TY - JOUR

T1 - Early light curves for Type Ia supernova explosion models

AU - Noebauer, U. M.

AU - Kromer, M.

AU - Taubenberger, S.

AU - Baklanov, P.

AU - Blinnikov, S.

AU - Sorokina, E.

AU - Hillebrandt, W.

PY - 2017/12

Y1 - 2017/12

N2 - Upcoming high-cadence transient survey programmes will produce a wealth of observational data for Type Ia supernovae. These data sets will contain numerous events detected very early in their evolution, shortly after explosion. Here, we present synthetic light curves, calculated with the radiation hydrodynamical approach STELLA for a number of different explosion models, specifically focusing on these first few days after explosion. We show that overall the early light curve evolution is similar for most of the investigated models. Characteristic imprints are induced by radioactive material located close to the surface. However, these are very similar to the signatures expected from ejecta-CSM or ejecta-companion interaction. Apart from the pure deflagration explosion models, none of our synthetic light curves exhibit the commonly assumed power-law rise. We demonstrate that this can lead to substantial errors in the determination of the time of explosion. In summary, we illustrate with our calculations that even with very early data an identification of specific explosion scenarios is challenging, if only photometric observations are available.

AB - Upcoming high-cadence transient survey programmes will produce a wealth of observational data for Type Ia supernovae. These data sets will contain numerous events detected very early in their evolution, shortly after explosion. Here, we present synthetic light curves, calculated with the radiation hydrodynamical approach STELLA for a number of different explosion models, specifically focusing on these first few days after explosion. We show that overall the early light curve evolution is similar for most of the investigated models. Characteristic imprints are induced by radioactive material located close to the surface. However, these are very similar to the signatures expected from ejecta-CSM or ejecta-companion interaction. Apart from the pure deflagration explosion models, none of our synthetic light curves exhibit the commonly assumed power-law rise. We demonstrate that this can lead to substantial errors in the determination of the time of explosion. In summary, we illustrate with our calculations that even with very early data an identification of specific explosion scenarios is challenging, if only photometric observations are available.

KW - Hydrodynamics

KW - Radiative transfer

KW - Supernovae: general

KW - SN 2011FE

KW - radiative transfer

KW - DEFLAGRATION MODELS

KW - hydrodynamics

KW - supernovae: general

KW - SHOCK BREAKOUT

KW - MAXIMUM LIGHT

KW - MASS MODELS

KW - RISE-TIME

KW - SYNTHETIC OBSERVABLES

KW - SPECTRA

KW - RADIATIVE-TRANSFER CALCULATIONS

KW - WHITE-DWARF MODELS

UR - http://www.scopus.com/inward/record.url?scp=85040686335&partnerID=8YFLogxK

U2 - 10.1093/MNRAS/STX2093

DO - 10.1093/MNRAS/STX2093

M3 - Article

AN - SCOPUS:85040686335

VL - 472

SP - 2787

EP - 2799

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 3

ER -