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.
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| High resolution image |
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| High resolution image |
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| High resolution image |
