Certain Aspects of the Gravitational Field of a Disk ()

Jonathan D. Weiss^{}

JSA Photonics, LLC, Albuquerque, NM, USA.

**DOI: **10.4236/am.2018.912089
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JSA Photonics, LLC, Albuquerque, NM, USA.

There are at least two reasons why one would study the gravitational field of a
disk. The first is that many astronomical objects, such as spiral galaxies like
the Milky Way, are disk-like. The second is that the field of a disk is interesting,
particularly when compared to that of a spherical, or near-spherical, object,
which is much easier to analyze because of its high degree of symmetry.
It is hoped that this study will augment previous work on this subject. The
aspects presented in this paper are as follows: 1) both the radial and vertical
gravitational fields of a thin disk within the plane of the disk and above it; 2) a
comparison of some of the field results obtained by Lass and Blitzer (1983)
involving elliptic integrals to those obtained by a standard numerical integration,
now available online, and separately through the use of Legendre polynomials;
3) the logarithmic divergence of the radial field at the edge of a thin
disk; 4) the fields in the plane of a disk containing a central hole, particularly
within the hole, such as the rings of Saturn; 5) circular orbits within the plane
of a single disk and half way between two disks, and their stability; 6) the escape
velocity at a point within the Milky Way, particularly at the position of
the solar system and without any added, or subtracted, orbital effects around
the galactic center; and 7) the radial field at the circular edge of a disk of finite
thickness.

Keywords

Disk-Shaped Mass, Gravitational Effects of a Disk-Shaped Mass, Calculational Techniques of Such Gravitational Effects

Share and Cite:

Weiss, J. (2018) Certain Aspects of the Gravitational Field of a Disk. *Applied Mathematics*, **9**, 1360-1377. doi: 10.4236/am.2018.912089.

1. Introduction

Although many astronomical objects, such as stars, planets, and certain galaxies, are spherical, or nearly spherical, in shape, many others are disk-like. Examples of the latter are bar spiral galaxies (such as the Milky Way), the rings of Saturn, viewed as disks with a large central hole, and protoplanetary disks, consisting of dense gas and dust surrounding a newly formed star that add mass to the star [1]. Thus, the gravitational fields of such structures have been studied, and we hope that the work presented here on various aspects of the gravitational fields of uniform disks, albeit a geometric simplification, will augment previous work and be of general interest as a problem in physics.

Certain Previous Work (Lass and Blitzer)

Two examples of previous work on the gravitational field of an infinitely thin disk are by Lass and Blitzer [2] and Krough, Ng, & Snyder [3], both published in the early 1980s. Neither presented specific graphic examples of their mathematical results, which would have made them more concrete for the reader. We will do so here, but only for the paper by Lass and Blitzer. Other augmentations of the paper by Lass and Blitzer will also presented.

With reference to Figure 1, the following is their expression for the gravitational potential, *V*(*r*, *z*), for *r* < *a*.

$\begin{array}{c}V\left(r,z\right)=2\sigma G[\text{\pi}\left|z\right|-\sqrt{{z}^{2}+{\left(a+r\right)}^{2}}E\left(k\right)\\ \text{\hspace{0.17em}}\text{\hspace{0.17em}}-\left[\left({a}^{2}-{r}^{2}\right)/\sqrt{{z}^{2}+{\left(a+r\right)}^{2}}\right]K\left(k\right)\\ \text{\hspace{0.17em}}\text{\hspace{0.17em}}-\left[\left(\left(a-r\right)/\left(a+r\right)\right){z}^{2}/\sqrt{{z}^{2}+{\left(a+r\right)}^{2}}\right]\Pi \left(n,k\right)].\end{array}$ (1)

For *r* > *a*, the first term,
$\text{\pi}\left|z\right|$, is eliminated because there is no surface mass beyond *r* = *a*. Thus, the z-component of the field at *z* = 0 is zero there, while it is not zero for *z* < *a*, where there is surface mass. Regarding the meaning of the symbols not noted in Figure 1, *σ* is the mass per unit area of the disk; *G* is Newton’s gravitational constant, and *K*(*k*),*E*(*k*), and Π(*n*, *k*) are the complete elliptic integrals of the first, second, and third kind, respectively. The parameters k and *n* are defined such that
${k}^{2}=4ar/\left[{z}^{2}+{\left(a+r\right)}^{2}\right]$ and
$n=4ar/{\left(a+r\right)}^{2}$. We note that at *z* = 0, *k*^{2} = *n*. As to the complete elliptic integrals, they have the following integral representations, as stated in [4],

