrum
GRB , , , , ,…

17. Swift era
Model verified in a precedently unobserved temporal window ( sec)
Structure of light curve afterglow simply explained the claimed
breaks in light curves
GRB050315

18. Conclusions
The model presented builts the whole temporal evolution of the GRB, from the progenitor to the non-relativistic phase of the afterglow.
Interpretation of temporal structure of GRB: P-GRB e E-APE.
The temporal variability of light curve traces the inomogeneities of ISM.
Afterglow observations are compatible with thermal spectrum in pulse comoving system.
No polarization predicted

19. Equations for afterglow
In the laboratory system
with

20. Arrival time (ta) vs. emission time (t)
Power-law slope in the afterglow:
Approximate ta computation:
Exact ta computation:
The observed one is: ± 0.067
(Halpern et al, 2000)
Ruffini, Bianco, Chardonnet, Fraschetti, Xue, 2002a, A&A, submitted to

21. Power law of Lorentz g factor (I)
Inelastic collision of expanding shell with an infinitesimally thick shell
of ISM of mass dm at rest.
Energy-momentum conservation and increment of mass:
from 1) 3)
g0 >> g>> 1

22. Power law of Lorentz g factor (II)
B=10-3
For g0 ~200, power law different from the predicted one (g0 >> g >> 1 not satisfied).
The predicted power laws in limits adiabatic and fully radiative are reached only when g tends to infinity and only in a limited region.
B=10-6

23. Prototype GRB
One of the most energetic GRB ever observd: z = 1.0.
Details on temporal structure by BATSE and on afterglow by satellites R-XTE
and Chandra (Iron lines).
Power law index for afterglow: n= ±

24. GRB 991216 - IBS paradigm BATSE noise threshold
Ruffini, Bianco, Chardonnet, Fraschetti, Xue, 2001b, ApJ, 555, L113

25. GRB 980425 - SN1998bw: A newly formed neutron star
(Pian)
The newly formed neutron star:

26. The luminosity of GRB 030329 and SN 2003dh in the EMBH model

27. The ISM inhomogeneity “mask”
<nism> = 1 particle/cm3 i.e. an interstellar medium with variable density but average density of 1 particle/cm3.
g = 139.9
g = 200.5
DR= 1015 cm
g = 265.4
g = 303.8
g = 57.23
g = 56.24

28. The ABM pulse visible area
Invisible
Visible

29. The observed luminosity: two different time scales
t is the photon emission time from the source.
tad is the photon arrival time at the detector.
Ruffini, Bianco, Chardonnet, Fraschetti, Xue, ApJ, 555, L107, (2001)

30. Arrival time ta vs. emission time t
Ruffini, Bianco, Chardonnet, Fraschetti, Xue, ApJ, 555, L107, (2001) Ruffini, Bianco, Chardonnet, Fraschetti, Xue, Int. Journ. Mod. Phys. D, 12, 173, (2003) Ruffini, Bianco, Chardonnet, Fraschetti, Vitagliano, Xue, “Cosmology and Gravitation”, AIP, (2003)

31. Arrival time ta vs. emission time t
Afterglow power-law slope for GRB :
Approximate ta computation:
Exact ta computation:
Observed slope: ± 0.067
(Halpern et al, 2000)
Ruffini, Bianco, Chardonnet, Fraschetti, Xue, Int. Journ. Mod. Phys. D, 12, 173, (2003) Ruffini, Bianco, Chardonnet, Fraschetti, Vitagliano, Xue, “Cosmology and Gravitation”, AIP, (2003)

32. Angular dispersion
Ruffini, Bianco, Chardonnet, Fraschetti, Xue, ApJ, 581, L19, (2002) Ruffini, Bianco, Chardonnet, Fraschetti, Vitagliano, Xue, “Cosmology and Gravitation”, AIP, (2003)

33. The Equitemporal Surfaces
Constant speed (r = vt):
Ellipsoids of constant eccentricity v/c
Numerical integration
General case:
Ruffini, Bianco, Chardonnet, Fraschetti, Xue, ApJ, 581, L19, (2002) Ruffini, Bianco, Chardonnet, Fraschetti, Vitagliano, Xue, “Cosmology and Gravitation”, AIP, (2003)

