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Workshop: Kinetic physics of astrophysical plasmas

18–20 mai 2026
Montpellier
Fuseau horaire Europe/Paris

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Contributions

30 sur 30 affichés
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  1. 31. Welcome & coffee
    18/05/2026 09:30
  2. 34. Magnetized turbulence and dynamos in compact objects
    Dr Alexis Reboul-Salze (Max-Planck Institute for Gravitational Physics)
    18/05/2026 10:00

    Turbulence plays a fundamental role in the transfer, amplification, and dissipation of magnetic and kinetic energy in astrophysical plasmas, from the solar corona to the vicinity of compact objects. In compact objects, including neutron stars, neutron star merger remnants and black-hole accretion flows, turbulent motions are crucial as they drive angular momentum transport, magnetic...

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  3. 35. Contribution 1
    18/05/2026 10:40
  4. 36. TBA
    Dr Yohan Dubois (IAP)
    18/05/2026 11:30
  5. 38. Cosmic-ray propagation in our Galaxy: Insights from the diffuse emission, TeV halos and the CR anisotropy
    Dr Gwenael Giacinti (APC Paris)
    18/05/2026 14:00

    Gamma-ray observations provide important information on cosmic-ray (CR) propagation in our Galaxy.
    First, we present a new model of CR propagation in the Milky Way, where CRs are injected at discrete transient sources in the disc. We then calculate the corresponding diffuse Galactic gamma-ray emission. We find that the diffuse gamma-ray emission at >~ 100 TeV is very clumpy, and does not...

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  6. 39. Contribution 2
    18/05/2026 14:40
  7. 40. TBA
    Dr Pierre Lesaffre (CNRS/LEPNS)
    18/05/2026 15:30
  8. 41. Contribution 3
    18/05/2026 16:10
  9. 42. Discussion
    18/05/2026 16:30
  10. 43. TBA
    Dr Pierre Cristofari (Observatoire de Paris)
    19/05/2026 09:30
  11. 44. Contribution 4
    19/05/2026 10:10
  12. 45. Does the Bohm limit determine the maximum of energy of shock-accelerated cosmic rays?
    Prof. Tony Bell (University of Oxford)
    19/05/2026 11:00

    Ever since the classic papers of Lagage & Cesarsky (1983) and Hillas (1984), the Bohm limit uBR has been taken as the measure of the maximum energy to which cosmic rays can be accelerated by shocks. The obvious problem in the 1980s was that the Bohm limit for supernova remnants fell well short of the knee in the spectrum at a few PeV. This problem appeared to be solved when fields of a few...

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  13. 47. Contribution 5
    19/05/2026 12:00
  14. 32. Presentation of the COST action
    Dr Anna Grassi (LULI), Arno Vanthieghem (Observatoire de Paris)
    19/05/2026 14:00
  15. 51. Highlight Talk
    Dr Alexis Marret (SLAC)
    19/05/2026 14:30
  16. 48. TBA
    Dr Gaëtan Fichet de Clairfontaine (University of Würzburg)
    19/05/2026 15:10
  17. 49. Contribution 6
    19/05/2026 16:20
  18. 50. Discussion
    19/05/2026 16:40
  19. 52. TBA
    Dr Pierre Henri ((1) Laboratoire Lagrange, Observatoire Côte d'Azur, Université Côte d'Azur, CNRS, Nice, France & (2) LPC2E, CNRS, Univ. Orléans, CNES, Orléans, France)
    20/05/2026 09:15
  20. 53. Contribution 7
    20/05/2026 09:55
  21. 54. Contribution 8
    20/05/2026 10:15
  22. 55. TBA
    Dr Sophie Masson (LPP - Observatoire de Paris)
    20/05/2026 11:05
  23. 57. Contribution 9
    20/05/2026 12:05
  24. 58. TBA
    Dr Nicolas Aunai
    20/05/2026 14:00
  25. 59. TBA
    Dr Valentin Brunn (Arcetri Observatory)
    20/05/2026 14:40
  26. 60. Discussion
    20/05/2026 15:30
  27. 33. End of the workshop
    20/05/2026 16:30
  28. 56. Contribution 11
  29. 37. contribution 2
  30. 46. Contribution 6