PN abundances in five galaxies (Stasińska+ 1998)

Details PN abundances in five galaxies (Stasińska+ 1998) PN abundances in five galaxies (Stasińska+ 1998)

May 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998ycat..33360667s&link_type=abstract

VizieR On-line Data Catalog: J/A+A/336/667. Originally published in: 1998A&A...336..667S

Computer Science

Planetary Nebulae, Abundances, Opacities

Scientific paper

The models are computed using the photoionization code PHOTO in the same conditions as Stasińska (1990A&AS...83..501S) but with atomic data updated as reported in Stasińska & Leitherer (1996ApJS..107..661S). The planetary nebulae are modeled as uniformly expanding spherical shells of constant total mass and constant relative thickness δR/R, in which the density, assumed uniform, is varying with time appropriately. The evolution of the central stars is interpolated from the hydrogen burning post-AGB evolutionary tracks of Blocker (1995, Cat. ). The stars are assumed to radiate like blackbodies. The files containing the models are named mMvVsSSZ.res, where M defines the total nebular mass MNEB: m=1 stands for Mneb= 0.1 solar mass m=2 stands for Mneb= 0.2 solar mass m=4 stands for Mneb= 0.4 solar mass V defines the expansion velocity VEXP of the outer edge v=1 stands for Vexp=10 km/sec v=2 stands for Vexp=20 km/sec v=4 stands for Vexp=40 km/sec SS defines the central star mass Mstar (in units of hundredths of a solar mass) ex: ss=58 stands for Mstar=0.58 solar mass Z is a character defining the abundance set with respect to the solar value Zsol In the present grid, the values of z are defined as follows: h for Z=0.5Zsol e for Z=0.1Zsol k for Z=2.0Zsol the abundance ratios are defined as in Stasińska & Leitherer, 1996ApJS..107..661S. The grid is composed of the following 94 ascii files of record length 132: m1v1s56h.res m1v4s62h.res m2v2s62k.res m4v1s61h.res m1v1s57h.res m1v4s63h.res m2v2s63h.res m4v1s62h.res m1v1s58h.res m1v4s64h.res m2v2s64e.res m4v1s63h.res m1v1s59h.res m2v1s56h.res m2v2s64h.res m4v1s64h.res m1v1s60h.res m2v1s57h.res m2v2s64k.res m4v2s56h.res m1v1s61h.res m2v1s58h.res m2v2s65h.res m4v2s57h.res m1v1s62h.res m2v1s59h.res m2v2s66h.res m4v2s58h.res m1v1s63h.res m2v1s60h.res m2v2s70h.res m4v2s59h.res m1v1s64h.res m2v1s61h.res m2v2s80h.res m4v2s60h.res m1v2s56h.res m2v1s62h.res m2v2s90h.res m4v2s61h.res m1v2s57h.res m2v1s63h.res m2v4s56h.res m4v2s62h.res m1v2s58h.res m2v1s64h.res m2v4s57h.res m4v2s63h.res m1v2s59h.res m2v2s56h.res m2v4s58h.res m4v2s64h.res m1v2s60h.res m2v2s57h.res m2v4s59h.res m4v4s56h.res m1v2s61h.res m2v2s58e.res m2v4s60h.res m4v4s57h.res m1v2s62h.res m2v2s58h.res m2v4s61h.res m4v4s58h.res m1v2s63h.res m2v2s58k.res m2v4s62h.res m4v4s59h.res m1v2s64h.res m2v2s59h.res m2v4s63h.res m4v4s60h.res m1v4s56h.res m2v2s60e.res m2v4s64h.res m4v4s61h.res m1v4s57h.res m2v2s60h.res m4v1s56h.res m4v4s62h.res m1v4s58h.res m2v2s60k.res m4v1s57h.res m4v4s63h.res m1v4s59h.res m2v2s61h.res m4v1s58h.res m4v4s64h.res m1v4s60h.res m2v2s62e.res m4v1s59h.res m1v4s61h.res m2v2s62h.res m4v1s60h.res A file is composed of a series of models computed at time intervals of 500 years. Each model is described by a group of 51 rows. (3 data files).

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