News:

Key Dates:
• 31 January 2025: Abstract Submission Portal opened.
• 3 March 2025: Deadline for Abstract Submission.
• 10 March 2025: Abstract Review begins.
• 2 April 2025: Review deadline.
• Mid- April 2025: Acceptance Notifications sent to participants.

The solar neighbourhood, understood as the region within roughly one kiloparsec from the Sun, is the closest laboratory for the study of the processes of interstellar medium (ISM) accumulation into cold, dense star-forming clouds, injection of energy, momentum, and mass from stellar feedback, and interaction between ISM phases. It is the only region of the Universe where the 3D distribution of interstellar dust has been reconstructed, where the 3D motions of young stars can be mapped and linked to their parental clouds, and where the coupling between the gas, magnetic fields, and cosmic rays can be resolved. It is also our unique neighbourhood in the universe; reconstructing its history is pivotal to determining the initial conditions that produced the Solar System.

This Special Session aims to provide a comprehensive view of the solar neighborhood's physical conditions in the context of the latest observations of stellar properties, clustering, and proper motions, soft X-ray emission with eROSITA, Faraday tomography with LOFAR and the SKA pathfinders, NIR and MIR emission with JWST, and ionized gas emission with the SDSS-V's Local volume mapper (LVM) and Milky Way mapper (MWM).

The main questions that we aim to address are:

- What have we learned about the ISM dynamics and the history of the solar neighborhood from the latest 3D ISM reconstructions?

- What is the connection between ISM phases in the local ISM and how do they compare to the rest of the Milky Way?

- What is the role of magnetic fields and cosmic rays in the distribution and dynamics of matter in the Solar Neighbourhood?

- What have we learned about the solar neighbourhood from the new analysis methods that combine different local ISM tracers and the modelling based on numerical simulations of magnetohydrodynamic (MHD) turbulence in a multiphase medium?

Programme

• Local ISM contribution Faraday rotation sky
• Three-dimensional extinction reconstruction
• Local magnetic field modelling
• Ionization in the Solar neighborhood
• Physical conditions and dynamics of the Local Bubble and its surroundings

Invited speakers

• Vibor Jelic (Ruder Boskovic Institute, Croatia)
• Kathryn Kreckel(Zentrum für Astronomie Heidelberg, Germany)
• Theo O'Neill (Harvard University, USA)
• Vincent Pelgrims (Universite Libre de Bruxelles, Belgium)
• Martin Piecka (University of Vienna, Austria)
• Michael Yeung (Max Planck Institute for Extraterrestrial Physics, Germany)

Scientific organisers

Juan Diego Soler, INAF-IAPS (Italy); Andrea Bracco, INAF - Osservatorio Astrofisico di Arcetri (Italy); Neal J. Evans II. University of Texas at Austin (United States); Isabelle Grenier. AIM, Service d'Astrophysique. CEA Saclay (France); Ralf Klessen. Heidelberg University (Germany); Gina Panopoulou. Chalmers University of Technology (Sweden)

Contact

eas2025localism @ gmail.com