Figure 1. Basic geometry; uniform circular gravitational disk of radius a. *P*(*x _{o}*,

$\begin{array}{l}K\left(k\right)={\displaystyle {\int}_{0}^{1}\frac{\text{d}t}{\sqrt{\left(1-{t}^{2}\right)\left(1-{k}^{2}{t}^{2}\right)}}};\\ E\left(k\right)={\displaystyle {\int}_{0}^{1}\frac{\text{d}t\sqrt{1-{k}^{2}t}}{\sqrt{1-{t}^{2}}}};\\ \Pi \left(n,k\right)={\displaystyle {\int}_{0}^{1}\frac{\text{d}t}{\left(1-n{t}^{2}\right)\sqrt{\left(1-{t}^{2}\right)\left(1-{k}^{2}{t}^{2}\right)}}};\end{array}$ (2)

Although it is of no consequence, we should be aware of a slight difference in notation between [2] and [4] What [4] refers to as *n *is called *n*^{2} in [2]. Since [4] is a more modern publication, we shall adhere to its convention and define 4*ar*/(*a* + *r*)^{2} as *n*.

To obtain the force in the radial direction, *F _{r}*, we calculate –∂

$\begin{array}{l}{F}_{r}\left(z=0\right)/2G\sigma \\ =-\left[\frac{1+{r}_{a}^{2}}{{r}_{a}\left(1+{r}_{a}\right)}\right]K\left(k\right)+\left[\frac{\left(1+{r}_{a}\right)\left(2+{r}_{a}\right)}{2{r}_{a}}\right]E\left(k\right)-\left[\frac{{\left(1-{r}_{a}\right)}^{2}}{2\left(1+{r}_{a}\right)}\right]\Pi \left(n,k\right)\end{array}$ (3)

In this equation, *r _{a}* ≡

The scaled radial field in the plane of the disk is plotted in Figure 2, for 0 ≤ *r _{a}* ≤ 1. The elliptic integrals were evaluated numerically with the help of “Keisan Online Calculator” [5]. The field is negative because it is directed in the negative r-direction. For comparison, the scaled radial field for a solid sphere of radius “

Figure 2. Radial gravitational field derived from [2]. Downward arrow indicates logarithmic divergence to negative infinity exactly at *r _{a}* = 1, caused by the complete elliptic integral of the first kind at

Figure 3. Gravitational field of a solid sphere.

Figure 4. Linear-Ln plot of *K*(*k*) from 0.8 ≤ *r _{a}* ≤ 1.2. The shape of the curve indicates that

In addition, a view of the complete elliptic integral of the third kind in [5], when both arguments are near unity, suggests a divergence of Π(*n*, *k*) in that region. Indeed, it does diverge, but with what behavior? The graph in Figure 5,

Figure 5. n-Ln plot of Π(*n*, *k*) vs (1 − *r _{a}*)

obtained in the same way as that for *K*(*k*), demonstrates that Π(*n*, *k*) diverges as 1/(1 − *r _{a}*)

Certain Current Work

In this section, we examine two other methods of calculating the same radial field as above. These are the use of “standard” numerical integration and Legendre Polynomials.

2. Numerical Integration

Figure 6 is relevant to the use of numerical integration.

The gravitational field, *V*(*r _{o}*), will be first calculated and then

$\begin{array}{c}V\left({r}_{o}\right)=-2G\sigma [{\displaystyle {\int}_{0}^{a}\text{d}y}{\displaystyle {\int}_{0}^{\sqrt{{a}^{2}-{y}^{2}}}\frac{\text{d}x}{\sqrt{{\left({r}_{o}-y\right)}^{2}+{x}^{2}}}}\\ \text{\hspace{0.17em}}\text{\hspace{0.17em}}+{\displaystyle {\int}_{0}^{a}\text{d}y}{\displaystyle {\int}_{0}^{\sqrt{{a}^{2}-{y}^{2}}}\frac{\text{d}x}{\sqrt{{\left({r}_{o}+y\right)}^{2}+{x}^{2}}}}]\end{array}$ (4)

The first term represents the contribution from the right half of the disk in Figure 6, while the second represents the contribution from the left half of the disk. After calculating −∂*V*/∂*r* and performing a variety of tedious algebraic manipulations, we obtain, using the relative coordinates *r _{a}* and

