Interacting Supernovae

6 February - 3 March 2023

Luc Dessart, Raffaella Margutti, Jim Fuller, Rolf-Peter Kudritzki

High-cadence long-term monitoring of the transient sky suggests that most core-collapse supernovae are influenced at some level by interaction with circumstellar material. Although considered so far a feature in core-collapse supernovae, this observation has led theorists to revise the idealized view of massive star evolution and explosion, introducing a slew of time-dependent, dynamical, and multi-dimensional effects that remain today poorly understood. Bringing together experts on this multi-faceted domain of astrophysics, this MIAPP programme will allow the community 1) to investigate the various mechanisms at the origin of eruptions and explosions of massive stars, 2) to improve the techniques of radiation hydrodynamics and radiative transfer modeling of these events, 3) to integrate these advances in order to dissect the rapidly growing observational zoo of interacting supernovae, and 4) to quantify the influence of circumstellar interaction on supernova-based extragalactic distance measurements. This gathering will prepare the supernova community for the upcoming era of transient astrophysics with the Vera Rubin Observatory LSST.

 

Tentative Programme:

== Day 1-5 (week 1): Theoretical considerations

   Multi-D modeling of stellar interiors. Advanced stages.
   Wave excitation
   Nuclear flashes
   Pulsational-pair instability
   Binary effects (mass transfer versus time, common envelope)
   Super-Eddington winds in the context of shocked stellar envelopes


== Day 6-10 (week 2): The interaction zoo

   SN II-P with CSM like 13fs or 20tlf.
   IIL versus IIn.
   IIn-P like 94W.
   Superluminous SNe IIn like 10jl, 06gy.
   SNe Ibn, Icn and Ian
   FBOTs


== Day 11-15 (week 3): Additional clues

   Spectropolarimetry
   Dust and molecules in interacting SNe.
   SN progenitor observations
   Environments
   Future surveys and observations: LSST, ELT etc. Interacting SNe at cosmological distances.
   UV observations: past, current, and future.


== Day 16-20 (week 4): SN radiation

   Radiation hydrodynamics
   Radiative transfer
   Polarized radiative transfer
   Dust and molecule formation
   Impact of interaction on SN-based distances (WLR for SNe Ia, EPM for SNe II)