The GYRE Forums

Fair enough! I closed my issue.

I ran into this and instinctively opened an issue on GitHub but realised I should probably stick to the forum. This is a copy of what I wrote there, though having looked at the code, I'm not sure how easily I'd be able to restore the old behaviour. I've just noticed that as of GYRE 6.0 and 6.0.1, th...

Hi Benard, The HDF5 library is provided with the SDK so you shouldn't need to add system paths to find it. On our cluster, I add the SDK paths to LIBRARY_PATH and LD_LIBRARY_PATH, for which I use: export LIBRARY_PATH="$MESASDK_ROOT/lib64:$MESASDK_ROOT/lib:$LIBRARY_PATH" export LD_LIBRARY_PATH="$MESA...

Hi Rich,

The URL in the GitHub repo still autoforwards to the Bitbucket repo, which is apparently no longer supported. I just get a page that says "Repository unavailable: Bitbucket no longer supports Mercurial repositories." I presume you want to link to docs at Read the Docs.

Cheers,
Warrick

Rich has already explained why the calculation is inescapably slow but I'm curious about your models. Specifically, I'd say they don't actually include the structure of the neutron star. e.g. in ns10.GYRE, there's a point at the centre and then the remaining structure starts from 10⁶ cm (= 10 km). T...

Your calculation of the dynamical timescale τ is basically correct but subtly depends on whether its defined as an angular or cyclic frequency, from which we get a factor of 2π. You've also missed out that the frequencies are being reported in μHz. So to get from 'Re(omega)' to 'Re(freq)' you need t...

The control is freq_min_units, not freq_units. You can set freq_max_units to be something different, otherwise I think the default is to use the same units as freq_min_units.

Cheers,
Warrick

At this point, your questions aren't really about GYRE but about stellar oscillation theory in general. You may want to consult some course notes or your advisor. I recommend the notes by Jørgen Christensen-Dalsgaard . In Section 5.3.3, he discusses mixed modes in the star η Boo. Fig. 5.19 (eigenfun...

What's the radius of your stellar model compared to the entry for α Boo in that table? How would that affect νmax? I'm deliberately baiting you into computing νmax of your model for the sake of your own understanding. That is, I don't think it's helpful for me to just tell you what νmax is for your ...

Gyre_Beginner wrote: ↑

Thu Dec 05, 2019 10:16 am

For the frequency scan I used freq_min = 3 microhertz and freq_max = 4 microhertz since the frequency of maximum oscillation power v_max = 3.47 microhertz for the star I want to investigate.

How exactly did you estimate νmax?