We analyze the data of the Gamma-Ray Burst/Supernova GRB030329/SN2003dh
system obtained by HETE-2 (GCN [1]), R-XTE (GCN [2]), XMM (Tiengo et al. [3])
and VLT (Hjorth et al. [4]) within our theory (Ruffini et al. [5] and
references therein) for GRB030329. By fitting the only three free parameters of
the EMBH theory, we obtain the luminosity in fixed energy bands for the prompt
emission and the afterglow (see Fig.1). Since the Gamma-Ray Burst (GRB)
analysis is consistent with a spherically symmetric expansion, the energy of
GRB030329 is E = 2.1 * 10^{52} erg, namely ~ 2 * 10^3 times larger than the
Supernova energy. We conclude that either the GRB is triggering an
induced-supernova event or both the GRB and the Supernova are triggered by the
same relativistic process. In no way the GRB can be originated from the
supernova. We also evidence that the XMM observations (Tiengo et al. [3]), much
like in the system GRB980425/SN1998bw (Ruffini et al. [6], Pian et al. [7]),
are not part of the GRB afterglow, as interpreted in the literature (Tiengo et
al. [3]), but are associated to the Supernova phenomenon. A dedicated campaign
of observations is needed to confirm the nature of this XMM source as a newly
born neutron star cooling by generalized URCA processes.Comment: 4 pages, 1 figure, to appear in the Proceedings of the Los Alamos
  "Gamma Ray Burst Symposium" in Santa Fe, New Mexico, September 8-12 2003 (AIP
  Conf. Ser.), CHAPTER: GRB03032

Bernardini, M. G.

Bianco, C. L.

Chardonnet, P.

Fraschetti, F.

Ruffini, R.

Xue, S. -S.

