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• W3104382014 endingPage "83" @default.
• W3104382014 startingPage "83" @default.
• W3104382014 abstract "The rising luminosity of the recent, nearby supernova 2011fe shows a quadratic dependence with time during the first ≈0.5–4 days. In addition, studies of the composite light curves formed from stacking together many Type Ia supernovae (SNe Ia) have found similar power-law indices for the rise, but may also show some dispersion that may indicate diversity. I explore what range of power-law rises are possible due to the presence of radioactive material near the surface of the exploding white dwarf (WD). I summarize what constraints such a model places on the structure of the progenitor and the distribution and velocity of ejecta. My main conclusion is that for the inferred explosion time for SN 2011fe, its rise requires an increasing mass fraction X56 ≈ (4–6) × 10−2 of 56Ni distributed between a depth of ≈10−2 and 0.3 M☉ below the WD's surface. Radioactive elements this shallow are not found in simulations of a single C/O detonation. Scenarios that may produce this material include helium-shell burning during a double-detonation ignition, a gravitationally confined detonation, and a subset of deflagration to detonation transition models. In general, the power-law rise can differ from quadratic depending on the details of the velocity, density, and radioactive deposition gradients in a given event. Therefore, comparisons of this work with observed bolometric rises of SNe Ia would place strong constraints on the properties of the shallow outer layers, providing important clues for identifying the elusive progenitors of SNe Ia." @default.
• W3104382014 created "2020-11-23" @default.
• W3104382014 creator A5037828745 @default.
• W3104382014 date "2012-10-19" @default.
• W3104382014 modified "2023-10-17" @default.
• W3104382014 title "RADIOACTIVELY POWERED RISING LIGHT CURVES OF TYPE Ia SUPERNOVAE" @default.
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• W3104382014 doi "https://doi.org/10.1088/0004-637x/759/2/83" @default.
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