The Heidelberg Supernova Model Archive [1] provides data on about 70 models from the Type Ia supernova group formerly based at the Max Planck Institute for Astrophysics in Garching (MPA) and now spread to Heidelberg, Belfast and Canberra. The models cover a wide range of progenitor scenarios and explosion mechanisms of Type Ia supernovae.

The explosion simulations were performed with the hydrodynamics code LEAFS [2] or the moving-mesh code AREPO [3]. Simulations of the merging process in the violent merger scenario were conducted using GADGET [4]. Detailed isotopic abundances were obtained from nucleosynthesis calculations employing a large 384-isotope network on thermodynamic trajectories of tracer particles [5]. Finally, synthetic spectral time series were derived with the multi-dimensional Monte Carlo radiative transfer code ARTIS [6]. For some models, synthetic light curves for early epochs in the U, B, V, and R passbands were calculated with the one-dimensional radiation hydrodynamics code STELLA [7].

In HESMA, we provide integrated isotopic abundances as well as radially averaged density and isotopic abundance profiles of the explosion ejecta after they achieved homologous expansion. We also offer angle-averaged UVOIR bolometric light curves and gamma-ray and optical spectral time series. Bolometric light curves are tabulated from ~ 6 to 80 d past explosion. Gamma-ray spectra for selected models are available from ~ 6 to 100 d past explosion. Optical (λ ϵ [3500,9500] Å) spectral time series are available from ~ 6 to 40 d past explosion. Finally, early synthetic light curves calculated with STELLA for the epoch from 1.1 to 10 d past explosion are provided in the U, B, V, and R passbands. For some models, additional data (e.g. viewing-angle dependent spectra) are available and can be accessed via the corresponding links on the model pages.

You have to register to get the data. If you are interested in additional data for a specific model (e.g. gamma-ray or near-infrared spectra), or encounter inconsistencies in the data please contact us directly at hesma@h-its.org.

Please always use model data from this archive, which will be updated if we encounter errors in the data (see News for a changelog). If you make use of the data provided through this website in publications, please add the following acknowledgements: “This work made use of the Heidelberg Supernova Model Archive (HESMA), https://hesma.h-its.org.”

[1] Kromer, M., Ohlmann, S.T., Roepke, F.K., arXiv:1706.09879

[2] Reinecke, M., Hillebrandt, W., & Niemeyer, J. C. 2002, A&A, 386, 936

[3] Springel, V. 2010, MNRAS, 401, 791

[4] Pakmor, R.; Edelmann, P.; Röpke, F. K.; Hillebrandt, W. 2012, MNRAS, 424, 2222

[5] Travaglio, C., Hillebrandt, W., Reinecke, M., & Thielemann, F.-K. 2004, A&A, 425, 1029

[6] Kromer, M. & Sim, S. A. 2009, MNRAS, 398, 1809

[7] Blinnikov, S. I., Röpke, F. K., Sorokina, E. I., Gieseler, M., Reinecke, M., Travaglio, C., Hillebrandt, W., Stritzinger, M. 2006, A&A, 453, 229