English

arXiv

M. G. Bernardini

Crossref

A New Astrophysical “Triptych”: GRB030329/SN2003dh/URCA-2

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A New Astrophysical “Triptych”:
GRB030329/SN2003dh/URCA-2
M.G. Bernardini∗, C.L. Bianco∗, P. Chardonnet†, F. Fraschetti∗∗, R.
Ruffini∗ and S.-S. Xue∗
∗ICRA - International Center for Relativistic Astrophysicsand Dipartimento di Fisica, Università
di Roma “La Sapienza”, Piazzale Aldo Moro 5, I-00185 Roma, Itly.
†Université de Savoie, LAPTH - LAPP, BP 110, F-74941 Annecy-l-Vieux Cedex, France.
∗∗Università di Trento, Via Sommarive 14, I-38050 Povo (Trento), Italy.
Abstract. We analyze the data of the Gamma-Ray Burst/Supernova GRB030329/SN2003dh sys-
tem obtained by HETE-2 (gcn [1]), R-XTE (gcn [2]), XMM (Tiengo et al. [3]) and VLT (Hjorth
et al. [4]) within our theory (Ruffini et al. [5] and references therein) for GRB030329. By fitting the
only three free parameters of the EMBH theory, we obtain the luminosity in fixed energy bands for
the prompt emission and the afterglow (see Fig. 1). Since theGamma-Ray Burst (GRB) analysis is
consistent with a spherically symmetric expansion, the energy of GRB030329 isE = 2.1×1052 erg,
namely∼ 2×103 times larger than the Supernova energy. We conclude that either the GRB is trig-
gering an induced-supernova event or both the GRB and the Suprnova are triggered by the same
relativistic process. In no way the GRB can be originated from the supernova. We also evidence
that the XMM observations (Tiengo et al. [3]), much like in the system GRB980425/SN1998bw
(Ruffini et al. [6], Pian and et al. [7]), are not part of the GRBafterglow, as interpreted in the liter-
ature (Tiengo et al. [3]), but are associated to the Supernova phenomenon. A dedicated campaign
of observations is needed to confirm the nature of this XMM source as a newly born neutron star
cooling by generalized URCA processes.
A distinctive feature of our model, developed in the framework f the three interpre-
tational paradigms (Ruffini et al. [8, 9, 10]), has been the relation between the photon
arrival time at the detectortda and the photon emission timet (see Ruffini et al. [5, 9, 11]):
tda = (1+z)
(
t−
∫ t
0 v(t
′)dt′+ r⋆
c
cosϑ +
r⋆
c
)
, (1)
wherer(t), v(t) andγ(t) are the radial coordinate, the velocity and the Lorentz gamm
factor of the expanding shell,r⋆ = r(t = 0), ϑ is the angle between the velocity of the
emission point of the photon and the line of sight andz is the cosmological redshift of
the source.
In contrast with the relation betweentda and t used in the literature, which depends
on an instantaneous value of the Lorentzγ factor (see e.g. Rees and Mészáros [12],
Eq.(30) in Piran [13]], Eq.(2) in van Paradijs et al. [14], Eq.(2) in Mészáros [15]), Eq.(1)
contains an integral which is a function of all previous values of the Lorentz gamma
factor along the source world-line since the timet = 0. Therefore the knowledge of the
Equations Of Motion (EOM) of the source is crucial to the evaluation of Eq.(1). In turns
all the quantities which are computed using the EQuiTemporal Surfaces (EQTS, Ruffini
et al. [5, 11], Bianco and Ruffini [16]) determined from Eq.(1) become themselves very
1036
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1040
1042
1044
1046
1048
1050
10-2 100 102 104 106 108 1010 1012 1014 1016
10-18
10-16
10-14
10-12
10-10
10-8
10-6
Lu
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 p
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 u
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 (
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)
O
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d 
flu
x 
(e
rg
s/
(c
m
2 *
s)
)
Detector arrival time (ta
d) (s)
Neutrino, kaon, pion cooling
2-10 keV
30-400 keV
HETE data (30-400 keV)
RXTE data (2-10 keV)
SN2003dh optical data
XMM data (0.2-10 keV)
FIGURE 1. The dotted line represents our theoretically predicted GRB030329 light curve inγ-rays
(30-400 keV) with the horizontal bar corresponding to the mean peak flux from HETE-2 (gcn [1]). The
solid line represents the corresponding one in X-rays (2-10keV) with the experimental data obtained by
R-XTE (gcn [2]). The remaining points refer respectively tothe optical VLT data (Hjorth et al. [4]) of
SN2003bw and to the X-ray XMM data (Tiengo et al. [3]) of URCA-2. The dash-dotted lines corresponds
to cooling theoretical curves of young neutron stars by generaliz d URCA processes. It is interesting to
compare and contrast these results with the ones for GRB980425/SN1998bw (see Fig. 3 in Ruffini et al.
[6])
sensitive functions of the EOM. This includes the slope of the afterglow (Ruffini et al.
[5]), which is essential in assessing the possible presenceof beaming in the source
(Ruffini et al. [17]), the luminosity in fixed energy bands andthe spectral analysis
(Ruffini et al. [18]).
The determination of the EOM leads to a quite complex treatmen , which starts from a
