Illuminating the Cosmos: Chemical Elements in Stars, Planets, Nebulae, and Transient Extra-galactic Events

Session

Supernovae

11 Nov 2026, 08:40

Auditorium (Haus der Astronomie)

64. TBA

Kenta Hotokezaka

11/11/2026, 09:00

Talks

18. Explodability and explosion energies of neutrino-driven supernovae

Kiril Maltsev (MPIA)

11/11/2026, 09:30

Supernovae

Talks

Massive stars undergoing iron-core collapse at the end of their evolution terminate their lives either in a successful or a failed supernova (SN). Their final fate and the explosion energy, Eexpl, depend on the Equation of State of dense matter, on uncertain neutrino physics and on properties of the stellar progenitor. An improved understanding of the stellar progenitor dependence of Eexpl is...

33. Signatures of the first stars among local extremely-metal-poor descendants

Francesco Gabrielli (Uppsala University)

11/11/2026, 09:50

Supernovae

Talks

Extremely-metal-poor (EMP) stars carry the chemical imprint of the first supernovae, offering a window into the initial mass function (IMF) of Population III (Pop III) stars. Upcoming surveys like 4MOST promise to greatly enhance these constraints through improved element coverage and larger samples, with key implications for a myriad of astrophysical topics including massive-star evolution...

27. Implications for the 12C(α,γ)16O Reaction Rate from G292.0+1.8

Mitsuki Kubo (Department of Earth Science and Astronomy, Graduate School of Arts and Sciences, The University of Tokyo)

11/11/2026, 11:10

Supernovae

Talks

The $^{12}$C($\alpha,\gamma$)$^{16}$O reaction sets the
carbon-to-oxygen ratio after core helium burning and thereby
influences the subsequent evolution and nucleosynthesis of
massive stars. Its rate at stellar energies, however, remains
uncertain. We present an observationally motivated diagnostic
by combining Chandra X-ray spectroscopy of the oxygen-rich
supernova remnant G292.0+1.8...

22. Clues for the Origin of the Heaviest Elements

Friedrich Thielemann (University of Basel)

11/11/2026, 11:30

Supernovae

Talks

For the origin of heavy r-process elements one verified astrophysical site exists up to now: neutron star mergers, identified by the spectra and the light curve of the kilonova related to GW170817.
But r-process nucleosynthesis predictions exist also for a number of additional sites: magneto-rotational supernovae with possibly related magnetar giant flares, collapsars/hypernovae as end...

45. Time Evolution of Dust Formation and Infrared Emission in Failed Supernovae

Kengo Shinoda (University of tokyo)

11/11/2026, 11:50

Supernovae

Talks

M31-2014-DS1 and NGC 6946-BH1 are candidate failed supernovae associated with black hole (BH) formation. Their rapid optical fading, accompanied by infrared brightening, suggests that newly formed dust may obscure the central source and reradiate its energy in the infrared. Understanding dust formation and the resulting infrared emission is therefore crucial for probing BH formation in failed...

60. TBA

Christine Collins

11/11/2026, 13:30

Talks

43. Mapping Helium-Burning Rate Sensitivities for 56Ni Production in Pair-Instability Supernovae

Hiroki KAWASHIMO (The University of Tokyo, Komaba)

11/11/2026, 14:00

Supernovae

Talks

Pair-instability supernovae (PISNe) are the final fates of massive stars with initial masses ranging from $140$--$260\,M_\odot$. Due to the efficient synthesis of ${}^{56}\mathrm{Ni}$, PISNe can be very luminous phenomena. According to some previous works, not only PISN progenitor evolution but also PISN nucleosynthesis is strongly affected by the...

51. Rethinking chemical evolution

Ralph Schoenrich (University College London)

11/11/2026, 15:40

Supernovae

Talks

Chemical evolution theory is central to connect abundance observations with supernova models and galactic structure. However, one can argue that traditional approaches are too simplistic, i.e. missing/neglected parameters can lead to wrong conclusions. The most prominent example is the assumption of a 1-phase interstellar medium that distorts "chemical clocks" and e.g. lead to the conclusion...

47. Grey M1 Photon Transport in Aenus-ALCAR: Towards 3D Supernovae from Core Collapse to Shock Breakout

Giorgio La Malfa (University of Valencia)

11/11/2026, 16:00

Supernovae

Talks

In core-collapse supernova simulations, photons become dynamically relevant as the ejecta expand, whereas neutrinos dominate the earlier phases. Modern approaches employ long-term photon radiation-hydrodynamics codes, where the explosion is either mapped from a self-consistent supernova code or triggered artificially. Treating photons within a self-consistent explosion code removes the need...

13. Illuminating nebular phase supernovae with 3D NLTE radiative transfer modelling

Bart van Baal (University of Turku)

11/11/2026, 16:20

Supernovae

Talks

The nebular phase of a supernova occurs several months to years after the explosion, when the ejecta become mostly optically thin yet there still is sufficient radioactive material to pump energy into the expanding remnant. The asymmetries created by the explosion are encoded into the line profiles of the emission lines which appear in the nebular phase. Modern 3D supernova simulations have...

76. meeting of Gruber Laureates 2026 with students

11/11/2026, 17:00

moderation Richard Hoppe

Prof. Alex Filippenko, Prof. Ken'ichi Nomoto, Prof. Stanford Woosley

all students are warmly invited

46. Modeling the late phase of energetic supernovae

Giacomo Ricigliano

Supernovae

Talks

Many energetic supernovae point to a variety of powering mechanisms that depart from the canonical heating from Nickel decay alone, hinting to central-engine activity and/or interaction with circumstellar material. This has important implications for the evolution of the progenitor and its explosion. One possible consequence in the hypothesis of a central engine is the trigger of r-process...