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We undertake a theoretical study of the near-infrared (NIR) lightcurves ofType Ia supernovae (SNe Ia). In these bands, the lightcurves are distinguishedby a secondary maximum occurring roughly 20 to 30 days after the initial one.Using time-dependent multi-group radiative transfer calculations, we calculatethe UBVRIJHK-band lightcurves of model SN Ia ejecta structures. Our syntheticNIR lightcurves show distinct secondary maxima, and provide favorable fits toobserved SNe Ia. We offer a detailed explanation of the origin of the NIRsecondary maximum, which is shown to relate directly to the ionizationevolution of iron group elements in the ejecta. This understanding providesimmediate intuition into the dependence of the NIR lightcurves on the physicalproperties of the ejecta, and in particular explains why brighter supernovaehave a later and more prominent secondary maximum. We demonstrate thedependence of the NIR lightcurves on the mass of 56Ni, the degree of 56Nimixing, the mass of electron caputre elements, the progenitor metallicity, andthe abundance of intermediate mass elements (especially calcium). The secondarymaximum is shown to be a valuable diagnostic of these important physicalparameters. The models further confirm that SNe Ia should be excellent standardcandles in the NIR, with a dispersion < 0.2 mag even when the physicalproperties of the ejecta are varied widely. This study emphasizes theconsummate value of NIR observations in probing the structure of SNe Ia and infurthering their cosmological utility.Comment: 14 pages; ApJ accepte

Secondary Maximum in the Near‐Infrared Light Curves of Type Ia Supernovae