<p>The key for stellar classification is the <a href="https://en.wikipedia.org/wiki/Hertzsprung%E2%80%93Russell_diagram" rel="nofollow noreferrer">Hertzsprung-Russell diagram</a> (or <em>HRD</em> for brevity), also know as the <em>color-magnitude diagram</em>.
<img src="https://i.sstatic.net/DQ8fd.png" alt="H-R diagram"></p>

<p>This shows the relation between the surface temperature (on the x-axis) of a star and its luminosity (on the y-axis). The temperature is an index of the <a href="http://www.uni.edu/morgans/astro/course/Notes/section2/spectraltemps.html" rel="nofollow noreferrer">Spectral type</a>. For distant stars also spectroscopy is taken into account, to classify spectral types according to their absorption lines <a href="http://hyperphysics.phy-astr.gsu.edu/hbase/starlog/staspe.html" rel="nofollow noreferrer">here some examples</a>. The usual classification is called MKK (from the astronomers that had developed it - Morgan, Keenan and Kellman in 1943), and divides the stars in 7 stellar types O, B, A, F, G, K, M. Please note that from the 1943 other stellar types have added, but these are the most used. This sequence goes from the hottest (O) to coolest (M) stars. Each letter class is then subdivided using a numeric digit with 0 being hottest and 9 being coolest. Our Sun is a G2 type star. This classification also uses an additional notation to avoid the "degeneracy" you mentioned: a roman numeral between "I" (one) and "V" (five). The higher the number, the wider the lines in the observed spectrum. However, despite of the quantity these roman numbers indicate, they are an index of <strong>luminosity class</strong>. This is based on the width of certain absorption lines in the star's spectrum which vary with the density of the atmosphere and so distinguish giant stars from dwarfs. Luminosity class I stars are supergiants, class III regular giants, and class V dwarfs or main-sequence stars, with II for bright giants, IV for sub-giants, and VI for sub-dwarfs (<a href="https://en.wikipedia.org/wiki/Stellar_classification" rel="nofollow noreferrer">from here</a>). Then, our Sun is "completely" identified by the type G2V. You can take a look at the figure below, and check out by yourself where it belongs:
<img src="https://i.sstatic.net/BBYuw.png" alt="H-R diagram 2">.
Also note that other indexes are used to characterize the stars, as for the width of the lines in the luminosity class, or for some <a href="https://en.wikipedia.org/wiki/Stellar_classification#Spectral_peculiarities" rel="nofollow noreferrer">peculiarities</a>.</p>

<p>Finally, if you are interested in the study of stars, you should always keep in mind the <a href="https://en.wikipedia.org/wiki/Stefan%E2%80%93Boltzmann_law#Temperature_of_stars" rel="nofollow noreferrer">Stefan-Boltzmann law</a>:</p>

<p>$L=4\pi\sigma R^2 T^4$</p>

<p>By this you can identify isoradii lines in the HR diagram:</p>

<p><img src="https://i.sstatic.net/iN7tT.png" alt="The red cross is our Sun"></p>

<p>Also, there is a proportionality between luminosity and mass:</p>

<p>$L\sim M^{3.5}$</p>

<p>Then you can identify "isomasses" lines in the HR diagram, but I can't find such a figure to show.</p>

CC BY-SA 3.0
2014-03-17T03:51:29.193Z
2014-07-10T03:38:38.923Z
2014-07-10T03:38:38.923Z
Py-ser
<p>consider two stars of the spectral type and subtype, but not necessarily both on the main sequence. Describe whether this information is sufficient to tell you how the stars differ in surface temperature, size, and distance?</p>

<p>so if they have they same spectral type and subtype i think they're supposed to have the same surface temperature. however this is not enough information to tell us about their sizes and distances. is this correct? any insight would be great, thanks!</p>

