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The recent X-ray and CO observations of RX J1713.7-3946 show that asignificant fraction of the nonthermal X-ray emission of this unique supernovaremnant associates, in one way or another, with a molecular cloud interactingwith the west part of the shell. This adds a new puzzle in the origin of X-rayemission which cannot be easily explained within the standard model inaccordance of which X-rays are result of synchrotron radiation of multi-TeVelectrons accelerated by supernova shock waves. We explore an alternativeorigin of the X-ray emission assuming that it is produced by secondaryelectrons resulting from high energy hadronic interactions in the moleculargas. Such a scenario could explain in a quite natural way the apparentcorrelation between the X-ray and CO morphologies. However, the TeV gamma-rayemission recently reported by H.E.S.S. significantly constrains the parameterspace of this model. Namely, this mechanism cannot reproduce the bulk of theobserved X-ray flux unless one postulates existence of a PeV cosmic-raycomponent penetrating with an unusually hard spectrum into the dense cloud.Comment: 6 pages, 3 figures, to appear in Proc. of Int. Symp. on High Energy  Gamma-ray Astronomy, Heidelberg (July 2004

Nonthermal X-radiation of SNR RX J1713.7-3946: The Relations to a Nearby Molecular Cloud