$\begin{array}{l}F\left({r}_{a}<1\right)=2G\sigma [{\displaystyle {\int}_{0}^{1}\frac{\text{d}{y}_{a}\left({r}_{a}-{y}_{a}\right)}{\left(\sqrt{1-{y}_{a}^{2}}+\sqrt{1+{r}_{a}^{2}-2{y}_{a}{r}_{a}}\right)\sqrt{1+{r}_{a}^{2}-2{y}_{a}{r}_{a}}}}\\ +{\displaystyle {\int}_{0}^{1}\frac{\text{d}{y}_{a}\left({r}_{a}+{y}_{a}\right)}{\left(\sqrt{1-{y}_{a}^{2}}+\sqrt{1+{r}_{a}^{2}+2{y}_{a}{r}_{a}}\right)\sqrt{1+{r}_{a}^{2}+2{y}_{a}{r}_{a}}}}+\text{ln}\left(\left(1-{r}_{a}\right)/\left(1+{r}_{a}\right)\right)]\end{array}$ (5)

Figure 6. The geometry needed for the use of numerical integration, as a method of calculating the radial force in the plane of the disk. In this case, the field point coordinate is within the disk (*y _{o}* <

For *r _{a}* > 1, the expression for the force is the same, except that (1 −

3. Legendre Polynomials

Figure 8 shows the azimuthally symmetric disk geometry needed for the use of Legendre polynomials of varying degree *l*, *P _{l}*(cos

$V\left(r,\theta \right)={\displaystyle {\sum}_{0}^{\infty}{A}_{l}{r}^{l}{P}_{l}\left(\mathrm{cos}\theta \right)}\text{\hspace{0.05em}}\text{\hspace{0.05em}};\text{\hspace{0.17em}}\text{\hspace{0.17em}}r<a$ (6a)

$V\left(r,\theta \right)={\displaystyle {\sum}_{0}^{\infty}{B}_{l}{r}^{-\left(l+1\right)}{P}_{l}\left(\mathrm{cos}\theta \right)}\text{\hspace{0.05em}}\text{\hspace{0.05em}};\text{\hspace{0.17em}}\text{\hspace{0.17em}}r>a$ (6b)

In the case of other azimuthally symmetric geometries, such as the annular region between a disk and a ring, the potential could be expressed as the sum of these two equations. These expressions are standard for solutions of Laplace’s Equation with azimuthal symmetry and can be found in any textbook on the subject.

Figure 7. Geometry for the application of the Legendre polynomials to the disk problem, where “*a*” and “*r*” are simply lengths and *θ* is the angle with respect to the normal to the disk.

Figure 8. Gravitational field vs. distance from center, using the three different calculational methods identified in the legend. All three agree very well, except very near *r _{a}* = 1, where the logarithmic divergence occurs and the use of Legendre polynomials falls short.

Since *P _{l}*(1) = 1 for all l, we first determine

$V\left(r,0\right)=-\left(2G\sigma \right)\text{\pi}\left[\sqrt{{r}^{2}+{a}^{2}}-r\right]$ (7)

For *r *< *a*, one factors out the a-term under the square root, which allows for the expansion of the potential in powers of (*r*/*a*). Factoring out the r-term allows for the expansion in powers of (*a*/*r*). After performing the expansions out to a respectable six terms (the chosen number), making use of the expressions for *P*_{2n}(0), and calculating the derivative −∂*V*/∂*r*, we obtain the following for *F _{r}*:(using the relative coordinate

$\begin{array}{l}{F}_{r}=-\left(2G\sigma \right)\text{\pi}[0.5{r}_{a}+0.1875{r}_{a}^{3}+\left(0.1171\cdots \right){r}_{a}^{5}+\left(0.0854\cdots \right){r}_{a}^{7}\\ \text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.05em}}\text{\hspace{0.05em}}+\left(0.06729\cdots \right){r}_{a}^{9}+\left(0.0555\cdots \right){r}_{a}^{11}];\text{\hspace{0.17em}}\text{\hspace{0.17em}}{r}_{a}<1\end{array}$ (8a)