CC BY-SA 3.0
2014-03-15T09:33:50.430Z
What do you mean by "subtype"? However, the luminosity is also to be taken into account to discriminate among different types of stars.
Py-ser
CC BY-SA 3.0
2014-03-15T23:56:22.860Z
i think it's referring to the spectral class and then each class further divided into the numbers 0-9.
rawrPanda
CC BY-SA 3.0
2014-03-16T06:49:53.240Z
What do you mean you **think** it is referring to the spectral class with numbers - it is **your** question!
Jeremy
CC BY-SA 3.0
2014-03-16T19:43:47.140Z
Right, so this is a homework question out of *The Cosmos*...
Jeremy
<star>
regarding spectral type of a star
rawrPanda
# regarding spectral type of a star

(Asked by: username_0 on 2014-03-14)

consider two stars of the spectral type and subtype, but not necessarily both on the main sequence. Describe whether this information is sufficient to tell you how the stars differ in surface temperature, size, and distance?

so if they have they same spectral type and subtype i think they're supposed to have the same surface temperature. however this is not enough information to tell us about their sizes and distances. is this correct? any insight would be great, thanks!

**Tags:** star
> **Comments:**
> **username_1**: What do you mean by "subtype"? However, the luminosity is also to be taken into account to discriminate among different types of stars.  
> **username_0**: i think it's referring to the spectral class and then each class further divided into the numbers 0-9.  
> **username_2**: What do you mean you **think** it is referring to the spectral class with numbers - it is **your** question!  
> **username_2**: Right, so this is a homework question out of *The Cosmos*...  

---

## 1 answers

### Answer by username_1 on 2014-03-17. Score: 2 | Accepted answer

The key for stellar classification is the [Hertzsprung-Russell diagram](https://en.wikipedia.org/wiki/Hertzsprung%E2%80%93Russell_diagram) (or *HRD* for brevity), also know as the *color-magnitude diagram*.
![H-R diagram](https://i.sstatic.net/DQ8fd.png)

This shows the relation between the surface temperature (on the x-axis) of a star and its luminosity (on the y-axis). The temperature is an index of the [Spectral type](http://www.uni.edu/morgans/astro/course/Notes/section2/spectraltemps.html). For distant stars also spectroscopy is taken into account, to classify spectral types according to their absorption lines [here some examples](http://hyperphysics.phy-astr.gsu.edu/hbase/starlog/staspe.html). The usual classification is called MKK (from the astronomers that had developed it - Morgan, Keenan and Kellman in 1943), and divides the stars in 7 stellar types O, B, A, F, G, K, M. Please note that from the 1943 other stellar types have added, but these are the most used. This sequence goes from the hottest (O) to coolest (M) stars. Each letter class is then subdivided using a numeric digit with 0 being hottest and 9 being coolest. Our Sun is a G2 type star. This classification also uses an additional notation to avoid the "degeneracy" you mentioned: a roman numeral between "I" (one) and "V" (five). The higher the number, the wider the lines in the observed spectrum. However, despite of the quantity these roman numbers indicate, they are an index of **luminosity class**. This is based on the width of certain absorption lines in the star's spectrum which vary with the density of the atmosphere and so distinguish giant stars from dwarfs. Luminosity class I stars are supergiants, class III regular giants, and class V dwarfs or main-sequence stars, with II for bright giants, IV for sub-giants, and VI for sub-dwarfs ([from here](https://en.wikipedia.org/wiki/Stellar_classification)). Then, our Sun is "completely" identified by the type G2V. You can take a look at the figure below, and check out by yourself where it belongs:
![H-R diagram 2](https://i.sstatic.net/BBYuw.png).
Also note that other indexes are used to characterize the stars, as for the width of the lines in the luminosity class, or for some [peculiarities](https://en.wikipedia.org/wiki/Stellar_classification#Spectral_peculiarities).

Finally, if you are interested in the study of stars, you should always keep in mind the [Stefan-Boltzmann law](https://en.wikipedia.org/wiki/Stefan%E2%80%93Boltzmann_law#Temperature_of_stars):

$L=4\pi\sigma R^2 T^4$

By this you can identify isoradii lines in the HR diagram:

![The red cross is our Sun](https://i.sstatic.net/iN7tT.png)

Also, there is a proportionality between luminosity and mass:

$L\sim M^{3.5}$

Then you can identify "isomasses" lines in the HR diagram, but I can't find such a figure to show.


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