29. G5
The spectral type (except for the supergiants) is determined from the ratios 4144: H and 4096: H and the blend at 4030-4034; the violet side of the G band. On spectrograms of low dispersion H appears to be stronger in dwarfs of this class than in giants and sub-giants.
Star | MKK | a | m | HD | Notes | |
µ Cas.... | G5 V | 01:01 | +54°26' | 5.3 | G5 | 1 |
Cet..... | G5 V | 03:14 | +03 00 | 5.0 | G5 | |
UMa... | G5 II | 08:22 | +61 03 | 3.5 | G0 | |
Crv..... | G5 II | 12:29 | -22 51 | 2.8 | G5 | |
Hya..... | G5 III | 13:13 | -22 39 | 3.3 | G5 | |
70 Vir.... | G5 IV-V | 13:23 | +14 19 | 5.2 | G0 | 2 |
Her..... | G5 II-III | 16:25 | +21 42 | 2.8 | K0 | |
Her..... | G5 III | 16:39 | +39 07 | 3.6 | K0 | |
µ Her..... | G5 IV | 17:42 | +27 47 | 3.5 | G5 | |
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: 4077, 4063: 4077, 4144: 4077, 4085: 4077, 4250: 4215, 4226: 4045, and the relative intensity of the continuous spectrum on each side of 4215.
High resolution image |
High resolution image |
High resolution image |