$\begin{array}{l}{F}_{r}=-\left(2G\sigma \right)\text{\pi}[\frac{0.5}{{r}_{a}^{2}}+\frac{0.1875}{{r}_{a}^{4}}+\frac{\left(0.1171\cdots \right)}{{r}_{a}^{6}}+\frac{\left(0.0854\cdots \right)}{{r}_{a}^{8}}\\ \text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}+\frac{\left(0.06729\cdots \right)}{{r}_{a}^{10}}+\frac{\left(0.0593\cdots \right)}{{r}_{a}^{12}}];\text{\hspace{0.17em}}\text{\hspace{0.17em}}{r}_{a}>1\end{array}$ (8b)

Although it is difficult to resolve details, Figure 8 shows how well the use of Legendre polynomials agrees with the other two methods, except near*r _{a}* = 1. An expanded view of this region is shown in Figure 9, where we can see the disagreement developing between 0.8 <

4. Z-Dependence of the Radial Field and the Field in the Z-Direction

So far, we have only looked at the radial field in the plane of the disk, but what about the radial field at different values of *z _{a}* and the vertical field at different values of

$\begin{array}{c}V\left({r}_{o},{z}_{o}\right)=-2G\sigma [{\displaystyle {\int}_{0}^{a}\text{d}y}{\displaystyle {\int}_{0}^{\sqrt{{a}^{2}-{y}^{2}}}\frac{\text{d}x}{\sqrt{{\left({r}_{o}-y\right)}^{2}+{z}_{o}^{2}+{x}^{2}}}}\\ \text{\hspace{0.17em}}\text{\hspace{0.17em}}+{\displaystyle {\int}_{0}^{a}\text{d}y}{\displaystyle {\int}_{0}^{\sqrt{{a}^{2}-{y}^{2}}}\frac{\text{d}x}{\sqrt{{\left({r}_{o}+y\right)}^{2}+{z}_{o}^{2}+{x}^{2}}}}]\end{array}$ (9)

Figure 9. An expanded version of Figure 8, demonstrating more clearly where the use of Legendre polynomials deviates from Lass and Blitzer and numerical integration.

Figure 10 shows the first of these results for *z _{a}* = 0, 0.2, and 0.4. The basic shapes are the same for all three curves, but there is no logarithmic divergence for values of

Figure 11 shows the field in the z-direction, *F _{z}* (=−∂

Figure 10. Radial gravitational field at three values of *z _{a}*, using “standard” numerical integration.

Figure 11. Gravitational field in z-direction for solid disk for various values of *r _{a}* out to 4. Three are for

result follows from the Gaussian formulation of the law of gravitation, Ñ*F *= −4π*Gρ*, where *F* is the gravitational field and *ρ* is the mass density at each point. Using a Gaussian pillbox, as in electrostatics, that straddles the surface mass density of the disk, along with the integral form of Gauss’ law, leads to the result. All mass points on the disk, other than the one in question, only contribute to the field parallel to the surface of the disk at *z* = 0.

We note that *F _{z}* = 0 for all

This is definitely not true for the radial field, as we now discuss in the case of a solid disk containing a hole of half of its area and centered within it. The radial field can readily be obtained from linear superposition by subtracting the field of a smaller disk, identical in size and position of the hole, from that of the solid disk. Figure 13 shows the fields of the two disks, while Figure 14 shows the result of the subtraction. The counter-intuitive result is that radial field within the hole is in the positive radial direction and increases to the edge of the hole, where the logarithmic divergence occurs. It continues in that direction, with reduced magnitude, into bulk of the remaining mass of the original disk, until *r _{a}* ≈ 0.81. At that point, the field becomes negative and stays that way for all

By comparison, Figure 15 shows the gravitational field, *F _{s}*, of a sphere of mass density

Figure 12. *F _{z}* (gravitational field in

Figure 13. The radial field from the two disks. The smaller disk is the size of the hole that will be created by subtraction.

Figure 14. Gravitational field in the hole, in the remaining mass of the disk, and somewhat beyond the mass of the disk.

Figure 15. Gravitational field of a sphere with a central hole that removes half the mass of the solid sphere. The diagonal dotted line shows the slight deviation from linearity for *r** _{a}* < 1.

