Abundances of the observed species for IRAS 18095+2704 are presented for a model atmospheres of Teff = 6700 K, log g = 0.3 (KT), ξ = 6.0 and Teff = 6500 K, log g = 0.5, ξ = 4.7 (this work). The solar abundances from Asplund et al. (2009) is used to convert Klochkova's abundance of element X to [X/Fe] for comparison purposes.
Species | K95 | K95 | This work | log ε⊙ | |||
log ε(X) | [X/Fe] | log ε(X) | [X/Fe] | Δ | N | ||
C i | 8.27 | +0.50 | 7.92 | +0.40 | −0.35 | 11 | 8.43 |
N i | 7.66 | +0.47 | ≤7.19 | ≤+0.27 | ≤−0.47 | 2 | 7.83 |
O i | 8.74 | +0.65 | 8.55 | +0.77 | −0.19 | 6 | 8.69 |
Na i | 6.02 | +0.47 | 6.12 | +0.79 | +0.10 | 5 | 6.24 |
Mg i | 7.42 | +0.62 | 7.14 | +0.45 | −0.28 | 4 | 7.60 |
Mg ii | 7.52 | +0.72 | 7.17 | +0.48 | −0.35 | 1 | 7.60 |
Al i | 5.81 | +0.12 | 4.86 | −0.68 | −0.95 | 2 | 6.45 |
Si i | 7.48 | +0.71 | 7.18 | +0.58 | −0.30 | 6 | 7.51 |
Si ii | … | … | 6.70 | +0.10 | … | 1 | 7.51 |
S i | 6.96 | +0.53 | 6.98 | +0.77 | +0.02 | 7 | 7.12 |
Ca i | 5.84 | +0.26 | 5.48 | +0.05 | −0.36 | 13 | 6.34 |
Ca ii | … | … | 5.40 | −0.03 | … | 4 | 6.34 |
Sc ii | 2.25 | −0.30 | 2.08 | −0.16 | −0.17 | 7 | 3.15 |
Ti i | 5.68 | +1.44 | 3.97 | −0.07 | −1.71 | 1 | 4.95 |
Ti ii | 4.05 | −0.19 | 4.04 | +0.00 | −0.01 | 12 | 4.95 |
V ii | 3.45 | +0.23 | 3.24 | +0.22 | −0.21 | 2 | 3.93 |
Cr i | 6.02 | +1.13 | 4.71 | −0.02 | −1.31 | 10 | 5.64 |
Cr ii | 4.98 | +0.09 | 4.54 | −0.19 | −0.44 | 9 | 5.64 |
Mn i | 5.12 | +0.51 | 4.44 | −0.08 | −0.68 | 3 | 5.43 |
Fe i | 6.71 | −0.01 | 6.59 | +0.00 | −0.12 | 31 | 7.50 |
Fe ii | 6.73 | +0.01 | 6.59 | +0.00 | −0.14 | 11 | 7.50 |
Co i | 5.74 | +1.60 | 4.26 | +0.18 | −1.48 | 1 | 4.99 |
Ni i | 6.13 | +0.66 | 5.48 | +0.17 | −0.65 | 11 | 6.22 |
Cu i | 4.06 | +0.63 | ≤3.35 | ≤ +0.07 | ≤−0.71 | 1 | 4.19 |
Zn i | 4.60 | +0.78 | 3.86 | +0.21 | −0.74 | 3 | 4.56 |
Sr ii | … | … | 2.52 | +0.56 | … | 2 | 2.87 |
Y ii | 1.42 | −0.04 | 0.72 | −0.58 | −0.70 | 4 | 2.21 |
Zr ii | … | … | 1.31 | −0.36 | … | 3 | 2.58 |
Ba ii | 1.13 | −0.22 | 1.05 | −0.22 | −0.08 | 1 | 2.18 |
La ii | 0.83 | +0.39 | ≤0.31 | ≤ +0.12 | ≤−0.52 | 1 | 1.10 |
Nd ii | 1.56 | +0.84 | ≤0.44 | ≤ −0.07 | ≤−1.12 | 1 | 1.42 |
