<p>Some classical Cepheids pulsate simultaneously in two or even three modes.
Their lightcurves can be explained as a overposition of fundamental plus overtone modes.</p>

<p><img src="https://i.sstatic.net/u7TjS.gif" alt="enter image description here"></p>

<p>The terminology you used is also found <a href="http://www.google.co.jp/url?sa=t&amp;rct=j&amp;q=&amp;esrc=s&amp;source=web&amp;cd=1&amp;cad=rja&amp;uact=8&amp;ved=0CCgQFjAA&amp;url=http://mnras.oxfordjournals.org/content/286/3/L33.full.pdf&amp;ei=GgJ_U7-YL8yA8gWZm4DoAQ&amp;usg=AFQjCNFiZaxYDMa-kXosuP-7fEv4jWf6HA&amp;sig2=ECz3B_Rh2BWLhqBpCvmyqQ&amp;bvm=bv.67720277,d.dGc" rel="nofollow noreferrer">in this paper</a> (where you have also other references):
"the discovery of many double-mode Cepheids (DMCs) pulsating in both the fundamental and first-overtone modes (F/10) and the first and second-overtone modes (10/20)"</p>

<p>Other reference: <a href="http://ogle.astrouw.edu.pl/atlas/classical_Cepheids.html" rel="nofollow noreferrer">Classical cepheids</a></p>

CC BY-SA 3.0
2014-05-23T08:56:34.663Z
Okay. What is this pulsation basically? A brief explanation please.
MycrofD
CC BY-SA 3.0
2014-05-23T09:19:32.213Z
What do you mean? Don't you know about cepheid pulsation?
Py-ser
CC BY-SA 3.0
2014-05-23T09:31:00.427Z
I kind of wanted that.
MycrofD
CC BY-SA 3.0
2014-05-23T09:36:35.487Z
I am sorry, I can't understand. Please try to be more "wordy" :)
Py-ser
CC BY-SA 3.0
2014-05-23T09:41:09.107Z
Stellar pulsations are caused by expansions and contractions in the outer layers as a star seeks to maintain equilibrium.
What kind of equilibrium is being referred to here?
MycrofD
CC BY-SA 3.0
2014-05-23T10:34:51.477Z
I am pretty convinced it is just observational decomposition, but I can not confirm this for sure. Perhaps, radial and non radial contemporary pulsations could induce those modes. But I am not an expert at all of cepheids.
Py-ser
CC BY-SA 3.0
2014-05-28T09:04:02.170Z
Ok. I found that the equilibrium sought for is between gravitational pressure and radiation pressure. Got it! :)
MycrofD
CC BY-SA 3.0
2014-05-23T08:12:10.503Z
2014-05-23T08:12:10.503Z
Py-ser
<p>[In addition to the answer already provided by Py-ser]</p>

<p>In the body of a Cepheid, there is a regular or periodical variation of difference between the gravitational pressure and radiation pressure. This radiation pressure is due to the consumption of fuel in it, lighter elements like hydrogen and helium undergoing nuclear fusion into forming heavier elements. The gravitational pressure occurs of course due to the elements and compounds in the star. </p>

<p>One increases, then decreases, equals the other and then further decreases, and again increases and this happens periodically. This equilibrium between both the pressures is being referred to here.</p>

CC BY-SA 3.0
2014-07-14T13:03:56.090Z
2014-07-14T13:03:56.090Z
MycrofD
<p><strong>Cepheid pulsations</strong></p>

<p>The basic description of the mechanism behind Cepheid pulsations is given <a href="https://en.wikipedia.org/wiki/Cepheid_variable#Dynamics_of_the_pulsation">here</a>:</p>

<blockquote>
  <p>The accepted explanation for the pulsation of Cepheids is called the Eddington valve,[38] or κ-mechanism, where the Greek letter κ (kappa) denotes gas opacity. Helium is the gas thought to be most active in the process. Doubly ionized helium (helium whose atoms are missing two electrons) is more opaque than singly ionized helium. The more helium is heated, the more ionized it becomes. At the dimmest part of a Cepheid's cycle, the ionized gas in the outer layers of the star is opaque, and so is heated by the star's radiation, and due to the increased temperature, begins to expand. As it expands, it cools, and so becomes less ionized and therefore more transparent, allowing the radiation to escape. Then the expansion stops, and reverses due to the star's gravitational attraction. The process then repeats.</p>
</blockquote>

