Theoretical interpretation of GRB060124 preliminary results

Theoretical interpretation of GRB060124 preliminary results
Theoretical interpretation of GRB060124 preliminary results

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Theoretical interpretation of GRB060124:preliminary results.R.Guida ?,M.G.Bernardini,C.L.Bianco,L.Caito,M.G.Dainotti and R.Ru?ni Dipartimento di Fisica,Universit`a La Sapienza,Roma,00185,Italy ?E-mail:roberto.guida@icra.it www.icra.it We show the preliminary results of the application of our “?reshell”model to GRB060124.This source is very peculiar because it is the ?rst event for which both the prompt and the afterglow emission were observed simultaneously by the three Swift instruments:BAT (15?350keV),XRT (0.2?10keV)and UVOT (170?650nm),due to the presence of a precursor ~570s before the main burst.We analyze GRB060124within our “canonical”GRB scenario,identifying the precursor with the P-GRB and the prompt emission with the afterglow peak emission.In this way we reproduce correctly the energetics of both these two components.We reproduce also the observed time delay between the precursor (P-GRB)and the main burst.The e?ect of such a time delay in our model will be discussed.Keywords :Gamma rays:bursts –Black hole physics –Radiation mechanisms:thermal 1.GRB060124observational properties On 2006-01-24at 15:54:52UT,Swift-BAT triggered on the precursor of GRB060124,that occurred ~570s before the main burst peak.1This allowed Swift to immedi-ately re-point the narrow ?eld instruments (NFIs)and acquire a pointing towards the burst ~350s before the main burst occurred.The burst has a highly structured pro?le,comprising three major peaks following the precursor and has the longest duration (even excluding the precursor)ever recorded.2GRB060124also triggered Konus-Wind (10?770keV)3559.4s after the BAT trigger.4The Konus light curve con?rmed the presence of both the precursor and the three peaks of prompt emission.The prompt emission of GRB 060124was observed simultaneously by XRT with exceptional signal-to-noise (S/N)and was detected by UVOT at V =16.96±0.08(T +183s)and V =16.79±0.04(T +633s).1This fact makes it an exceptional test case to study prompt emission models,since this is the very ?rst case that the

burst could be observed with an X-ray CCD with high spatial resolution imaging down to 0.2keV.

2.The ?t

Within our “canonical GRB”scenario 5we identify the ?rst main pulse with the P-GRB and the three major peaks following the precursor with the afterglow peak emission.

We therefore obtain for the two parameters characterizing the source in our model E tot

e ±=3.73×1054erg and B =2.3×10?3.This implies an initial e ±plasma

created between the radii r 1=1.12×107cm and r 2=4.58×108cm with a total number of e ±pairs N e ±=1.46×1059and an initial temperature T =2.23MeV.

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))Detector arrival time (s)XRT observations in 0.2-10 keV band Theoretical fit in 0.2-10 keV band

Fig.1.The XRT light curve (0.2–10keV,red points)and the preliminary theoretical simulation in the same energy band (green line).The ?t is quite good,but the double peaked structure is not reproduced,due to the fact that our radial approximation for modeling the CBM is not valid anymore at the late time of the peaks (see text).

The theoretically estimated total isotropic energy emitted in the P-GRB is E P ?GRB =1.41%E tot

e ±=5.26×1052erg,in excellent agreement with the one

observed in the ?rst main pulse (E obs

P ?GRB ~6.00×1052erg in 15?350keV en-

ergy band),as expected due to their identi?cation.After the transparency point at r 0=4.76×1014cm from the progenitor,the initial Lorentz gamma factor of the ?reshell is γ0=430.The distribution of the CircumBurst medium has been parametrized assuming an average value for the e?ective density in the prompt phase of 10?2particle per cm 3and in the afterglow phase of 10?4particle per cm 3.Such a low e?ective density has been assumed in order to reproduce the ~500s of quiescence between the P-GRB and the prompt,according to the way in which the emission is produced within our model,that it will be clari?ed in the next session.

In Fig.1we present the preliminary theoretical ?t of the Swift XRT data (0.2–10keV),while in Fig.2of the BAT ones (15–350keV).The problems of the ?t will be discussed in the next section.

3.The CircumBurst 3D structure

Within our ?reshell model all the GRB emission after the transparency is produced by the interaction of the accelerated baryons with the CBM,and such interaction is modeled as inelastic collisions.6The number of such collisions,hence,depends on

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)Detector arrival time (s)P-GRB

BAT observations in 15-350 keV band

BAT observations in 15-350 keV band (precursor)Theoretical fit in 15-350 keV band

Fig.2.The BAT light curve in the 15?350keV band (red points)comprising also the precursor (green points)and our preliminary theoretical simulation in the same energy band (blue line).Clearly the energetics is well reproduced,but in order to have a good ?t of the peaks,a correct treatment of the 3-dimensional structure of the CBM is needed (see text).

the CBM density.

The simplest way to model the CBM structure is to assume that n cbm is a function only of the radial coordinate,n cbm =n cbm (r )(radial approximation).The CBM is arranged in spherical shells of width ~1015cm positioned in such a way that the modulation of the emitted ?ux coincides with the observed peaks.It is important to emphasize that,when the accelerated baryons collide with a shell,the increase in the ?ux is almost immediate due to the photons coming from the line of sight.Then it follows an exponential decrease of the ?ux due to the contribution of the photons emitted from di?erent angles.In this way we obtain the observed FRED structure for each peak,together with all the other observed peculiarities (hard to soft transition,spectral lag).

