Asteroseismological constraints on the pulsating planetary nebula nucleus (PG1159-type) RXJ2117.1+3412

A. H. Córsico^1,2, - L. G. Althaus^1,2, - M. M. Miller Bertolami^1,2,

1 - Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque S/N, (1900) La Plata, Argentina
2 - Instituto de Astrofísica La Plata, IALP, CONICET-UNLP, Argentina

A&A, 461, 1095-1102 (2007), DOI: 10.1051/0004-6361:20066452

Key words: stars: evolution - stars: interiors - stars: oscillations - ISM: planetary nebulae: general - errata, addenda

1 Erratum

The value of the expansion age of the planetary nebula of RXJ2117.1+3412 ( $t_{\rm PN}$ ) that appears in the last column and last line in Table 2, and also in the last paragraph of Sect. 7 and fourth paragraph of Sect. 8 is wrong. The mistake originated because we erroneously employed the diameter of the nebula ( $D_{\rm PN}= 5.3 \times 10^{13}$ km) instead of the radius ( $R_{\rm PN}= D_{\rm PN}/2= 2.65 \times 10^{13}$ km) to compute $t_{\rm PN}$ . If we use the radius of the nebula and the expansion velocity of 31 kms^-1, we arrive at the correct value for the expansion age of the nebula: $t_{\rm PN}\sim 2.72 \times 10^4$ yr.

Note that the evolutionary timescale of the central star of RXJ2117.1+3412 is $t_* \sim 2.5 \times 10^4$ yr (last column in Table 2). Therefore, by considering the correct value for the expansion age we found that $t_{\rm PN} \simeq t_*$ . This result definitively solves the discrepancy between the RXJ2117.1+3412 evolutionary timescale and the size of its nebula (see Appleton et al. 1993).

References

Appleton, P. N., Kawaler, S. D., & Eitter, J. J. 1993, AJ, 106, 1973 [NASA ADS] [CrossRef] (In the text)