<p>The two main methods to detect the solar <em>p</em>-mode oscillations, which have a period of about 5 minutes (so frequency of ~3 milliHertz) are line of sight Doppler shift and change in irradiance.</p>

<p>The Doppler method works by measuring the intensity of light in (normally) two narrow regions either side of a prominent spectral line in the Solar spectrum and using this change to measure the velocity shift caused by the oscillations (once the solar rotation is removed). The ground-based <a href="https://gong.nso.edu/instrument/" rel="noreferrer">GONG</a> instrument uses the Ni I at 676.8nm, <a href="http://bison.ph.bham.ac.uk/index.php?page=bison,background" rel="noreferrer">BiSON</a> network and the GOLF instrument on the SOHO spacecraft both use the sodium D lines. After isolating the light around a suitable spectral feature, then you can either use a Michelson interferometer to get a velocity image of the shifts across the surface (GONG and MDI on SOHO) or a disk-averaged velocity, treating the Sun as a star (BiSON and GOLF on SOHO). The difficulties are in keeping everything stable so that the measured shifts only come from the Sun and not the instrument. For example GONG note that their optical elements are stabilized in an oven to the order of 0.00001 K.</p>

<p>The irradiance method simply involves measuring the disk-integrated intensity of the Sun and watching for changes caused by the oscillations. However fluctuations in the Earth's atmosphere make this very difficult to do from the ground and the most successful has been the <a href="https://www.pmodwrc.ch/en/research-development/space/virgo-soho/" rel="noreferrer">VIRGO instrument</a> on the SOHO spacecraft. </p>

<p>The imaging instruments have a resolution of about 2" (MDI) to 5" (GONG) so return velocity data at approx. 800,000 to 100,000 locations across the Sun. This allow the study of oscillations with very high degree (up to 1000) which have very small scale on the surface. The disk-integrated "Sun-as-a-star" instruments by comparison are sensitive to the low order oscillations.</p>

CC BY-SA 4.0
2019-02-07T22:31:21.823Z
Nice concise summary and exactly what I needed, thanks! Possibly what's needed for an answer [here](https://astronomy.stackexchange.com/q/29486/7982)?
uhoh
CC BY-SA 4.0
2019-02-07T23:21:10.370Z
I've looked at that one but don't have a good answer - photons don't come with timestamps written on them... ;-) There is also the Shapiro delay caused by the Sun's gravity but this effect (112$\micro$s) is dwarfed by the path length difference. Normally you only care about correcting the timing to the Solar System Barycenter inside the Sun; the actual size of the Sun is irrelevant since most don't observe it or near it...
astrosnapper
CC BY-SA 4.0
2019-02-07T23:48:00.030Z
When analyzing the data above, wouldn't failure to correct for light-time differences induce systematic center-to-edge phase error that would result in a redistribution of energy between modes? Trivial example; a monopole or breathing mode would look like it is happening earlier in the center than towards the edge, thereby looking like there's some energy in a quadrupole mode as well?
uhoh
CC BY-SA 4.0
2019-02-07T17:19:32.340Z
2019-02-07T17:19:32.340Z
astrosnapper
<p>Wikipedia's article <a href="https://en.wikipedia.org/wiki/Helioseismology" rel="nofollow noreferrer">Helioseismology</a> outlines several ways to analyze, data but is fairly thin on the nature of the measurements themselves.</p>

<p>Are there hundreds or thousands of high resolution spectroscopic measurements of the Doppler shift of some emission or absorption line distributed across the disk, or can this be done using low resolution spectroscopy to generate some variation in temperature or brightness?</p>

<p>I'm interested in a basic appreciation of the nature and granularity of the data (e.g. 0.1 angstrom in wavelength, 1 second of time, 1 minute of arc, etc.) and what kind of instruments collect said data. </p>

<p>The answer doesn't necessarily have to be long, just something to get me started.</p>

<the-sun>
Helioseismology of the Sun, what is actually measured?
uhoh
# Helioseismology of the Sun, what is actually measured?

(Asked by: username_0 on 2019-02-07)

Wikipedia's article [Helioseismology](https://en.wikipedia.org/wiki/Helioseismology) outlines several ways to analyze, data but is fairly thin on the nature of the measurements themselves.

Are there hundreds or thousands of high resolution spectroscopic measurements of the Doppler shift of some emission or absorption line distributed across the disk, or can this be done using low resolution spectroscopy to generate some variation in temperature or brightness?

I'm interested in a basic appreciation of the nature and granularity of the data (e.g. 0.1 angstrom in wavelength, 1 second of time, 1 minute of arc, etc.) and what kind of instruments collect said data.

The answer doesn't necessarily have to be long, just something to get me started.

**Tags:** the-sun

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## 1 answers

### Answer by username_1 on 2019-02-07. Score: 5 | Accepted answer

The two main methods to detect the solar *p*-mode oscillations, which have a period of about 5 minutes (so frequency of ~3 milliHertz) are line of sight Doppler shift and change in irradiance.

The Doppler method works by measuring the intensity of light in (normally) two narrow regions either side of a prominent spectral line in the Solar spectrum and using this change to measure the velocity shift caused by the oscillations (once the solar rotation is removed). The ground-based [GONG](https://gong.nso.edu/instrument/) instrument uses the Ni I at 676.8nm, [BiSON](http://bison.ph.bham.ac.uk/index.php?page=bison,background) network and the GOLF instrument on the SOHO spacecraft both use the sodium D lines. After isolating the light around a suitable spectral feature, then you can either use a Michelson interferometer to get a velocity image of the shifts across the surface (GONG and MDI on SOHO) or a disk-averaged velocity, treating the Sun as a star (BiSON and GOLF on SOHO). The difficulties are in keeping everything stable so that the measured shifts only come from the Sun and not the instrument. For example GONG note that their optical elements are stabilized in an oven to the order of 0.00001 K.

The irradiance method simply involves measuring the disk-integrated intensity of the Sun and watching for changes caused by the oscillations. However fluctuations in the Earth's atmosphere make this very difficult to do from the ground and the most successful has been the [VIRGO instrument](https://www.pmodwrc.ch/en/research-development/space/virgo-soho/) on the SOHO spacecraft.

The imaging instruments have a resolution of about 2" (MDI) to 5" (GONG) so return velocity data at approx. 800,000 to 100,000 locations across the Sun. This allow the study of oscillations with very high degree (up to 1000) which have very small scale on the surface. The disk-integrated "Sun-as-a-star" instruments by comparison are sensitive to the low order oscillations.

> **Comments:**
> **username_0**: Nice concise summary and exactly what I needed, thanks! Possibly what's needed for an answer [here](https://astronomy.stackexchange.com/q/29486/7982)?  
> **username_1**: I've looked at that one but don't have a good answer - photons don't come with timestamps written on them... ;-) There is also the Shapiro delay caused by the Sun's gravity but this effect (112$\micro$s) is dwarfed by the path length difference. Normally you only care about correcting the timing to the Solar System Barycenter inside the Sun; the actual size of the Sun is irrelevant since most don't observe it or near it...  
> **username_0**: When analyzing the data above, wouldn't failure to correct for light-time differences induce systematic center-to-edge phase error that would result in a redistribution of energy between modes? Trivial example; a monopole or breathing mode would look like it is happening earlier in the center than towards the edge, thereby looking like there's some energy in a quadrupole mode as well?  

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