Clearly our radial approximation is valid until the visible area of the incoming baryons pulse is comparable with the characteristic dimensions of the clouds.The transverse dimension of such area is R T =r sin θ,where θ~1/γis the relativistic beaming angle,so we have R T ~r/γ.

We have found in many cases that this approximation cannot be valid during the whole prompt emission.In fact,when the accelerated baryons impact with dense clouds of CBM,they are decelerated and their gamma factor drops abruptly.In this situation,after the ?rst peaks (the number of peaks depending from their height,the higher they are the smaller their number is)the visible area becomes comparable

4

with the size of the clouds and our approximation is not valid anymore.This is case for other GRBs we analyzed,as GRB9912166and GRB0503157.

Another situation in which our radial approximation fails can occurs.Because the transverse dimension of the baryonic?reshell’s visible area,as outlined above, depends not only from the Lorentz gamma factor but also from the radius of the ?reshell,it can be that for very large value of this radial coordinate,the size of the visible area becomes comparable with the CBM clouds,that is,the approximation of spherical symmetric distribution for the CBM fails.

In all the GRB sources studied up to date,this have never been the case,because usually the radial coordinate r at which the prompt emission occurs is small.

It is important here to remember the fact that within our?reshell model,the initial instant of time t0(related to the initial value of the radial coordinate,r0= ct0)is often di?erent from the moment in which the satellite instrument triggers: in fact in our model the GRB emission starts at the transparency point when the P-GRB is emitted,but sometimes the P-GRB is under the instrumental threshold or comparable with it and so is not enough to trigger the instrument.For example in the case of GRB050315,a possible precursor was observed~50s before the trigger,8that indeed occurred when the main prompt emission started.

In this case instead the BAT instrument triggers on a precursor that we identify as the P-GRB because of the excellent agreement in terms of the energetics and of the time delay between it and the main prompt emission;so in this case our t0 coincides with the BAT trigger and the main prompt emission occurs at?T~600 s so at a value r=c?T for the radial coordinate of the?reshell;with this value of r the transverse dimension of the baryonic?reshell’s visible area is such that the radial approximation is not valid anymore.

In particular,we found that at t d a~600s,that is when the main burst oc-curs,the radius of the?reshell is r~1018cm and the Lorentz gamma factor has dropped abruptly to a value of~100from the initialγ0=430,due to the CBM cloud assumed to be present at the moment of the prompt emission.The transverse dimension of the visible area of the incoming baryons pulse indeed results R T~1016 cm,so even bigger then the characteristic dimensions of the CBM clouds usually assumed(from61014to1015cm),in this case~1015cm.

A correct treatment of the3-dimensional structure of the CBM clouds is needed in this case.

We have already tested this idea in order to explain an apparently physical di?erent feature of the GRBs:the?ares.This phenomenon has been discovered to occurs in the early part of the X-ray afterglow,that means very late from the satellite trigger and very far.From our point of view,there are no di?erences between a?are and the prompt emission in this case,that has occurred at600s.

Many interpretations have been provided in order to explain the?ares.The most common explanation is a central engine activity which results in internal shocks(or similar energy dissipation events)at later times9.Another possibility is emission from reverse shock,but the predicted amplitude is too low to interpret all

5 the cases9,10.Alternatively such emission could be produced by a multi-component jet11–13:the X-ray?are is caused by the deceleration of the wider cocoon component with the ambient medium.In this case,however,the decay after the peak should follow the standard afterglow model,so it cannot interpret the observed rapid fall-o?in the?ares9.The same problem9a?ects also the scenario in which the?are is produced by the energy injection into the decelerating shell by the collision with a high-γshell14.

Within our?reshell model the?ares are interpreted as being due to the same process responsible for the following afterglow emission.So the di?culties to?t them are due to the radial approximation,not valid anymore at such late time(or at such big value of the radial coordinate).

We tested our idea of abandoning the radial approximation and introducing a3-dimensional structure of the CBM clouds in order to?t the?are(occurred at~250 s)of GRB01112115,16,an old burst observed by Beppo SAX which for the?rst time showed the feature of an X-ray?are.We obtain good results that demonstrate at least the validity of such proposal.Anyway the implementation of a such description of the CBM clouds is not yet?nished,but we are currently working on it.

4.Conclusion

We applied the?reshell model to GRB060124.The work is not?nished yet and we showed only the preliminary results.The main peculiarity of this source is the biggest ever recorded time delay between the precursor and the prompt emission. We reproduced correctly the energetics of the precursor,identi?ed with the P-GRB, and of the prompt emission,identi?ed with the extended afterglow peak emission.

The most important consequence of having such a big time delay between P-GRB and afterglow peak is that the radial approximation assumed in modeling the CBM structure is not valid anymore at the time of the prompt emission.For this reason our model failed in reproducing the narrow two peaks of the prompt emission.Our peaks,in particular the second,resulted much more spread.

In order to have a good?t of the light curves,we have to change our way of modeling the CBM structure.We have to take into account the fact that only a part of the visible area of the?reshell interacts with the CBM cloud.This is only possible introducing a3-dimensional structure of the clouds,that will mean to introduce a new parameter.In this way we will obtain narrow peaks also for big values of the ?reshell radius.

We have already successfully applied this idea in order to?t the?are of GRB011121,that is a bump of an order of magnitude in luminosity,lasting for20 s,occurred after250s from the trigger.The likeness of this?are with the prompt emission of GRB060124,a short bump of an order of magnitude in luminosity oc-curred at very late time as well,is evident:so we expect to obtain also in this case the same good agreement we had in the case of GRB011121.

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