<p>I can't really describe it much better than this, but let me know if it needs to be made more clear.</p>

<p>Note that this mechanism isn't restricted to helium II/III.  Other classes of variable star operate in the same way. e.g. RR Lyraes and $\beta$ Cepheids.</p>

<p><strong>The equilibrium state of stars</strong></p>

<p>In all phases, stars are presumed to be in <em>hydrostatic equilibrium</em>: the outward force of pressure in the star (from the gas, radiation and sometimes electron or neutron degeneracy) is precisely balanced by the inward force of gravity. In many phases, we can additional regard the star as being in <em>local thermodynamic equilibrium</em>.  What we really mean here is that the star is not generating (or absorbing) energy through expansion and contraction.  This isn't true for, say, pre-main-sequence stars, which are only generating energy by their contraction toward the main sequence.</p>

<p>Cepheid pulsations are oscillations about the equilibrium state.  They aren't linearly stable but the non-linear components mean that the oscillations aren't big enough to tear the star apart.  The calculation of the frequencies is either a tricky sixth-order eigenvalue problem or a simulation of the oscillation from which the frequencies can be determined by analysing the output.</p>

<p>Which modes are excited is a similarly complicated problem.  There are many things we haven't actually solved!  But you can think of the system as a driven, damped oscillator. The driving is given by the opacity mechanism described above, and the damping is related to the equilibrium structure of the star. So, the excited modes are usually around where these match best, which may happen to be the fundamental mode (where the entire star expands or contracts as a whole) or the overtones (where different layers are expanding or contracting).</p>

CC BY-SA 3.0
2014-07-15T05:48:02.197Z
2014-07-15T05:48:02.197Z
Warrick
<p>There are various modes of Cepheids like</p>

<ul>
<li>single modes: 
   fundamental (F), 
   first overtone (1O), and likewise.</li>
</ul>

<p>And then we have </p>

<ul>
<li>double modes: F/1O, 1O/2O etc.</li>
<li>triple modes: 1O/2O/3O etc.</li>
</ul>

<p>What are these <code>modes</code> actually? What do they mean and which frequencies do they correspond to?</p>

<p><code>Stellar pulsations</code> are caused by <code>expansions</code> and <code>contractions</code> in the outer layers as a star seeks to maintain equilibrium. <strong>What kind of <em>equilibrium</em> is being referred to here?</strong></p>

<galaxy><stellar-evolution><star-systems><stellar-dynamics><cepheids>
Pulsation Modes of Cepheids
MycrofD
# Pulsation Modes of Cepheids

(Asked by: username_0 on 2014-05-21)

There are various modes of Cepheids like

* single modes:
  fundamental (F),
  first overtone (1O), and likewise.

And then we have

* double modes: F/1O, 1O/2O etc.
* triple modes: 1O/2O/3O etc.

What are these `modes` actually? What do they mean and which frequencies do they correspond to?

`Stellar pulsations` are caused by `expansions` and `contractions` in the outer layers as a star seeks to maintain equilibrium. **What kind of *equilibrium* is being referred to here?**

**Tags:** galaxy, stellar-evolution, star-systems, stellar-dynamics, cepheids


---

## 3 answers

### Answer by username_2 on 2014-07-15. Score: 5 | Accepted answer

**Cepheid pulsations**

The basic description of the mechanism behind Cepheid pulsations is given [here](https://en.wikipedia.org/wiki/Cepheid_variable#Dynamics_of_the_pulsation):

> The accepted explanation for the pulsation of Cepheids is called the Eddington valve,[38] or κ-mechanism, where the Greek letter κ (kappa) denotes gas opacity. Helium is the gas thought to be most active in the process. Doubly ionized helium (helium whose atoms are missing two electrons) is more opaque than singly ionized helium. The more helium is heated, the more ionized it becomes. At the dimmest part of a Cepheid's cycle, the ionized gas in the outer layers of the star is opaque, and so is heated by the star's radiation, and due to the increased temperature, begins to expand. As it expands, it cools, and so becomes less ionized and therefore more transparent, allowing the radiation to escape. Then the expansion stops, and reverses due to the star's gravitational attraction. The process then repeats.

