Possible explanation for the surface brightness profile of the stellar disk

Kang, Dong-Biao; Cui, Lang

doi:10.1140/epjp/i2015-15189-x

Cited by 1 publication

(8 citation statements)

References 35 publications

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“…indicating a much steeper slope. Figure 2 The SBP of NGC3631 (cited from [30]) fitted by equations in [25] (Kang15) and Equation (28) in this work (Kang24). The root mean squared error of Kang15 and Kang24 is 0.565 and 0.351, respectively.…”

Section: Effect Of the Central Bodymentioning

confidence: 89%

“…If α ̸ = 0, ρ is a linear combination of the first kind of Bessel J function and the second kind of Bessel function. The numerical solution, as discussed in [25], shows that ρ(R) can still be well approximated by the logarithmic form (13). This logarithmic function, inverse to the exponential function, depicts a straight line over certain intervals in surface brightness profile plots, leading us to propose the log model for describing the downbending exponential profile.…”

Section: Effect Of the Central Bodymentioning

confidence: 91%

“…Let us first review our previous work [25]. By virtue of the large radial-to-vertical scale ratio of the disk [27] and for the purpose of simplifying the issue, we calculate in two dimensions, which is also adopted by other authors [21].…”

Section: Entropy Principlementioning

confidence: 99%

“…Works by [21,22] demonstrate that exponential disks can be achieved by maximizing entropy subject to mass and angular momentum constraints. Additionally, based on the saddle point entropy concept introduced by [23], we have derived an equilibrium density profile of a spherical self-gravitating system with finite mass for the first time [24], and we believe it can also provide unique insights on the disk-shaped self-gravitating system [25]. However, these studies have not concurrently considered the exponential disk and the black hole.…”

Section: Introductionmentioning

confidence: 99%

“…[26] considers the maximized entropy with the central body for the spherical system. In this work, based on our previous work [25], we will study the effects of the central black hole on the stellar disk. This paper is structured as follows: Section 2 provides a review of our earlier work to establish the foundational concepts.…”

Section: Introductionmentioning

confidence: 99%

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Revisiting the Surface Brightness Profile of the Stellar Disk with the Statistical Mechanics of the Self-Gravitating System with the Central Body

Kang

2024

Entropy

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We have explored the exponential surface brightness profile (SBP) of stellar disks, a topic extensively discussed by many authors yet seldom integrated with the study of correlations between black holes, bulges, and entire disks. Building upon our prior work in the statistical mechanics of disk-shaped systems and aligning with methodologies from other research, we analyze the influence of the central body. This analysis reveals analytical relationships among black holes, bulges, and the entire stellar disk. Additionally, we incorporate a specific angular momentum distribution (SAMD) that aligns more closely with observational data, showing that for the self-gravitating disk, with the same surface density, a reduction in its spin results in only a slight decrease in its radius, whereas with the same SAMD, an increment in its spin significantly limits its extent. A key feature of our model is its prediction that the surface density profile of an isolated disk will invariably exhibit downbending at a sufficient distance, a hypothesis that future observations can test. Our refined equations provide a notably improved fit for SBPs, particularly in the central regions of stellar disks. While our findings underscore the significance of statistical mechanics in comprehending spiral galaxy structures, they also highlight areas in our approach that warrant further discussion and exploration.

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Section: Effect Of the Central Bodymentioning

confidence: 89%

Section: Effect Of the Central Bodymentioning

confidence: 91%