very special set of initial conditions, proven to be unique.This treatment fits the observed
luminosities with a large number of redundancy checks on theEOM (see Fig. 1). It fits as
well the time variability in the prompt radiation self-consistently with the determination
of the EOM [19].
We have adopted a spherically symmetric distribution for the GRB source and, as
initial conditions att = 10−21 s, ane+-e−-photon neutral plasma lying between the
radii r1 = 2.9× 106 cm andr2 = 9.0× 107 cm. The temperature of such a plasma is
2.1 MeV, the total energyEtot = 2.1×1052 erg and the total number of pairsNe+e− =
1.1× 1057. These conditions have been derived evaluating the vacuum polarization
processes (Damour and Ruffini [20]) occurring in the dyadosphere of an EMBH (Ruffini
[21], Preparata et al. [22], Cherubini et al. [23], Ruffini and Vitagliano [24, 25], Ruffini
et al. [26]). The total energyEtot coincides with the dyadosphere energyEdyawhich is the
first independent parameter of the EMBH theory. The optically thick electron-positron
plasma created in the dyadosphere self-propels itself outward reaching ultrarelativistic
velocities (Ruffini et al. [27]) and then interacts with the baryonic matter of the remnant
of the progenitor star. The baryonic matter componentMB is the second free parameter
of the EMBH theory:B= MBc2/Edya= 4.8×10−3. Thee+-e−-photon-baryon plasma
by further expansion becomes optically thin (Ruffini et al. [28]). As the transparency
condition is reached, the Proper-GRB (P-GRB) is emitted with an extremely relativistic
shell of Accelerated Baryonic Matter (the ABM pulse) with initial Lorentz gamma factor
of γ = 183.6. It is this ABM pulse which produces the afterglow through its interaction
with the ISM, whose average density is best fitted by< nism>= 1 particle/cm3. In such
a collision the “fully radiative condition” is implemented(for details see Ruffini et al.
[5]): the internal energy∆Eint which results is instantaneously radiated away.
We have recently assumed that the radiation emitted in the collision between the
ABM pulse and the ISM has a thermal spectrum measured in the ABM pulse comov-
ing frame (Ruffini et al. [18]). In our approach the source luminosity is derived from an
infinite set of foliations of events on the EQTS, each one characte ized by a different
thermal spectrum in the comoving frame boosted by a different r lativistic transforma-
tion obtained from the EOM. The third free parameter of the EMBH theory describes
this process of generating the thermal spectrum in the comoving frame. It is given by
1.1× 10−7 < R= Ae f f/Aabm< 5.0× 10−11, whereAabm is the ABM pulse external
surface area andAe f f is the ABM pulse effective emitting area.
We can then obtain for the GRB030329 the luminosities in given energy bands,
computed in the range 2-400 keV with very high accuracy. Fig.1 shows the results for
the luminosities in the 30-400 keV and 2-10 keV bands. Subsequently, the theoretically
predicted GRB spectra have been evaluated at selected values of the arrival time [19].
We can now compare these results with those for GRB980425/SN1998bw (Ruffini
et al. [6]). We conclude that:
a) The intensity of the GRB versus the Supernova, comparablein the case of
GRB980425, becomes 2×103 times larger in the case of GRB030329. This crucial fact
clearly indicates beyond any doubt the independence of the GRB phenomenon from the
Supernova (Ruffini et al. [10]). Moreover, the GRB is generally energetically dominant
on the supernova; either the GRB is triggering an induced-supernova event or both the
GRB and the Supernova are triggered by the same relativisticpro ess. In no way the
GRB can originate from the supernova.
b) In both systems the XMM observations point to the existence of an additional
X-ray source, which we consider related to the Supernova phenom non and not to the
GRB. There is the distinct possibility that this source originates from the emission of a
newly formed hot neutron star, cooling via generalized URCAprocesses (Ruffini et al.
[6]). It has been recently proposed (Ruffini et al. [29]) to indicate this new physical
and astrophysical systems as URCA-1 for GRB980425/SN1998bw and URCA-2 for
GRB030329/SN2003dh. A dedicated campaign of observationswith XMM is urgently
needed in order to explore this unprecedented “triptych” astrophysical systems, formed
by a GRB, an induced-supernova and possibly a newly born pulsating hot neutron star.
Details of this results are going to be published in [19].
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M. G. BERNARDINI

P. CHARDONNET

F. FRASCHETTI

R. RUFFINI

S. S. XUE

BIANCO, Carlo Luciano

Archivio della ricerca- Università di Roma La Sapienza

http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.255.1534

A New Astrophysical "Triptych": GRB030329/SN2003dh/URCA-2

A New Astrophysical "Triptych": GRB030329/SN2003dh/URCA-2

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