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Radiation spectra from relativistic electrons moving in turbulent magnetic fields

Radiation spectra from relativistic electrons moving in turbulent magnetic fields. Ｙｕｔｏ Ｔｅｒａｋｉ & Fumio Takahara Theoretical A strophysics Group Osaka Univ., Japan. The distribution of lower energy spectral index of Band function. Line of Death. The number of GRB. Standard scenario.

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Radiation spectra from relativistic electrons moving in turbulent magnetic fields

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  1. Radiation spectra from relativistic electrons moving in turbulent magnetic fields Ｙｕｔｏ Ｔｅｒａｋｉ & Fumio Takahara Theoretical Astrophysics Group Osaka Univ., Japan Raleigh

  2. The distribution of lower energy spectral index of Band function Line of Death The number of GRB Standard scenario Internal shock Synchrotron radiation Many GRB don’t suit Synchrotron theory! (low energy Spectral index) Kaneko et al 2006 BATSE Raleigh

  3. Weibel instability near the S.F. Shock Front PIC simulationby Sironi & Spitkovsky ‘09 Turbulent magnetic field Raleigh

  4. What decide spectrum shape ? Synchrotron Ｅ（ｔ） ・ ｔ Fourier transform spectrum →synchrotron spectrum. Observed pulse Beaming Synchrotron radiation or not Electrons can trace gyro motion in or not. Raleigh

  5. ? Which is larger, or We focus on the Weibel instability. is the order of . Proportional coefficient The relative Lorentz factor of shells where Plasma frequency Lorentz factor which generate the turbulent field : typical value from PIC. synchrotron radiation Jitter radiation Intensive study is required ! Raleigh

  6. The missing link spectrum In this work, we reveal this unknown spectrum. Raleigh

  7. Model of turbulent fields 3D turbulent magnetic field Kolmogorov type. : mean value of B Define by Raleigh

  8. E.O.M. and radiation spectrum. Example of trajectory Equation of motion we calculate. and Radiation spectrum is calculated using Lienard-Wiechert potential. Unit vector points observer Retarded time Raleigh

  9. In case of (3D jitter radiation) where Normalized by Vertical axis: Flux Horizontal axis: Normalized frequency Break1 Break1 Raleigh

  10. In case of where Break 2 The low frequency region becomes hard. Raleigh

  11. The spectrum in the case of Raleigh

  12. In case of Raleigh

  13. In this case spectrum is harder than synchrotron theory predict. ! ! Ｃｏｎｓｉｓｔｅｎｔ The value of of near the GRB internal shock front Ｔhe harder spectral index of GRB prompt emission than synchrotron is naturally explained. Raleigh

  14. SUMMARY • We calculate radiation spectra from electrons moving in turbulent magnetic fields by using first principle numerical simulation. • The radiation spectrum in case of was not known precisely, we reveal it clearly. • We get harder spectrum than synchrotron which power index is up to in the case of which is in the range of predicted value of near the GRB internal shock front by PIC simulations. Raleigh

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