I can't really describe it much better than this, but let me know if it needs to be made more clear.

Note that this mechanism isn't restricted to helium II/III. Other classes of variable star operate in the same way. e.g. RR Lyraes and $\beta$ Cepheids.

**The equilibrium state of stars**

In all phases, stars are presumed to be in *hydrostatic equilibrium*: the outward force of pressure in the star (from the gas, radiation and sometimes electron or neutron degeneracy) is precisely balanced by the inward force of gravity. In many phases, we can additional regard the star as being in *local thermodynamic equilibrium*. What we really mean here is that the star is not generating (or absorbing) energy through expansion and contraction. This isn't true for, say, pre-main-sequence stars, which are only generating energy by their contraction toward the main sequence.

Cepheid pulsations are oscillations about the equilibrium state. They aren't linearly stable but the non-linear components mean that the oscillations aren't big enough to tear the star apart. The calculation of the frequencies is either a tricky sixth-order eigenvalue problem or a simulation of the oscillation from which the frequencies can be determined by analysing the output.

Which modes are excited is a similarly complicated problem. There are many things we haven't actually solved! But you can think of the system as a driven, damped oscillator. The driving is given by the opacity mechanism described above, and the damping is related to the equilibrium structure of the star. So, the excited modes are usually around where these match best, which may happen to be the fundamental mode (where the entire star expands or contracts as a whole) or the overtones (where different layers are expanding or contracting).


---

### Answer by username_1 on 2014-05-23. Score: 7

Some classical Cepheids pulsate simultaneously in two or even three modes.
Their lightcurves can be explained as a overposition of fundamental plus overtone modes.

![enter image description here](https://i.sstatic.net/u7TjS.gif)

The terminology you used is also found [in this paper](http://www.google.co.jp/url?sa=t&rct=j&q=&esrc=s&source=web&cd=1&cad=rja&uact=8&ved=0CCgQFjAA&url=http://mnras.oxfordjournals.org/content/286/3/L33.full.pdf&ei=GgJ_U7-YL8yA8gWZm4DoAQ&usg=AFQjCNFiZaxYDMa-kXosuP-7fEv4jWf6HA&sig2=ECz3B_Rh2BWLhqBpCvmyqQ&bvm=bv.67720277,d.dGc) (where you have also other references):
"the discovery of many double-mode Cepheids (DMCs) pulsating in both the fundamental and first-overtone modes (F/10) and the first and second-overtone modes (10/20)"

Other reference: [Classical cepheids](http://ogle.astrouw.edu.pl/atlas/classical_Cepheids.html)

> **Comments:**
> **username_0**: Okay. What is this pulsation basically? A brief explanation please.  
> **username_1**: What do you mean? Don't you know about cepheid pulsation?  
> **username_0**: I kind of wanted that.  
> **username_1**: I am sorry, I can't understand. Please try to be more "wordy" :)  
> **username_0**: Stellar pulsations are caused by expansions and contractions in the outer layers as a star seeks to maintain equilibrium. What kind of equilibrium is being referred to here?  
> **username_1**: I am pretty convinced it is just observational decomposition, but I can not confirm this for sure. Perhaps, radial and non radial contemporary pulsations could induce those modes. But I am not an expert at all of cepheids.  
> **username_0**: Ok. I found that the equilibrium sought for is between gravitational pressure and radiation pressure. Got it! :)  

---

### Answer by username_0 on 2014-07-14. Score: 1

[In addition to the answer already provided by username_1]

In the body of a Cepheid, there is a regular or periodical variation of difference between the gravitational pressure and radiation pressure. This radiation pressure is due to the consumption of fuel in it, lighter elements like hydrogen and helium undergoing nuclear fusion into forming heavier elements. The gravitational pressure occurs of course due to the elements and compounds in the star.

One increases, then decreases, equals the other and then further decreases, and again increases and this happens periodically. This equilibrium between both the pressures is being referred to here.


---

