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Testing the blast wave model with Swift GRBs Peter A. Curran Mullard Space Science Laboratory, UCL with RLC Starling, AJ van der Horst, A Kamble, RAMJ.

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Presentation on theme: "Testing the blast wave model with Swift GRBs Peter A. Curran Mullard Space Science Laboratory, UCL with RLC Starling, AJ van der Horst, A Kamble, RAMJ."— Presentation transcript:

1 Testing the blast wave model with Swift GRBs Peter A. Curran Mullard Space Science Laboratory, UCL with RLC Starling, AJ van der Horst, A Kamble, RAMJ Wijers, M de Pasquale & M Page

2 pre-Swift versus Swift GRBs

3 pre-Swift (GRB ) (Kuulkers et al. 2000) X-ray Optical

4 pre-Swift (GRB ) Swift era(GRB ) (Evans et al. 2007) (Kuulkers et al. 2000) X-ray Optical X-ray only pre-Swift versus Swift GRBs

5 pre-Swift (GRB ) Swift era(GRB ) (Evans et al. 2007) (Kuulkers et al. 2000) X-ray Optical pre-Swift versus Swift GRBs Does pre-Swift theory work? X-ray only

6 The blast wave model (CXC/M. Weiss)

7 The blast wave model (CXC/M. Weiss) k – circumburst density profile (ρ ~ r -k )

8 The blast wave model (CXC/M. Weiss) k – circumburst density profile (ρ ~ r -k ) q – continued energy injection index (E ~ t q )

9 The blast wave model (CXC/M. Weiss) p – electron energy distribution (Fermi; dN/dE ~ E -p ) k – circumburst density profile (ρ ~ r -k ) q – continued energy injection index (E ~ t q )

10 Synchrotron spectra (Sari et al. 1998)

11 Synchrotron spectra Optical / X-ray (Sari et al. 1998)

12 Derivation of p

13 α ➝ p( α, k,q) & accuracy of temporal fit ⇒ multiple options Derivation of p

14 α ➝ p( α, k,q) & accuracy of temporal fit ⇒ multiple options β opt ➝ p( β opt,E B-V ) ⇒ multiple options Derivation of p

15 α ➝ p( α, k,q) & accuracy of temporal fit ⇒ multiple options β opt ➝ p( β opt,E B-V ) ⇒ multiple options β X ➝ p( β X,N H ) ⇒ multiple options Derivation of p

16 α ➝ p( α, k,q) & accuracy of temporal fit ⇒ multiple options β opt ➝ p( β opt,E B-V ) ⇒ multiple options β X ➝ p( β X,N H ) ⇒ multiple options ⇒ above/below synchrotron cooling frequency Derivation of p

17 Sample of 10 Swift GRB afterglows

18 (GRB ) X-ray Optical

19 Consistent with the blast wave model? (GRB ) X-ray Optical Sample of 10 Swift GRB afterglows

20 Blast wave interpretations Compare possible multi-wavelength interpretations with blast wave †... ( † Nousek et al. 2006; Starling et al. 2008)

21 Blast wave interpretations Compare possible multi-wavelength interpretations with blast wave †... 8/10 consistent with blast wave 4/10 unambiguous jet breaks 6/10 calculated k 3/10 require q ; 3/10 don’t 6/10 unambiguous p 4 above cooling break 2 below cooling break ( † Nousek et al. 2006; Starling et al. 2008) (Curran et al. 2009)

22 k

23 Circumburst density profile, k (Curran et al. 2009)

24 Circumburst density profile, k Wind

25 (Curran et al. 2009) Wind ISM Circumburst density profile, k

26 (Curran et al. 2009) Wind ISM Circumburst density profile, k Not consistent with only one of ISM or Wind

27 q

28 Energy injection index, q (Curran et al. 2009) E ~ t q

29 Energy injection index, q (Curran et al. 2009) E ~ t q

30 Energy injection index, q (Curran et al. 2009) E ~ t q

31 Energy injection index, q (Curran et al. 2009) E ~ t q Required but inconclusive... so far

32 p

33 Distribution of p (Curran et al. 2009)

34 Distribution of p Not consistent with a single, universal value

35 Distribution of p

36 βXβX

37

38 Distribution of spectral index, β below cooling break above cooling break

39 Distribution of spectral index, β (Curran et al. in prep; data from Evans et al. 2009)

40 Distribution of spectral index, β (Curran et al. in prep; data from Evans et al. 2009)

41 Distribution of spectral index, β (Curran et al. in prep; data from Evans et al. 2009) Most X-rays above cooling break?

42 Conclusions 8 out of 10 GRBs favour the blast wave model* (*or at least don't disfavour it) k is not consistent with only one of ISM or Wind q is required in some bursts, inconclusive so far p is not consistent with a single, universal value Most X-rays above the cooling break?


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