2007A&A...473..467S


Query : 2007A&A...473..467S

2007A&A...473..467S - Astronomy and Astrophysics, volume 473, 467-484 (2007/10-2)

The evolution of planetary nebulae. IV. On the physics of the luminosity function.

SCHOENBERNER D., JACOB R., STEFFEN M. and SANDIN C.

Abstract (from CDS):

The luminosity function of planetary nebulae, in use for about two decades in extragalactic distance determinations, is still subject to controversial interpretations. The physical basis of the luminosity function is investigated by means of several evolutionary sequences of model planetary nebulae computed with a 1D radiation-hydrodynamics code. The nebular evolution is followed from the vicinity of the asymptotic-giant branch across the Hertzsprung-Russell diagram until the white-dwarf domain is reached, using various central-star models coupled to different initial envelope configurations. Along each sequence the relevant line emissions of the nebulae are computed and analysed. Maximum line luminosities in Hβ and [OIII] 5007Å are achieved at stellar effective temperatures of about 65000K and 95000... 100000K, respectively, provided the nebula remains optically thick for ionising photons. In the optically thin case, the maximum line emission occurs at or shortly after the thick/thin transition. Our models suggest that most planetary nebulae with hotter (>45000K) central stars are optically thin in the Lyman continuum, and that their [OIII] 5007Å emission fails to explain the bright end of the observed planetary nebulae luminosity function. However, sequences with central stars of >0.6M and rather dense initial envelopes remain virtually optically thick and are able to populate the bright end of the luminosity function. Individual luminosity functions depend strongly on the central-star mass and on the variation of the nebular optical depth with time. Hydrodynamical simulations of planetary nebulae are essential for any understanding of the basic physics behind their observed luminosity function. In particular, our models do not support the claim of Marigo et al. (2004A&A...423..995M) according to which the maximum 5007 Å luminosity occurs during the recombination phase well beyond 100000K when the stellar luminosity declines and the nebular models become, at least partially, optically thick. Consequently, there is no need to invoke relatively massive central stars of, say >0.7M, to account for the bright end of the luminosity function.

Abstract Copyright:

Journal keyword(s): hydrodynamics - radiative transfer - planetary nebulae: general - stars: AGB and post-AGB

Simbad objects: 22

goto Full paper

goto View the references in ADS

Number of rows : 22
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 6555 1
2 NGC 1360 PN 03 33 14.6468527944 -25 52 17.977647900   10.95 11.16     sdO 274 0
3 NGC 1535 PN 04 14 15.7689913368 -12 44 21.932484324   12.01 12.82     sdO3: 508 0
4 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 16507 1
5 LHA 120-N 201 PN 05 24 55.1017509912 -71 32 56.326765848 14.822 15.319 14.240 14.440 15.698 ~ 61 0
6 IC 418 PN 05 27 28.2059533560 -12 41 50.282287764   9.405 9.010 10.118   O7fp 1021 2
7 IRAS 05319-7042S pA? 05 31 21.892 -70 40 45.47 15.439 15.842 14.676 14.950 16.530 ~ 43 0
8 2MASS J05332981-7152289 pA? 05 33 29.8030370760 -71 52 28.639071300 15.961 16.327 15.199 15.510 17.082 ~ 32 0
9 NGC 2022 PN 05 42 06.1904253312 +09 05 10.585995576   14.9 14.2     [WC] 356 0
10 SMP LMC 88 PN 05 42 33.193 -70 29 24.08 17.119 17.335 16.825 16.260 16.226 ~ 34 0
11 2MASS J05470479-6927320 pA? 05 47 04.80 -69 27 32.1 15.707 15.999 14.910   16.691 ~ 38 0
12 NGC 2610 PN 08 33 23.4238416720 -16 08 57.796735596   9.02   11.23   ~ 179 0
13 IC 2448 PN 09 07 06.3191779848 -69 56 30.692677668   11.1 11.10     O(H)3III-V 230 0
14 NGC 3242 PN 10 24 46.1335521792 -18 38 32.296857792   11.83 12.15     ~ 814 1
15 PN My 60 PN 10 31 33.4335093912 -55 20 50.821580400     13.30     ~ 74 0
16 NGC 4361 PN 12 24 30.7510527528 -18 47 05.567336304   12.8 13.2     [WC] 390 1
17 NGC 6578 PN 18 16 16.517 -20 27 02.67           [WC4/6] 202 0
18 NGC 6826 PN 19 44 48.1500225888 +50 31 30.249034932   10.21 9.6     O6fp 714 0
19 NGC 6884 PN 20 10 23.6424784416 +46 27 39.631794408   11.9 10.9     ~ 312 1
20 NGC 7027 PN 21 07 01.571952 +42 14 10.47120   10.358 8.831 10.157   ~ 2416 1
21 NGC 7293 PN 22 29 38.5454047152 -20 50 13.747242408 11.894 13.158 13.524 13.689 13.898 DAO.5 930 0
22 NGC 7662 PN 23 25 53.6 +42 32 06   9.4 12     ~ 921 0

To bookmark this query, right click on this link: simbad:objects in 2007A&A...473..467S and select 'bookmark this link' or equivalent in the popup menu


2023.01.27-12:05:16

© Université de Strasbourg/CNRS

    • Contact