Entropy and Mass Distribution in Disc Galaxies

被引:5
|
作者
Marr, John Herbert [1 ]
机构
[1] Unit Computat Sci, Bldg 250,Babraham Res Campus, Cambridge CB22 3AT, England
来源
GALAXIES | 2020年 / 8卷 / 01期
关键词
galaxies; kinematics and dynamics; spiral; lognormal density distribution; entropy; DISCREPANCY-ACCELERATION RELATION; MODIFIED NEWTONIAN DYNAMICS; RESOLUTION ROTATION CURVES; TULLY-FISHER RELATION; ANGULAR-MOMENTUM; DARK-MATTER; DWARF GALAXIES; DENSITY; PROFILES; VELOCITY;
D O I
10.3390/galaxies8010012
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
The relaxed motion of stars and gas in galactic discs is well approximated by a rotational velocity that is a function of radial position only, implying that individual components have lost any information about their prior states. Thermodynamically, such an equilibrium state is a microcanonical ensemble with maximum entropy, characterised by a lognormal probability distribution. Assuming this for the surface density distribution yields rotation curves that closely match observational data across a wide range of disc masses and galaxy types and provides a useful tool for modelling the theoretical density distribution in the disc. A universal disc spin parameter emerges from the model, giving a tight virial mass estimator with strong correlation between angular momentum and disc mass, suggesting a mechanism by which the proto-disc developed by dumping excess mass to the core or excess angular momentum to a satellite galaxy. The baryonic-to-dynamic mass ratio for the model approaches unity for high mass galaxies, but is generally <1 for low mass discs, and this discrepancy appears to follow a similar relationship to that shown in recent work on the Radial Acceleration Relation (RAR). Although this may support Modified Newtonian Dynamics (MOND) in preference to a Dark Matter (DM) halo, it does not exclude undetected baryonic mass or a gravitational DM component in the disc.
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页数:16
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