Eu ii | 0.96 | +1.23 | −0.05 | +0.34 | −1.01 | 1 | 0.52 |
Species | K95 | K95 | This work | log ε⊙ | |||
log ε(X) | [X/Fe] | log ε(X) | [X/Fe] | Δ | N | ||
C i | 8.27 | +0.50 | 7.92 | +0.40 | −0.35 | 11 | 8.43 |
N i | 7.66 | +0.47 | ≤7.19 | ≤+0.27 | ≤−0.47 | 2 | 7.83 |
O i | 8.74 | +0.65 | 8.55 | +0.77 | −0.19 | 6 | 8.69 |
Na i | 6.02 | +0.47 | 6.12 | +0.79 | +0.10 | 5 | 6.24 |
Mg i | 7.42 | +0.62 | 7.14 | +0.45 | −0.28 | 4 | 7.60 |
Mg ii | 7.52 | +0.72 | 7.17 | +0.48 | −0.35 | 1 | 7.60 |
Al i | 5.81 | +0.12 | 4.86 | −0.68 | −0.95 | 2 | 6.45 |
Si i | 7.48 | +0.71 | 7.18 | +0.58 | −0.30 | 6 | 7.51 |
Si ii | … | … | 6.70 | +0.10 | … | 1 | 7.51 |
S i | 6.96 | +0.53 | 6.98 | +0.77 | +0.02 | 7 | 7.12 |
Ca i | 5.84 | +0.26 | 5.48 | +0.05 | −0.36 | 13 | 6.34 |
Ca ii | … | … | 5.40 | −0.03 | … | 4 | 6.34 |
Sc ii | 2.25 | −0.30 | 2.08 | −0.16 | −0.17 | 7 | 3.15 |
Ti i | 5.68 | +1.44 | 3.97 | −0.07 | −1.71 | 1 | 4.95 |
Ti ii | 4.05 | −0.19 | 4.04 | +0.00 | −0.01 | 12 | 4.95 |
V ii | 3.45 | +0.23 | 3.24 | +0.22 | −0.21 | 2 | 3.93 |
Cr i | 6.02 | +1.13 | 4.71 | −0.02 | −1.31 | 10 | 5.64 |
Cr ii | 4.98 | +0.09 | 4.54 | −0.19 | −0.44 | 9 | 5.64 |
Mn i | 5.12 | +0.51 | 4.44 | −0.08 | −0.68 | 3 | 5.43 |
Fe i | 6.71 | −0.01 | 6.59 | +0.00 | −0.12 | 31 | 7.50 |
Fe ii | 6.73 | +0.01 | 6.59 | +0.00 | −0.14 | 11 | 7.50 |
Co i | 5.74 | +1.60 | 4.26 | +0.18 | −1.48 | 1 | 4.99 |
Ni i | 6.13 | +0.66 | 5.48 | +0.17 | −0.65 | 11 | 6.22 |
Cu i | 4.06 | +0.63 | ≤3.35 | ≤ +0.07 | ≤−0.71 | 1 | 4.19 |
Zn i | 4.60 | +0.78 | 3.86 | +0.21 | −0.74 | 3 | 4.56 |
Sr ii | … | … | 2.52 | +0.56 | … | 2 | 2.87 |
Y ii | 1.42 | −0.04 | 0.72 | −0.58 | −0.70 | 4 | 2.21 |
Zr ii | … | … | 1.31 | −0.36 | … | 3 | 2.58 |
Ba ii | 1.13 | −0.22 | 1.05 | −0.22 | −0.08 | 1 | 2.18 |
La ii | 0.83 | +0.39 | ≤0.31 | ≤ +0.12 | ≤−0.52 | 1 | 1.10 |
Nd ii | 1.56 | +0.84 | ≤0.44 | ≤ −0.07 | ≤−1.12 | 1 | 1.42 |
Eu ii | 0.96 | +1.23 | −0.05 | +0.34 | −1.01 | 1 | 0.52 |
Notes. K95: Klochkova (1995).
N is the number of the lines employed in our abundance determination.
The solar abundances (log ε⊙) are from Asplund et al. (2009).
