Abstract
Photoelectric spectrophotometry of emission lines in the 3400-7400 A region is presented for the planetary nebulae 108-76/sup 0/1(BB1). From these observations the relative abundances of H, He, C, N, O and Ne are derived. The abundances of the halo PN (BB1, H4-1 and K648) are compared to those predicted by stellar evolution theory under the assumption that the envelope has the chemical composition of the matter located between the H burning shell and the surface. The observed He/H and C/O values are higher than predicted which implies that halo PN contain matter from deeper layers than the H burning shell. Furthermore, the O/Ar, N/Ar and Ne/Ar values in halo PN are higher than in the solar neighbourhood, at least part of this enrichment is produced by the PN progenitors.
Torres-Peimbert, S;
Rayo, J F;
Peimbert, M
[1]
- Universidad Nacional Autonoma de Mexico, Mexico City. Inst. de Astronomia
Citation Formats
Torres-Peimbert, S, Rayo, J F, and Peimbert, M.
Chemical enrichment in halo planetary nebulae.
Mexico: N. p.,
1981.
Web.
Torres-Peimbert, S, Rayo, J F, & Peimbert, M.
Chemical enrichment in halo planetary nebulae.
Mexico.
Torres-Peimbert, S, Rayo, J F, and Peimbert, M.
1981.
"Chemical enrichment in halo planetary nebulae."
Mexico.
@misc{etde_6574429,
title = {Chemical enrichment in halo planetary nebulae}
author = {Torres-Peimbert, S, Rayo, J F, and Peimbert, M}
abstractNote = {Photoelectric spectrophotometry of emission lines in the 3400-7400 A region is presented for the planetary nebulae 108-76/sup 0/1(BB1). From these observations the relative abundances of H, He, C, N, O and Ne are derived. The abundances of the halo PN (BB1, H4-1 and K648) are compared to those predicted by stellar evolution theory under the assumption that the envelope has the chemical composition of the matter located between the H burning shell and the surface. The observed He/H and C/O values are higher than predicted which implies that halo PN contain matter from deeper layers than the H burning shell. Furthermore, the O/Ar, N/Ar and Ne/Ar values in halo PN are higher than in the solar neighbourhood, at least part of this enrichment is produced by the PN progenitors.}
journal = []
volume = {6}
place = {Mexico}
year = {1981}
month = {Jan}
}
title = {Chemical enrichment in halo planetary nebulae}
author = {Torres-Peimbert, S, Rayo, J F, and Peimbert, M}
abstractNote = {Photoelectric spectrophotometry of emission lines in the 3400-7400 A region is presented for the planetary nebulae 108-76/sup 0/1(BB1). From these observations the relative abundances of H, He, C, N, O and Ne are derived. The abundances of the halo PN (BB1, H4-1 and K648) are compared to those predicted by stellar evolution theory under the assumption that the envelope has the chemical composition of the matter located between the H burning shell and the surface. The observed He/H and C/O values are higher than predicted which implies that halo PN contain matter from deeper layers than the H burning shell. Furthermore, the O/Ar, N/Ar and Ne/Ar values in halo PN are higher than in the solar neighbourhood, at least part of this enrichment is produced by the PN progenitors.}
journal = []
volume = {6}
place = {Mexico}
year = {1981}
month = {Jan}
}