photometry for the carbon Mira star V CrB are presented. The infrared observations were carried out in the time interval 1989–2018, while the , , and data were obtained in 2001–2014. The light and color curves are analyzed. The pulsation period of V CrB has been found to be in the infrared bands and for the optical band. In the bands, apart from periodic pulsations, there are distinct sinusoidal variations in the average brightness level with a characteristic period of days. Color–magnitude relationships have been revealed for the infrared and optical bands. The phase curves exhibit the wavelength dependence of the brightness variability amplitude. The light curves for various bands and colors are discussed. We have constructed the model of a spherically symmetric circumstellar dust envelope that allows the observed spectral energy distribution at both maximum and minimum light to be reproduced equally well (within the model assumptions) and is consistent with the observations of V CrB by differential speckle polarimetry. The model is characterized by the following parameters: the optical depth is , the inner and outer radii of the envelope are 8 and 40 000 AU, respectively. The envelope contains spherical carbon dust grains ( by mass) and silicon carbide dust grains. Dust grains with a radius of 0.5 m account for of the envelope mass. The remaining of the mass is accounted for by finer dust with a grain radius of 0.1 m. Based on the observational data, we have estimated the bolometric flux from V CrB: and erg cm s at minimum and maximum light, respectively. The effective temperature of the star is K at maximum light and K at minimum light.