Abundances of the observed species for IRAS 18095+2704 are presented for a model atmospheres of Teff = 6700 K, log g = 0.3 (KT), ξ = 6.0 and Teff = 6500 K, log g = 0.5, ξ = 4.7 (this work). The solar abundances from Asplund et al. (2009) is used to convert Klochkova's abundance of element X to [X/Fe] for comparison purposes.
Species | K95 | K95 | This work | log ε⊙ | |||
log ε(X) | [X/Fe] | log ε(X) | [X/Fe] | Δ | N | ||
C i | 8.27 | +0.50 | 7.92 | +0.40 | −0.35 | 11 | 8.43 |
N i | 7.66 | +0.47 | ≤7.19 | ≤+0.27 | ≤−0.47 | 2 | 7.83 |
O i | 8.74 | +0.65 | 8.55 | +0.77 | −0.19 | 6 | 8.69 |
Na i | 6.02 | +0.47 | 6.12 | +0.79 | +0.10 | 5 | 6.24 |
Mg i | 7.42 | +0.62 | 7.14 | +0.45 | −0.28 | 4 | 7.60 |
Mg ii | 7.52 | +0.72 | 7.17 | +0.48 | −0.35 | 1 | 7.60 |
Al i | 5.81 | +0.12 | 4.86 | −0.68 | −0.95 | 2 | 6.45 |
Si i | 7.48 | +0.71 | 7.18 | +0.58 | −0.30 | 6 | 7.51 |
Si ii | … | … | 6.70 | +0.10 | … | 1 | 7.51 |
S i | 6.96 | +0.53 | 6.98 | +0.77 | +0.02 | 7 | 7.12 |
Ca i | 5.84 | +0.26 | 5.48 | +0.05 | −0.36 | 13 | 6.34 |
Ca ii | … | … | 5.40 | −0.03 | … | 4 | 6.34 |
Sc ii | 2.25 | −0.30 | 2.08 | −0.16 | −0.17 | 7 | 3.15 |
Ti i | 5.68 | +1.44 | 3.97 | −0.07 | −1.71 | 1 | 4.95 |
Ti ii | 4.05 | −0.19 | 4.04 | +0.00 | −0.01 | 12 | 4.95 |
V ii | 3.45 | +0.23 | 3.24 | +0.22 | −0.21 | 2 | 3.93 |
Cr i | 6.02 | +1.13 | 4.71 | −0.02 | −1.31 | 10 | 5.64 |
Cr ii | 4.98 | +0.09 | 4.54 | −0.19 | −0.44 | 9 | 5.64 |
Mn i | 5.12 | +0.51 | 4.44 | −0.08 | −0.68 | 3 | 5.43 |
Fe i | 6.71 | −0.01 | 6.59 | +0.00 | −0.12 | 31 | 7.50 |
Fe ii | 6.73 | +0.01 | 6.59 | +0.00 | −0.14 | 11 | 7.50 |
Co i | 5.74 | +1.60 | 4.26 | +0.18 | −1.48 | 1 | 4.99 |
Ni i | 6.13 | +0.66 | 5.48 | +0.17 | −0.65 | 11 | 6.22 |
Cu i | 4.06 | +0.63 | ≤3.35 | ≤ +0.07 | ≤−0.71 | 1 | 4.19 |
Zn i | 4.60 | +0.78 | 3.86 | +0.21 | −0.74 | 3 | 4.56 |
Sr ii | … | … | 2.52 | +0.56 | … | 2 | 2.87 |
Y ii | 1.42 | −0.04 | 0.72 | −0.58 | −0.70 | 4 | 2.21 |
Zr ii | … | … | 1.31 | −0.36 | … | 3 | 2.58 |
Ba ii | 1.13 | −0.22 | 1.05 | −0.22 | −0.08 | 1 | 2.18 |
La ii | 0.83 | +0.39 | ≤0.31 | ≤ +0.12 | ≤−0.52 | 1 | 1.10 |
Nd ii | 1.56 | +0.84 | ≤0.44 | ≤ −0.07 | ≤−1.12 | 1 | 1.42 |
