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Table 2

Basic stellar parameters, silicon abundance, and 28Si/29Si and 28Si/30Si ratios of the K–M giants and optically bright red supergiants in our sample.

Name T eff log 1 L M MARCS model
(K) (cm s-2) (L) (M) Teff /log 1 /Mmicro /[Fe/H] log ASi 28Si/29Si 28Si/30Si

K–M giants
α Boo 4275 ± 50a + 1.7 ± 0.1a 198 ± 3b 1.1 ± 0.2a 4250/1.5/1.0/2.0/− 0.5 7.5 ± 0.1 15 ± 5 25 ± 10
γ Cru 3630 ± 90 + 0.9 ± 0.1 820 ± 80 1.5 ± 0.3 3600/1.0/1.0/2.0/+0.0 7.5 ± 0.2 15 ± 5 25 ± 10
σ Lib 3596 ± 100c +0.7 ± 0.1d c 2.2 ± 0.5c 3600/0.5/1.0/2.0/+0.0 7.5 ± 0.2 30 ± 10 50 ± 20
V806 Cen 3360 ± 190 + 0.4 ± 0.2 780 ± 80 0.8 ± 0.3 3400/0.5/1.0/2.0/+0.0 7.5 ± 0.3 15 ± 5 25 ± 10
ε Mus 3390 ± 190 + 0.6 ± 0.1 1840 ± 190 1.5 ± 0.5 3400/0.5/1.0/2.0/+0.0 7.5 ± 0.3 15 ± 5 50 ± 20
L2 Pup 2770 ± 150 − 0.3 ± 0.2 1480 ± 240 0.5 ± 0.2 2800/0.0/0.5/2.0/+0.0
θ Aps 2850 ± 160 − 0.3 ± 0.1 3050 ± 460 1.0 ± 0.3 2800/0.0/1.0/2.0/+0.0

Red supergiants
α Ori 3690 ± 54e − 0.3 ± 0.3f g 20 ± 5g 3600/0.0/5.0/5.0/+0.0 7.45i 20i 25j
α Sco 3660 ± 120h −0.2 ± 0.3h h 15 ± 5h 3600/0.0/5.0/5.0/+0.0 7.44i 13i 25j
α Her 3293 ± 100c + 0.0 ± 1.5d c 5.0 ± 2.0c 3300/0.0/5.0/2.0/+0.0 7.26i 20i 29i

Notes.The values taken from the literature are marked with references, while the values without notes were derived in the present work as described in Sect. 4.

Reference.

(a)

Smith et al. (2013).

(b)

Based on the bolometric flux from Lacour et al. (2008) and the parallax from van Leeuwen (2007).

(c)

Tsuji (2008).

(d)

Derived from the absolute bolometric magnitude, Teff, and M in Tsuji (2008).

(e)

Ohnaka et al. (2011).

(f)

Derived from M and the radius in Harper et al. (2008).

(g)

Harper et al. (2008).

(h)

Ohnaka et al. (2013).

(i)

Tsuji et al. (1994).

(j)

Assumed.

(†)

Heavily CN-cycled composition.

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