Early excess emission in Type Ia supernovae from the interaction between supernova ejecta and their circumstellar wind

The effects of the interaction between Type Ia supernova ejecta and their circumstellar wind on the photometric properties of Type Ia supernovae are investigated. We assume that a hydrogen-rich, dense, and extended circumstellar matter (CSM) is formed by the steady mass-loss of their progenitor systems. The CSM density is assumed to be proportional to r (2). When the mass-loss rate is above 10 (4) M-circle dot yr (1) with a wind velocity of 100 km s-1, CSM interaction results in an early flux excess in optical light curves within 4 d of explosion. In these cases, the optical colour quickly evolves to the blue. The ultraviolet flux below 3000 angstrom is found to have a persistent flux excess compared to Type Ia supernovae as long as CSM interaction continues. Type Ia supernovae with progenitor mass-loss rates between 10 (4) and 10 (3) M-circle dot yr (1) may not have a CSM that is dense enough to affect spectra to make them Type Ia CSM, but they may still result in Type Ia supernovae with an early optical flux excess. Because they have a persistent ultraviolet flux excess, ultraviolet light curves around the luminosity peak would be significantly different from those with a low-density CSM.