Astronomy and Astrophysics, volume 461, 1095-1102 (2007/1-3)
Asteroseismological constraints on the pulsating planetary nebula nucleus (PG1159-type) RXJ2117.1+3412.
CORSICO A.H., ALTHAUS L.G., MILLER BERTOLAMI M.M. and WERNER K.
Abstract (from CDS):
We present asteroseismological inferences on RXJ2117.1+3412, the hottest known pulsating PG1159 star. Our results are based on full PG1159 evolutionary models recently presented by Miller Bertolami & Althaus (2006A&A...454..845M
). We performed extensive computations of adiabatic g-mode pulsation periods on PG1159 evolutionary models with stellar masses ranging from 0.530 to 0.741M☉
. PG1159 stellar models are extracted from the complete evolution of progenitor stars started from the ZAMS, through the thermally pulsing AGB and born-again phases to the domain of the PG1159 stars. We constrained the stellar mass of RXJ2117.1+3412 by comparing the observed period spacing with the asymptotic period spacing and with the average of the computed period spacings. We also employed the individual observed periods to find a representative seismological model for RXJ2117.1+3412.We derive a stellar mass M*
from the period spacing data alone. In addition, we found a best-fit model representative for RXJ2117.1+3412 with an effective temperature Teff
=163400K, a stellar mass M*
, and a surface gravity logg=6.61. The derived stellar luminosity and radius are log (L*
)=3.36 and log(R*
)=-1.23, respectively, and the He-rich envelope thickness is Menv
. We derive a seismic distance d∼452pc and a linear size of the planetary nebula DPN
∼1.72pc. These inferences seem to solve the discrepancy between the RXJ2117.1+3412 evolutionary timescale and the size of the nebula. All of the seismological tools we use concur to the conclusion that RXJ2117.1+3412 must have a stellar mass M*
, much in agreement with recent asteroseismology studies and in clear conflict with the predictions of spectroscopy plus evolutionary tracks.
stars: evolution - stars: interiors - stars: oscillations - planetary nebulae: general
erratum vol. 470, p. 1031 (2007)
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