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We present asteroseismological inferences on RX J2117.1+3412, the hottestknown pulsating PG1159 star. Our results are based on full PG1159 evolutionarymodels recently presented by Miller Bertolami & Althaus (2006). We performedextensive computations of adiabatic g-mode pulsation periods on PG1159evolutionary models with stellar masses ranging from 0.530 to 0.741 Mo. PG1159stellar models are extracted from the complete evolution of progenitor starsstarted from the ZAMS, through the thermally pulsing AGB and born-again phasesto the domain of the PG 1159 stars. We constrained the stellar mass of RXJ2117.1+3412 by comparing the observed period spacing with the asymptoticperiod spacing and with the average of the computed period spacings. We alsoemployed the individual observed periods to find a representative seismologicalmodel. We derive a stellar mass of 0.56-0.57 Mo from the period spacing dataalone. In addition, we found a best-fit model representative for RXJ2117.1+3412 with an effective temperature of 163,400 K, a stellar mass of0.565 Mo, and a surface gravity log g= 6.61. The derived stellar luminosity andradius are log(L/Lo)= 3.36 and log(R/Ro)= -1.23, respectively, and the He-richenvelope thickness is Menv= 0.02 Mo. We derive a seismic distance of 452 pc anda linear size of the planetary nebula of 1.72 pc. These inferences seem tosolve the discrepancy between the RX J2117.1+3412 evolutionary timescale andthe size of the nebula. All of the seismological tools we use concur to theconclusion that RX J2117.1+3412 must have a stellar mass of 0.565 Mo much inagreement with recent asteroseismology studies and in clear conflict with thepredictions of spectroscopy plus evolutionary tracks.Comment: 10 pages, 6 figures, 2 tables. Accepted for publication in Astronomy  and Astrophysics. Erratum available as a separate fil

Asteroseismological constraints on the pulsating planetary nebula nucleus (PG 1159-type) RX J2117.1+3412