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R~CrA is the brightest member of the Coronet star forming region and it isthe closest Herbig AeBe star with a spectrum dominated by emission lines. Itsluminosity has been monitored since the end of the 19th century, but the originof its variability, which shows a stable period of $65.767\pm 0.007$~days, isstill unknown. We studied photometric and spectroscopic data for this star toinvestigate the nature of the variability of R~CrA. We exploited the fact thatnear infrared luminosity of the Herbig AeBe stars is roughly proportional tothe total luminosity of the stars to derive the absorption, and then mass andage of R~CrA. In addition, we model the periodic modulation of the light curveas due to partial attenuation of a central binary by a circumbinary disk. Thismodel reproduces very well the observations. We found that the central objectin R~CrA is a very young ($1.5\pm 1.5$~Myr), highly absorbed ($A_V=5.47\pm0.4$~mag) binary; we obtain masses of $M_A=3.02\pm 0.43$~M$_\odot$ and$M_B=2.32\pm 0.35$~M$_\odot$ for the two components. We propose that thesecular decrease of the R~CrA apparent luminosity is due to a progressiveincrease of the disk absorption. This might be related to precession of aslightly inclined disk caused by the recently discovered M-dwarf companion.Thus, R~CrA may be a triple system hosting a disk.

The origin of R CrA variability: A complex triple system hosting a disk