Are GRB 980425 and GRB 031203 real outliers or twins of GRB 060218?

Ghisellini, G.; Ghirlanda, G.; Mereghetti, S.; Bošnjak, Ž.; Tavecchio, F.; Firmani, C.

doi:10.1111/j.1365-2966.2006.10972.x

Cited by 84 publications

(97 citation statements)

References 46 publications

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“…Clearly, our result is much more accurate. Actually, the value Γ m in (120) is obtained from equating asymptotes in (126) and there exists the following relation:…”

Section: Approximate Resultsmentioning

confidence: 99%

The Blackholic energy and the canonical Gamma-Ray Burst

Ruffini¹,

Bernardini²,

Bianco³

et al. 2007

AIP Conference Proceedings

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Abstract. Gamma-Ray Bursts (GRBs) represent very likely "the" most extensive computational, theoretical and observational effort ever carried out successfully in physics and astrophysics. The extensive campaign of observation from space based X-ray and γ-ray observatory, such as the Vela, CGRO, BeppoSAX, HETE-II, INTEGRAL, Swift, R-XTE, Chandra, XMM satellites, have been matched by complementary observations in the radio wavelength (e.g. by the VLA) and in the optical band (e.g. by VLT, Keck, ROSAT). The net result is unprecedented accuracy in the received data allowing the determination of the energetics, the time variability and the spectral properties of these GRB sources. The very fortunate situation occurs that these data can be confronted with a mature theoretical development. Theoretical interpretation of the above data allows progress in three different frontiers of knowledge: a) the ultrarelativistic regimes of a macroscopic source moving at Lorentz gamma factors up to ∼ 400; b) the occurrence of vacuum polarization process verifying some of the yet untested regimes of ultrarelativistic quantum field theories; and c) the first evidence for extracting, during the process of gravitational collapse leading to the formation of a black hole, amounts of energies up to 10 55 ergs of blackholic energy -a new form of energy in physics and astrophysics. We outline how this progress leads to the confirmation of three interpretation paradigms for GRBs proposed in July 2001. Thanks mainly to the observations by Swift and the optical observations by VLT, the outcome of this analysis points to the existence of a "canonical" GRB, originating from a variety of different initial astrophysical scenarios. The communality of these GRBs appears to be that they all are emitted in the process of formation of a black hole with a negligible value of its angular momentum. The following sequence of events appears to be canonical: the vacuum polarization process in the dyadosphere with the creation of the optically thick self accelerating electron-positron plasma; the engulfment of baryonic mass during the plasma expansion; adiabatic expansion of the optically thick "fireshell" of electronpositron-baryon plasma up to the transparency; the interaction of the accelerated baryonic matter with the interstellar medium (ISM). This leads to the canonical GRB composed of a proper GRB (P-GRB), emitted at the moment of transparency, followed by an extended afterglow. The sole parameters in this scenario are the total energy of the dyadosphere E dya , the fireshell baryon loading M B defined by the dimensionless parameter B ≡ M B c 2 /E dya , and the ISM filamentary distribution around the source. In the limit B → 0 the total energy is radiated in the P-GRB with a vanishing contribution in the afterglow. In this limit, the canonical GRBs explain as well the short GRBs. In these lecture notes we systematically outline the main results of our model comparing and contrasting them with the ones in the current literature. In both cases, we have li...

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“…Clearly, our result is much more accurate. Actually, the value Γ m in (120) is obtained from equating asymptotes in (126) and there exists the following relation:…”

Section: Approximate Resultsmentioning

confidence: 99%

The Blackholic energy and the canonical Gamma-Ray Burst

Ruffini¹,

Bernardini²,

Bianco³

et al. 2007

AIP Conference Proceedings

View full text Add to dashboard Cite

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“…3 of Ramirez-Ruiz et al 2005). We also note that for GRBs 980425 and 031203 Ghisellini et al (2006) have recently suggested two other possible scenarios that may cause such a deviation from the Amati relation. One is that the GRB radiation may have passed through a scattering screen, and the other is that we may have missed softer emission from the GRBs that lasts much longer.…”