Eu ii | 0.96 | +1.23 | −0.05 | +0.34 | −1.01 | 1 | 0.52 |
Species | K95 | K95 | This work | log ε⊙ | |||
log ε(X) | [X/Fe] | log ε(X) | [X/Fe] | Δ | N | ||
C i | 8.27 | +0.50 | 7.92 | +0.40 | −0.35 | 11 | 8.43 |
N i | 7.66 | +0.47 | ≤7.19 | ≤+0.27 | ≤−0.47 | 2 | 7.83 |
O i | 8.74 | +0.65 | 8.55 | +0.77 | −0.19 | 6 | 8.69 |
Na i | 6.02 | +0.47 | 6.12 | +0.79 | +0.10 | 5 | 6.24 |
Mg i | 7.42 | +0.62 | 7.14 | +0.45 | −0.28 | 4 | 7.60 |
Mg ii | 7.52 | +0.72 | 7.17 | +0.48 | −0.35 | 1 | 7.60 |
Al i | 5.81 | +0.12 | 4.86 | −0.68 | −0.95 | 2 | 6.45 |
Si i | 7.48 | +0.71 | 7.18 | +0.58 | −0.30 | 6 | 7.51 |
Si ii | … | … | 6.70 | +0.10 | … | 1 | 7.51 |
S i | 6.96 | +0.53 | 6.98 | +0.77 | +0.02 | 7 | 7.12 |
Ca i | 5.84 | +0.26 | 5.48 | +0.05 | −0.36 | 13 | 6.34 |
Ca ii | … | … | 5.40 | −0.03 | … | 4 | 6.34 |
Sc ii | 2.25 | −0.30 | 2.08 | −0.16 | −0.17 | 7 | 3.15 |
Ti i | 5.68 | +1.44 | 3.97 | −0.07 | −1.71 | 1 | 4.95 |
Ti ii | 4.05 | −0.19 | 4.04 | +0.00 | −0.01 | 12 | 4.95 |
V ii | 3.45 | +0.23 | 3.24 | +0.22 | −0.21 | 2 | 3.93 |
Cr i | 6.02 | +1.13 | 4.71 | −0.02 | −1.31 | 10 | 5.64 |
Cr ii | 4.98 | +0.09 | 4.54 | −0.19 | −0.44 | 9 | 5.64 |
Mn i | 5.12 | +0.51 | 4.44 | −0.08 | −0.68 | 3 | 5.43 |
Fe i | 6.71 | −0.01 | 6.59 | +0.00 | −0.12 | 31 | 7.50 |
Fe ii | 6.73 | +0.01 | 6.59 | +0.00 | −0.14 | 11 | 7.50 |
Co i | 5.74 | +1.60 | 4.26 | +0.18 | −1.48 | 1 | 4.99 |
Ni i | 6.13 | +0.66 | 5.48 | +0.17 | −0.65 | 11 | 6.22 |
Cu i | 4.06 | +0.63 | ≤3.35 | ≤ +0.07 | ≤−0.71 | 1 | 4.19 |
Zn i | 4.60 | +0.78 | 3.86 | +0.21 | −0.74 | 3 | 4.56 |
Sr ii | … | … | 2.52 | +0.56 | … | 2 | 2.87 |
Y ii | 1.42 | −0.04 | 0.72 | −0.58 | −0.70 | 4 | 2.21 |
Zr ii | … | … | 1.31 | −0.36 | … | 3 | 2.58 |
Ba ii | 1.13 | −0.22 | 1.05 | −0.22 | −0.08 | 1 | 2.18 |
La ii | 0.83 | +0.39 | ≤0.31 | ≤ +0.12 | ≤−0.52 | 1 | 1.10 |
Nd ii | 1.56 | +0.84 | ≤0.44 | ≤ −0.07 | ≤−1.12 | 1 | 1.42 |
Eu ii | 0.96 | +1.23 | −0.05 | +0.34 | −1.01 | 1 | 0.52 |
Notes. K95: Klochkova (1995).
N is the number of the lines employed in our abundance determination.
The solar abundances (log ε⊙) are from Asplund et al. (2009).
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