Galactic disc profiles and a universal angular momentum distribution from statistical physics
We show that the stellar surface brightness profiles in disc galaxies - observed to be approximately exponential - can be explained if radial migration efficiently scrambles the individual stars’ angular momenta while conserving the circularity of the orbits and the total mass and angular momentum....
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| Hauptverfasser: | , , |
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| Dokumenttyp: | Article (Journal) |
| Sprache: | Englisch |
| Veröffentlicht: |
09 February 2017
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| In: |
Monthly notices of the Royal Astronomical Society
Year: 2017, Jahrgang: 467, Heft: 4, Pages: 5022-5032 |
| ISSN: | 1365-2966 |
| DOI: | 10.1093/mnras/stx352 |
| Online-Zugang: | Verlag, lizenzpflichtig, Volltext: https://doi.org/10.1093/mnras/stx352
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| Verfasserangaben: | Jakob Herpich, Scott Tremaine and Hans-Walter Rix |
MARC
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| 520 | |a We show that the stellar surface brightness profiles in disc galaxies - observed to be approximately exponential - can be explained if radial migration efficiently scrambles the individual stars’ angular momenta while conserving the circularity of the orbits and the total mass and angular momentum. In this case, the disc's distribution of specific angular momenta j should be near a maximum entropy state and therefore approximately exponential, $\textrm{d}\!{N} \propto \exp (-j/\langle j\rangle ) \textrm{d}\!{j}$. This distribution translates to a surface density profile that is generally not an exponential function of radius: $\Sigma (R) \propto \exp \left[-R/R_{\rm e}({\scriptstyle {R}})\right]/ \left(R R_{\rm e}({\scriptstyle {R}})\right)\left(1+\textrm{d}\!{\,\log v_\mathrm{c} (R)}/ \textrm{d}\!{\,\log R}\right),$ for a rotation curve v∞(R) and $R_{\rm e}({\scriptstyle {R}})\equiv \langle j\rangle /v_\mathrm{c} (R)$. We show that such a profile matches the observed surface brightness profiles of disc-dominated galaxies just as well as the empirical exponential profile. Disc galaxies that exhibit population gradients cannot have fully reached a maximum-entropy state but appear to be close enough that their surface brightness profiles are well fit by this idealized model. | ||
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