${F}_{s}=\left(\frac{4\text{\pi}}{3}\right)Ga\rho \left[{r}_{a}-\frac{1}{2{r}_{a}^{2}}\right];\text{\hspace{0.17em}}\text{\hspace{0.17em}}{0.5}^{1/3}\le {r}_{a}\le 1$ (10a)

${F}_{s}=\left(\frac{\text{2\pi}}{3}\right)\frac{\left[Ga\rho \right]}{{r}_{a}^{2}};\text{\hspace{0.17em}}\text{\hspace{0.17em}}{r}_{a}\ge 1$ (10b)

*F _{s}* = 0 within the hole, where 0 ≤

5. Disk of Non-Zero Thickness

Until now, we have concentrated on a disk of zero thickness. In this section, we consider the radial gravitational field of a uniform disk of non-zero thickness *T* equal to a maximum of one tenth of its fixed radius “*a*”. Two different situations are considered, as shown in Figure 16. In situation A, the field point X is fixed at the lowest corner, while the relative thickness of the disk can change from 0 to *T _{a}* = 0.1. The field at X is determined as a function of the relative thickness,

These contributions are determined by breaking up the disk into thin slices and considering each slice to be a disk of zero thickness, having a vertical separation from point X. The contribution from a given slice is calculated as in Equation (9) and taking its radial gradient at *r _{a}* = 1. The total contribution is obtained by integrating the individual contributions over the relative thickness,

Figure 18 shows the contribution to the field at X as a function of *z _{a}*. The function is obviously linear in ln(

Figure 16. Basic geometry for the gravitational field of a disk of maximum relative thickness *T _{a}*, radius

Figure 17. Vertical cross-section of the disk, showing relevant characteristics.

Figure 18. The contribution to the radial field at X from a slice at *z** _{a}*.

contribution must asymptotically approach zero for very thick disks. Calling the function *F*(*z _{a}*),

$F\left({z}_{a}\right)=-\mathrm{ln}\left({z}_{a}\right)+0.0869$ (11)

To obtain the total contribution at X for situation A, these contributions must be summed from 0 to *Z _{a}*. Thus, the total contribution over that thickness is:

${\int}_{0}^{{Z}_{a}}F\left({Z}_{a}\right)\text{d}{Z}_{a}}=-{Z}_{a}\mathrm{ln}\left({Z}_{a}\right)+1.0869{Z}_{a$ (12)

Aside from a scale factor, this equation is plotted in Figure 19 as A. Graph B is obtained by adding the contributions from the entire regions above and below X, as obtained from A. The symmetry about *z _{a}* = 0.05 is obvious, as are values at the end points, both of which receive contributions from the entire disk.

6. Properties of Circular Orbits in the Plane of a Disk

The properties of these circular orbits considered are the orbital period as a function of their radius measured from the center of the disk and the mass of the disk. The disk is assumed to be an approximate representation of the Milky Way with the same mass and diameter. The estimated diameter of the Milky Way is 10^{5} ly [9], among others, and the estimated mass is 1.4 × 10^{42} kg [10]. Since the mean thickness of the Milky Way is estimated to be only about (1 - 2) × 10^{3} ly [9], it will be ignored. In addition, the stability of such orbits with respect to radial perturbations and perturbations perpendicular to the plane of the disk are considered.

Figure 19. The radial gravitational field at point X for A and B.

Finding the period of the orbit is a simple problem in orbital mechanics. Assuming the radial field, *F*(*R*), beyond the disk is as in Figure 2, but including 2*Gσ*, then

$F\left(R\right)=\frac{{V}^{2}}{R},$ (13)

where *V *and *R* are the orbital speed and radius, respectively. The period *T* is

$T=\frac{2\text{\pi}R}{V}=2\text{\pi}\sqrt{R/F}$ (14)

Figure 20 shows the orbital period in billions of years plotted against the orbital radius in light years, up to 5 × 10^{5} ly. Galaxies that are less than this distance from the Milky Way are listed in [11], but no information allowing for a comparison to Figure 20, if any exists, has been found by this author. It is of some interest, however, to determine at what orbital radius the orbital period deviates negligibly from that of a point mass of the same mass as the disk. A simple calculation shows that the radius is about 75 × 10^{3} ly, or 1.5 galactic radii, which suggests a rapid march toward the asymptotic limit (but not as rapid as in the case of a sphere!). The result for a disk was arrived at by noting that the period of the orbit of radius*R* around a point mass is, coincidentally, proportional to *R*^{1.5}. Thus, if Figure 20 were displayed on a log-log plot, its behavior would become essentially linear starting at about 1.5 galactic radii. Figure 21 is such a plot showing the transition to linearity, with a slope of about 1.5, as indicated by the accompanying (eyeballed) dashed line.