34. ABM Pulse visible area Invisible Visible
Ruffini, Bianco, Chardonnet, Fraschetti, Xue, ApJ, 581, L19, (2002) Ruffini, Bianco, Chardonnet, Fraschetti, Vitagliano, Xue, “Cosmology and Gravitation”, AIP, (2003)

35. The bolometric luminosity of the source
Where:
De = internal energy developed in the ABM - ISM collision.
L = g (1 - (v/c) cosJ)
Ruffini, Bianco, Chardonnet, Fraschetti, Xue, ApJ, 581, L19, (2002) Ruffini, Bianco, Chardonnet, Fraschetti, Vitagliano, Xue, “Cosmology and Gravitation”, AIP, (2003)

36. Arrival time ta vs. emission time t+ D R r a
1 £ g £ 310 t R D t a t t + D r g @ 4
Rees, Nature, 211, 468, (1966)
Ruffini, Bianco, Chardonnet, Fraschetti, Xue, ApJ, 555, L107, (2001) Ruffini, Bianco, Chardonnet, Fraschetti, Xue, Int. Journ. Mod. Phys. D, 12, 173, (2003) Ruffini, Bianco, Chardonnet, Fraschetti, Vitagliano, Xue, “Cosmology and Gravitation”, AIP, (2003)

37. Relativistic contraction or classical Doppler effect?
Doppler contraction:
where:
- g is the gamma Lorentz factor of the moving source, - T0 is the period of the radiation measured in the comoving frame, - T is the period of the radiation measured by an observer at rest.
The arrival time relation:
is then just a classical Doppler contraction and has nothing to do with special relativistic effects.

38. The initial conditions in the EMBH model:
The Dyadosphere +Q -Q
Preparata, Ruffini, Xue, 1998, A&A 338, L87
see also Ruffini, Vitagliano, Xue, in preparation + - + - + - + - + - + - + - + - + - + - + - + - + - + - + -
The initial conditions in the EMBH model:
e+e- plasma

39. R. Ruffini, J.A. Wheeler, “Introducing the Black Hole”, Physics Today, January 1971

40. Theoretical background of the EMBH model+ -
Heisenberg, Euler, 1935 Schwinger, 1951
Christodoulou, Ruffini, 1971
Damour & Ruffini 1974
In a Kerr-Newmann black hole vacuum polarization process occurs if 3.2MSun £ MBH £ 7.2·106MSun
Maximum energy extractable 1.8·1054 (MBH/MSun) ergs
“…naturally leads to a most simple model for the explanation of the recently discovered g-rays bursts”

41. Theoretical model
GRBs originate from the vacuum polarization process á la Heisenberg-Euler-Schwinger in the space-time surrounding a non-rotating electromagnetic black hole
Collision
PEMB pulse
ABM pulse
PEM pulse

42. Observations
Irregularity of temporal profile of single event and variability of temporal profile between different events
Bimodal distribution of duration
Observed spectrum non-thermal..

43. The g Lorentz factor
Ruffini, Bianco, Chardonnet, Fraschetti, Xue, ApJ, 555, L113, (2001) Ruffini, Bianco, Chardonnet, Fraschetti, Xue, Int. Journ. Mod. Phys. D, 12, 173, (2003) Ruffini, Bianco, Chardonnet, Fraschetti, Vitagliano, Xue, “Cosmology and Gravitation”, AIP, (2003)

44. Arrival time ta vs. emission time tD D D t a t + D t D t a t t + D r g @ 4
Dta = Dt
Ruffini, Bianco, Chardonnet, Fraschetti, Xue, ApJ, 555, L107, (2001) Ruffini, Bianco, Chardonnet, Fraschetti, Xue, Int. Journ. Mod. Phys. D, 12, 173, (2003) Ruffini, Bianco, Chardonnet, Fraschetti, Vitagliano, Xue, “Cosmology and Gravitation”, AIP, (2003)

45. GRB
BATSE noise threshold

46. The “Equitemporal” surfaces
Invisible region