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Rayleigh

By Nicholas Featherstone (primary-developer)1, Philip Edelmann (primary-developer)2, Rene Gassmoeller (primary-developer)3, Loren Matilsky (primary-developer)4, Ryan Orvedahl (primary-developer)5, Cian Wilson (primary-developer)6

1. Southwest Research Institute 2. Los Alamos National Lab 3. University of Florida 4. University of Colorado Boulder 5. University of California Davis 6. Carnegie DTM

Body Text

We thank the Computational Infrastructure for Geodynamics (http://geodynamics.org) which is funded by the National Science Foundation under awards EAR-0949446 and EAR-1550901.We use Rayleigh 1.0.0 ( Featherstone and Hindman, 2016; Featherstone et al., 2021) published under the GPL3 license.

Acknowledgement

We thank the Computational Infrastructure for Geodynamics (http://geodynamics.org) which is funded by the National Science Foundation under awards EAR-0949446 and EAR-1550901.

Cite Code As

Featherstone, Nicholas A., Edelmann, Philipp V. F., Gassmoeller, Rene, Matilsky, Loren I., Orvedahl, Ryan J., & Wilson, Cian R. (2021). geodynamics/Rayleigh: Rayleigh Version 1.0.0 (v1.0.0). Zenodo. https://doi.org/10.5281/zenodo.5683601

Primary References

Featherstone, N.A.; Hindman, B.W. (2016), The Spectral Amplitude Of Stellar Convection And Its Scaling In The High-Rayleigh-Number Regime, The Astrophysical Journal, 818 (1) , 32, doi: 10.3847/0004-637X/818/1/32, url: http://stacks.iop.org/0004-637X/818/i=1/a=32?key=crossref.a90f82507dd0eeb7a6e7562d1e4b0210

Secondary References

Please also cite:

Matsui, H.; Heien, E.; Aubert, J.; Aurnou, J.M.; Avery, M.; Brown, B.; Buffett, B.A.; Busse, F.; Christensen, U.R.; Davies, C.J.; Featherstone, N.; Gastine, T.; Glatzmaier, G.A.; Gubbins, D.; Guermond, J.-L.; Hayashi, Y.-Y.; Hollerbach, R.; Hwang, L.J.; Jackson, A.; Jones, C.A.; Jiang, W.; Kellogg, L.H.; Kuang, W.; Landeau, M.; Marti, P.H.; Olson, P.; Ribeiro, A.; Sasaki, Y.; Schaeffer, N.; Simitev, R.D.; Sheyko, A.; Silva, L.; Stanley, S.; Takahashi, F.; Takehiro, S.-ichi; Wicht, J.; Willis, A.P. (2016), Performance benchmarks for a next generation numerical dynamo model, Geochemistry, Geophysics, Geosystems, 17 (5) , 1586-1607, doi: 10.1002/2015GC006159, url: http://doi.wiley.com/10.1002/2015GC006159


CITE PREVIOUS VERSIONS

For previous versions, please substitute the appropriate version number, year, and DOI below. See also: https://doi.org/10.5281/zenodo.1158289

Body Text

We use Rayleigh 0.9.0 ( Featherstone and Hindman, 2016; Featherstone, 2018) published under the GPL3 license.

Acknowledgement

We thank the Computational Infrastructure for Geodynamics (http://geodynamics.org) which is funded by the National Science Foundation under awards EAR-0949446 and EAR-1550901.

Cite Code As

Featherstone, N. (2018), Rayleigh Version 0.9.0, Computational Infrastructure for Geodynamics, doi: 10.5281/zenodo.1158290, url: https://doi.org/10.5281/zenodo.1158290

Primary References

Featherstone, N.A.; Hindman, B.W. (2016), The Spectral Amplitude Of Stellar Convection And Its Scaling In The High-Rayleigh-Number Regime, The Astrophysical Journal, 818 (1) , 32, doi: 10.3847/0004-637X/818/1/32, url: http://stacks.iop.org/0004-637X/818/i=1/a=32?key=crossref.a90f82507dd0eeb7a6e7562d1e4b0210

Secondary References

Please also cite:

Matsui, H.; Heien, E.; Aubert, J.; Aurnou, J.M.; Avery, M.; Brown, B.; Buffett, B.A.; Busse, F.; Christensen, U.R.; Davies, C.J.; Featherstone, N.; Gastine, T.; Glatzmaier, G.A.; Gubbins, D.; Guermond, J.-L.; Hayashi, Y.-Y.; Hollerbach, R.; Hwang, L.J.; Jackson, A.; Jones, C.A.; Jiang, W.; Kellogg, L.H.; Kuang, W.; Landeau, M.; Marti, P.H.; Olson, P.; Ribeiro, A.; Sasaki, Y.; Schaeffer, N.; Simitev, R.D.; Sheyko, A.; Silva, L.; Stanley, S.; Takahashi, F.; Takehiro, S.-ichi; Wicht, J.; Willis, A.P. (2016), Performance benchmarks for a next generation numerical dynamo model, Geochemistry, Geophysics, Geosystems, 17 (5) , 1586-1607, doi: 10.1002/2015GC006159, url: http://doi.wiley.com/10.1002/2015GC006159