Why are x-rays crucial to investigate particle acceleration ? Why are x-rays crucial to investigate particle acceleration ?


НазваWhy are x-rays crucial to investigate particle acceleration ? Why are x-rays crucial to investigate particle acceleration ?
Дата конвертації26.04.2013
Розмір445 b.
ТипПрезентации











Why are X-rays crucial to investigate particle acceleration ?

  • Why are X-rays crucial to investigate particle acceleration ?

  • Physics of the synchrotron emission of the electrons accelerated at the highest energy

  • Physics of the thermal gas

    • Global parameters of the remnant : => downstream density => ambient density
    • Back-reaction of accelerated ions (protons)
  • Capability of performing spatially-resolved spectroscopy at small scale (< 10 arcsec)



The magnetic field is a crucial parameter :

  • The magnetic field is a crucial parameter :

  • for understanding particle acceleration

  • for deriving the maximum energy of accelerated particles

  • for interpreting the origin of TeV -rays : leptonic versus hadronic



Spectrum of the synchrotron emission (radio + X-rays)

  • Spectrum of the synchrotron emission (radio + X-rays)

  • Measurement of the rolloff photon energy hνroll, observable in X-rays

  • +

  • Estimate of downstream magnetic field

  • Estimate of the maximum energy of accelerated electrons :

  • Emax = 39 (hνroll / B10)1/2 TeV ~ few 10 TeV



Spatially resolved spectroscopy of the synchrotron emission

  • Spatially resolved spectroscopy of the synchrotron emission

  • Measurement of the azimuthal variation of νroll along the SNR shock

  • SN 1006: very strong variations ( hνroll up to 5 keV), which cannot be explained by variations of the magnetic compression alone.

  • => Maximum energy of accelerated particles must be higher at the bright limbs than elsewhere



Curvature of the spectrum :

  • Curvature of the spectrum :

  • indications in a few SNRs

  • SN 1006: combining radio and X-ray data

  • (Allen et al. 08)

  • RCW 86: combining radio and X-ray data

  • (Vink et al. 06)

  • Cas A: from infrared data

  • (Jones et al. 03)

  • Tycho and Kepler: from radio data

  • (Reynolds & Ellison 92)









Shock physics

  • Shock physics

  • High post-shock oxygen temperature in SN 1006 (XMM-Newton/RGS, Vink et al. 03)

  • kTO ~ 528 ± 150 keV and kTe ~ 1.5 keV => small degree (5%) of e-/ion equilibration at the shock

  • Low density ambient medium for

  • the SN Ia remnants:

  • G330.2+1.0: n0 ~ 0.1 cm-3, Park et al. 09

  • SNR 0509-67.5 n0 < 0.6 cm-3, Kosenko et al. 08

  • Tycho: n0 < 0.6 cm-3, Cassam-Chenaï et al. 07

  • SN 1006: n0 < 0.05 cm-3, Acero et al. 07

  • the core collapse remnant RXJ1713.7-3946: n0 < 0.02 cm-3, Cassam-Chenaï et al. 04b

  • => impact the level of pion decay emission in the TeV range due to proton-proton collisions

  • Stellar wind environment for the core collapse SNR Cas A: proper motion and morphology, Patnaude et al. 09

  • Sub-solar abundances in the Magellanic clouds (Borkowski et al. 06, 07, …)



A new class of Type Ia supernova ?

  • A new class of Type Ia supernova ?

  • Dense Fe-rich ejecta in DEM L238 and DEM L249 in the LMC

  • substantial amounts of CSM ? Remnant of prompt Type Ia SN with young progenitors ?

  • (Borkowski et al. 06)

  • Kepler’s SNR: iron emission, absence of oxygen and optical evidence of CSM.

  • SN Ia explosion in a more massive progenitor ?

  • (Reynolds et al. 07)



Presence of Cr and Mn K lines in the X-ray spectrum of young SNRs

  • Presence of Cr and Mn K lines in the X-ray spectrum of young SNRs

  • W49 B (ASCA, Hwang et al. 00, XMM-Newton Miceli et al. 06)

  • Tycho (Suzaku, Tamagawa et al. 09)

  • Cas A, Kepler (Cr only, Chandra, Yang et al. 09)













Strength of current X-ray observatories :

  • Strength of current X-ray observatories :

  • Spatially resolved spectroscopy at small spatial scale

  • High resolution spectroscopy

  • Needs for large programs to get sufficient statistics at the spatial, spectral and temporal scales relevant to the processes at work in SNRs.

  • Needs for mission extension of the current X-ray observatories as long as they give satisfaction, pending and preparing the future international X-ray observatory IXO.



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