Section: Comparisonmentioning

confidence: 96%

Prompt and Afterglow Emission Properties of Gamma-Ray Bursts with Spectroscopically Identified Supernovae

Kaneko¹,

Ramirez-Ruiz²,

Granot³

et al. 2006

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We present a detailed spectral analysis of the prompt and afterglow emission of four nearby long-soft gamma-ray bursts (GRBs 980425, 030329, 031203, and 060218) that were spectroscopically found to be associated with Type Ic supernovae and compare them to the general GRB population. For each event, we investigate the spectral and luminosity evolution and estimate the total energy budget based on broadband observations. The observational inventory for these events has become rich enough to allow estimates of their energy content in relativistic and subrelativistic form. The result is a global portrait of the effects of the physical processes responsible for producing long-soft GRBs. In particular, we find that the values of the energy released in mildly relativistic outflows appears to have a significantly smaller scatter than those found in highly relativistic ejecta. This is consistent with a picture in which the energy released inside the progenitor star is roughly standard, while the fraction of that energy that ends up in highly relativistic ejecta outside the star can vary dramatically between different events.

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“…This is particularly significant, since GRB 060218 is the only source in such a class to have an excellent data coverage without gaps. We are currently examining if the missing data in the other sources of such a class may have a prominent role in their nonfulfillment of the Amati et al (2002) relation (Dainotti et al, in preparation;Ghisellini et al 2006).…”

Section: Discussionmentioning

confidence: 99%

GRB 060218 and GRBs associated with supernovae Ib/c

Dainotti¹,

Bernardini²,

Bianco³

et al. 2007

A&A

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Context. The Swift satellite has given continuous data in the range 0.3-150 keV from 0 s to 10 6 s for GRB 060218 associated with SN2006aj. This Gamma-Ray Burst (GRB) which has an unusually long duration (T 90 ∼ 2100 s) fulfills the Amati relation. These data offer the opportunity to probe theoretical models for GRBs connected with Supernovae (SNe). Aims. We plan to fit the complete γ-and X-ray light curves of this long duration GRB, including the prompt emission, in order to clarify the nature of the progenitors and the astrophysical scenario of the class of GRBs associated with SNe Ib/c. Methods. We apply our "fireshell" model based on the formation of a black hole, giving the relevant references. It is characterized by the precise equations of motion and equitemporal surfaces and by the role of thermal emission. Results. The initial total energy of the electron-positron plasma E tot e ± = 2.32 × 10 50 erg has a particularly low value, similar to the other GRBs associated with SNe. For the first time, we observe a baryon loading B = 10 −2 which coincides with the upper limit for the dynamical stability of the fireshell. The effective CircumBurst Medium (CBM) density shows a radial dependence n cbm ∝ r −α with 1.0 < ∼ α < ∼ 1.7 and monotonically decreases from 1 to 10 −6 particles/cm 3 . This behavior is interpreted as being due to a fragmentation in the fireshell. Analogies with the fragmented density and filling factor characterizing Novae are outlined. The fit presented is particularly significant in view of the complete data set available for GRB 060218 and of the fact that it fulfills the Amati relation. Conclusions. We fit GRB 060218, usually considered as an X-Ray Flash (XRF), as a "canonical GRB" within our theoretical model. The smallest possible black hole, formed by the gravitational collapse of a neutron star in a binary system, is consistent with the especially low energetics of the class of GRBs associated with SNe Ib/c. We provide the first evidence for a fragmentation in the fireshell. This fragmentation is crucial in explaining both the unusually large T 90 and the consequently inferred abnormally low value of the CBM effective density.

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Are GRB 980425 and GRB 031203 real outliers or twins of GRB 060218?

Cited by 84 publications

References 46 publications

The Blackholic energy and the canonical Gamma-Ray Burst

The Blackholic energy and the canonical Gamma-Ray Burst

Prompt and Afterglow Emission Properties of Gamma-Ray Bursts with Spectroscopically Identified Supernovae

GRB 060218 and GRBs associated with supernovae Ib/c

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