52 
ASTRONOMY: W. W. COBLENTZ 
Proc. N. a. S. 
In the dense stars the shape of the spectral energy curve, and hence 
our inference of the effective temperature is determined by the spectral 
emissivity of the surface; while in the less dense stars the radiation ema- 
nates from great depths. 
e Ononis 
/3 Orionis 
a Lyrae 
a Canis 
Majoris 
a Cygnii 
a Aquilae 
a Canis 
Minoris 
a Aurigae 
a Bootis 
/3 Gemino- 
rum 
a Tauri 
a Orionis 
a Scorpii 
Bo 
B8p 
Ao 
Ao 
A2 
A5 
F5 
Go 
Ko 
Ko 
K5 
Ma 
Map 
TABI.E 1 
Stellar Temperatures 
Calculated 
13000 
to 
14000° K 
10000 
to 
12000 
8000 
to 
10000 
8000 
to 
11000 
8000 
to 
10000 
7000 
to 
9000 
5500 
to 
7500 
5300 
to 
6500 
3500 
to 
4500 
4500 
to 
7000 
2800 
to 
4500 
2800 
to 
3300 
2500 
to 
3200 
COBLENTZ 
Class Go as 
Standard 
13000° K 
10000 
8000 
8000 
9000 
8000 
6000 
6000 
4000 
5500 
3500 
3000 
3000 
WILSING, NORDMANN 
SCHEINER & NORDMANN 
& MUNCH LEMORVAN 
9400° K 
12200° K 
9400 
8100 
7200 
7100 
3700 
4900 
3500 
3000 
3600 
3500 
