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We present a numerical parameter survey of sub-Chandrasekhar mass white dwarf(WD) explosions. Carbon-oxygen WDs accreting a helium shell have the potentialto explode in the sub-Chandrasekhar mass regime. Previous studies have shownhow the ignition of a helium shell can either directly ignite the WD at thecore-shell interface or propagate a shock wave into the the core causing acentral ignition. We examine the explosions of WDs from 0.6 - 1.2 M$_\odot$with helium shells of 0.01, 0.05 and 0.08 M$_\odot$. Distinct observationalsignatures of sub-Chandrasekhar mass WD explosions are predicted for twocategories of shell size. Thicker-shell models show an early time flux excess,which is caused by the presence of radioactive material in the ashes of thehelium shell, and red colors due to these ashes creating significant lineblanketing in the UV through the blue portion of the spectrum. Thin shellmodels reproduce several typical Type Ia supernova signatures. We identify arelationship between Si II velocity and luminosity which, for the first time,identifies a sub-class of observed supernovae that are consistent with thesemodels. This sub-class is further delineated by the absence of carbon in theiratmospheres. We suggest that the proposed difference in the ratio of selectiveto total extinction between the high velocity and normal velocity Type Iasupernovae is not due to differences in the properties of the dust around theseevents, but is rather an artifact of applying a single extinction correction totwo intrinsically different populations of supernovae.

Observational Predictions for Sub-Chandrasekhar Mass Explosions: Further Evidence for Multiple Progenitor Systems for Type Ia Supernovae