A&A 470, 1031 (2007)
DOI: 10.1051/0004-6361:20066452e


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

A. H. Córsico1,2,[*] - L. G. Althaus1,2,[*] - M. M. Miller Bertolami1,2,[*]

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).



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