Talks and posters

• 5 review + 5 highlight talks (invited talks), 1 summary talk
  
• 35 contributed talks
  
• 1 poster session

 → slides available at https://zenodo.org/search?page=1&size=20&q=crism2018or download all slides at once from https://mycore.core-cloud.net/index.php/s/QKdgoeDjpFlPX7a/download

Group photo

→ see here (© Siddhartha Gupta)

Cosmic rays (CRs) are a major component of the interstellar medium (ISM), their energy density is similar to that of the gas and the magnetic field:

• Low-energy CRs (kinetic energies < 1 GeV) play an active role in the ISM dynamics through their pressure gradient at galactic and possibly at smaller scales. They contribute to ionization and heating of the ISM, especially in dense, optically thick, media where UV and X-ray photons cannot penetrate; CR ionization is the main process to couple matter and magnetic field and likely has an important impact on star and planet formation processes. Low-energy CRs can also self-trigger magnetic perturbations and small-scale magnetic turbulence via various kinetic plasma instabilities; this determines their residence timescale and the local matter ionization level.

• High-energy CRs (kinetic energies > 1-10 GeV) can be acelerated in strong collisionless shock waves in supernova remnants (SNR), and this can be tested by multi-wavelength observations from radio to gamma-ray frequencies. High-energy CRs escape from their sources and travel to Earth by a succession of random walks controlled by the ISM turbulence. Direct CR detection by balloon, satellite, and ground experiments start to unveil this diffusive transport up to PeV energies and beyond. CRs interact with the  interstellar gas to produce GeV gamma rays, electrons, positrons, antiprotons, and neutrinos. A good knowledge of the gas and magnetic field distribution combined with a mapping of diffuse CR background radiation are essential to claim any dark matter detection.

CRs physics is a key ingredient for both the local and global ISM dynamics. However, its integration in the modeling of the multi-scale ISM evolution is still a recent development in the field. The main objective of the CRISM international workshop is to contribute to a better review and understanding of the multiple effects of the energetic component of the ISM.

1. CR sources: acceleration mechanisms, multi-wavelength observations, possible sources (supernova remnants, pulsar winds, stellar clusters, young stellar objects)

2. CR transport (theory, observation, phenomenology): role of self-generated turbulence, large-scale injected turbulence; direct and indirect observations, modelling and phenomenology, link to dark matter detection

3. Local ISM: MeV CRs, Voyager data, gas and turbulence

4. Impact of GCRs: dynamics of the ISM, physics and chemistry of molecular clouds, role in the formation of stars and planets, composition of cosmomaterials

5. Future of CR studies: experiments, observations, simulations

Edwin Bergin (Univ. of Michigan, Dept. of Astronomy, Ann Arbor, USA)

Bruna Bertucci (Perugia University and INFN, Italy)

Pierre Hily-Blant (IPAG)

David Maurin (LPSC)

Gilles Maurin (LAPP)

Alexandre Marcowith (LUPM)

Johana Paquien (LPSC)

Marie-Helene Sztefek (IPAG)

Richard Taillet (LAPTh)

1^st CRISM in Montpellier (2009)
2^nd CRISM in Montpellier (June 2011)
3^rd CRISM in Montellier (June 2014) and proceedings

Photo: Tim Brook - Grenoble Panorama

25 June (first day)

12:00 am: Opening registration desk

12:50 am: Welcome address

 1:00 pm: First talk!

 6:30 pm: Cocktail at City Hall 

29 June (last day)

  2:50 pm: Summary talk

  3:30 pm: End of the conference