Sigma-D relation: Difference between revisions
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The '''Sigma-D relation''', or '''Σ-D Relation''', is the claimed relation between the radio [[surface brightness]] and [[diameter]] of a [[supernova remnant]]. It is generally regarded as of limited physical use, since it has very large scatter and is dominated by observational selection biases.<ref>{{Cite journal |last=Green |first=D. A. |date=1991-02-01 |title=Limitations Imposed on Statistical Studies of Galactic Supernova Remnants by Observational Selection Effects |url=https://ui.adsabs.harvard.edu/abs/1991PASP..103..209G |journal=Publications of the Astronomical Society of the Pacific |volume=103 |pages=209 |doi=10.1086/132810 |issn=0004-6280}}</ref><ref>{{Cite journal |last=Green |first=D. A. |date=2005-01-01 |title=Some statistics of Galactic SNRs |url=https://ui.adsabs.harvard.edu/abs/2005MmSAI..76..534G |journal=Memorie della Societa Astronomica Italiana |volume=76 |pages=534–541 |doi=10.48550/arXiv.astro-ph/0505428 |issn=0037-8720}}</ref> |
The '''Sigma-D relation''', or '''Σ-D Relation''', is the claimed relation between the radio [[surface brightness]] and [[diameter]] of a [[supernova remnant]]. It is generally regarded as of limited physical use, since it has very large scatter and is dominated by observational selection biases.<ref>{{Cite journal |last=Green |first=D. A. |date=1991-02-01 |title=Limitations Imposed on Statistical Studies of Galactic Supernova Remnants by Observational Selection Effects |url=https://ui.adsabs.harvard.edu/abs/1991PASP..103..209G |journal=Publications of the Astronomical Society of the Pacific |volume=103 |pages=209 |doi=10.1086/132810 |issn=0004-6280}}</ref><ref>{{Cite journal |last=Green |first=D. A. |date=2005-01-01 |title=Some statistics of Galactic SNRs |url=https://ui.adsabs.harvard.edu/abs/2005MmSAI..76..534G |journal=Memorie della Societa Astronomica Italiana |volume=76 |pages=534–541 |doi=10.48550/arXiv.astro-ph/0505428 |issn=0037-8720}}</ref> |
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Revision as of 18:14, 30 July 2024
The Sigma-D relation, or Σ-D Relation, is the claimed relation between the radio surface brightness and diameter of a supernova remnant. It is generally regarded as of limited physical use, since it has very large scatter and is dominated by observational selection biases.[1][2]
See also
References
- ^ Green, D. A. (1991-02-01). "Limitations Imposed on Statistical Studies of Galactic Supernova Remnants by Observational Selection Effects". Publications of the Astronomical Society of the Pacific. 103: 209. doi:10.1086/132810. ISSN 0004-6280.
- ^ Green, D. A. (2005-01-01). "Some statistics of Galactic SNRs". Memorie della Societa Astronomica Italiana. 76: 534–541. doi:10.48550/arXiv.astro-ph/0505428. ISSN 0037-8720.
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