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We present an analysis of mid-and far-infrared (IR) spectrum and spectralenergy distribution (SED) of the LBV R71 in the LMC.This work aims tounderstand the overall contribution of high-mass LBVs to the total dust-massbudget of the interstellar medium (ISM) of the LMC and compare this with thecontribution from low-mass asymptotic giant branch (AGB) stars. As a casestudy, we analyze the SED of R71. We compiled all the available photometric andspectroscopic observational fluxes from various telescopes for a widewavelength range (0.36 -- 250\,$\mu$m). We determined the dust composition fromthe spectroscopic data, and derived the ejected dust mass, dust mass-loss rate,and other dust shell properties by modeling the SED of R71. We noted ninespectral features in the dust shell of R71 by analyzing Spitzer spectroscopicdata. Among these, we identified three new crystalline silicate features. Wecomputed our model spectrum by using 3D radiative transfer code MCMax. Ourmodel calculation shows that dust is dominated by amorphous silicates, withsome crystalline silicates, metallic iron, and a very tiny amount of polycyclicaromatic hydrocarbon (PAH) molecules. The presence of both silicates and PAHsindicates that the dust has a mixed chemistry. We derived a dust mass of 0.01M$_\odot$, from which we arrive at a total ejected mass of $\approx$ 5M$_\odot$. This implies a time-averaged dust mass-loss rate of2.5$\times$10$^{-6}$ M$_\odot$\,yr$^{-1}$ with an explosion about 4000 yearsago. We assume that the other five confirmed dusty LBVs in the LMC loose massat a similar rate, and estimate the total contribution to the mass budget ofthe LMC to be $\approx$ 10$^{-5}$ M$_\odot$\,yr$^{-1}$, which is comparable tothe contribution by all the AGB stars in the LMC. Based on our analysis on R71,we speculate that LBVs as a class may be an important dust source in the ISM ofthe LMC.

Dust composition and mass-loss return from the luminous blue variable R71 in the LMC