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29. G5

The spectral type (except for the supergiants) is determined from the ratios lambda 4144: Hdelta and lambda 4096: Hdelta and the blend at lambda 4030-4034; the violet side of the G band. On spectrograms of low dispersion Hdelta appears to be stronger in dwarfs of this class than in giants and sub-giants.

TABLE 24
STANDARDS AT G5

Star MKK a delta m HD Notes

µ Cas.... G5 V 01:01 +54°26' 5.3 G5 1
kappa Cet..... G5 V 03:14 +03 00 5.0 G5
omicron UMa... G5 II 08:22 +61 03 3.5 G0
beta Crv..... G5 II 12:29 -22 51 2.8 G5
gamma Hya..... G5 III 13:13 -22 39 3.3 G5
70 Vir.... G5 IV-V 13:23 +14 19 5.2 G0 2
beta Her..... G5 II-III 16:25 +21 42 2.8 K0
eta Her..... G5 III 16:39 +39 07 3.6 K0
µ Her..... G5 IV 17:42 +27 47 3.5 G5
xi Her..... G5 III 17:53 +29 16 3.8 K0

NOTES
1. Considerably fainter spectroscopically than other dwarfs in table.
2. The star appears to be definitely less luminous than µ Her.

4226: lambda 4077, lambda 4063: lambda 4077, lambda 4144: lambda 4077, lambda 4085: lambda 4077, lambda 4250: lambda 4215, lambda 4226: lambda 4045, and the relative intensity of the continuous spectrum on each side of lambda 4215.

Plate 41. Luminosity Effects at G5
Plate 41
High resolution image

Plate 42. The High-Velocity Star Boss 2527
Plate 42
High resolution image

Plate 43. The Variable Star V Vul
Plate 43
High resolution image

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