Regarding orbital stability perpendicular to the plane of the disk, we can see in Figure 11 that the force in the positive *z*-direction for radii beyond the disk is negative. By anti-symmetry, the opposite is also true. Thus, the force out of the plane of the disk is always restorative and, therefore, maintains vertical stability

Figure 20. Orbital period of a satellite galaxy around the Milky Way, assuming a circular orbit in the plane of the Milky Way. Assumed radius and mass of Milky Way = 50,000 ly and 6 × 10^{42} kg, respectively.

Figure 21. Log-log version of Figure 20, showing the distance at which the disk effectively behaves as a point mass, as indicated by the dashed line.

(*i.e.*, a vertical oscillation about the plane of the disk). One could imagine a horizontal orbit half way between two identical disks, but such an orbit would be vertically unstable, since a perturbation toward either disk would only create a growing force imbalance toward that disk. This is particularly true for *r _{a}* < 1, where the magnitude of the negative force is monotonically decreasing with

Radial stability of a circular orbit is discussed in [12], which is a physics lecture. It occurs within the context of a coordinate system rotating with the orbiting particle, and thus includes the fictitious outward centrifugal force along with the real inward gravitational force. These two forces balance in the absence of a radial perturbation, thereby maintaining the orbital radius constant. In the presence of a perturbation, the author derives the condition for which an outward perturbation in the radius will induce a negative radial force, and vice versa, thereby causing an oscillation about the equilibrium radius. The condition for stability is:

$\frac{3}{\rho}+\frac{{g}^{\prime}\left(\rho \right)}{g\left(\rho \right)}>0$ (15)

where *ρ* is the radius of the unperturbed circle, *g*(*ρ*) is the negative of the gravitational force, and *g'*(*ρ*) is its derivative at *ρ*. Figure 22 is a plot of the above expression, called “stability condition”, for the field of a thin disk, as in Figure 7. Since extreme accuracy was not required for the current purpose of displaying the range of stability, the derivative was approximated by differences between successive calculated points. We see that radial stability occurs only for *r _{a}* ≳ 1.15. If the field behaved according to an inverse-square law, as outside a sphere, stability would occur for all values of

7. The Escape Velocity of the Earth from the Milky Way

In this section, we shall calculate the escape velocity from the disk-approximation of the Milky Way based solely on the gravitational attraction to an escaping object as a function of its location within the galaxy. The object’s orbital motion, or

Figure 22. Stability condition for a particle in orbit around a disk and in the plane of the disk.

other motion, within the galaxy, which influences the escape velocity, is not considered. As is well known, the escape velocity or, more properly, the escape speed, *v _{esc}*, is computed by equating the object’s initial kinetic energy to the negative of its initial potential energy. Thus,

${v}_{esc}=\sqrt{2V\left({r}_{a}\right)}$ (16)

where *V*(*r _{a}*) is the potential energy, as in Equation(4), using a relative coordinate. This expression gives the escape velocity as a function of position within the disk. Figure 23 is a graph of the computed escape velocity vs the radial position of the object. Since our solar system is ≈26,000 ly [9] from the center of the Milky Way,

8. Summary

In this paper, we have presented certain aspects of the gravitational characteristics of the disk geometry, including an ideally thin disk, a disk of finite thickness, and a thin disk in the form of a ring, though not thin walled. This geometry has been less studied than that of a sphere, which, because of its higher degree of symmetry, is simpler to analyze. Aside from its interest simply as a physics problem, certain astronomical objects, such as the Milky Way and protoplanetary disks, are disk-like in shape. In that regard, we have also presented calculations of the circular orbits in the plane of the Milky Way, approximated as a disk, concerning their orbital period and orbital stability. The escape velocity of an object, particularly at the position of the solar system, has been similarly calculated.

Figure 23. Escape velocity from Milky Way, assuming that the galactic radius = 50,000 ly, the galactic mass = 1.42 × 10^{42} kg, and the position of the solar system ≈ 0.5 galactic radii from the center. Reported escape velocity = 550 km/sec. The effect of the orbital velocity of the sun around the galactic center is not included.

Acknowledgements

The author thanks W. F. Filter, retired Sandia National Laboratories physicist, for reviewing the draft of this paper and making many valuable suggestions for its improvement.

Conflicts of Interest

The authors declare no conflicts of interest regarding the publication of this paper.

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