Research output: Contribution to journal › Article › peer-review
Early light curves for Type Ia supernova explosion models. / Noebauer, U. M.; Kromer, M.; Taubenberger, S. et al.
In: Monthly Notices of the Royal Astronomical Society, Vol. 472, No. 3, 12.2017, p. 2787-2799.Research output: Contribution to journal › Article › peer-review
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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 -
ID: 16246236