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phenomena such as spiral galaxy, hurricane, and drain in the sink (Figures 14, and 15). By neglecting the thickness of the spiral flow, Eq.(2) of the Navier-Stokes Equations in cylindrical coordinates can be expressed in the form: u _{r} (u_{r}/r) + u_{} (u_{r}/) = F_{r} ---------- (15a)u _{r} [(r u_{})/r] + u_{} [(r u_{})/] = 0 ---------- (15b)where u _{} = /t. If we assumed further that the force acts on the fluid only in the radial direction. In addition by assuming constant density for the fluid, | ||

## Figure 14 Barred Spiral Galaxy |
## Figure 15 Hurricane |
Eq.(1) of the continuity equation becomes: (1/r) [(r u _{r})/r] +
(1/r) [(r u_{})/] = 0 ---------- (16) |

A relationship between the velocity components is obtained by substituting Eq.(16) to Eq.(15b): u _{r} = b u_{} ---------- (17)where b is a constant having the dimension of length. This formula can be integrated once more to yield: r = a + b ---------- (18) | |

## Figure 16 Archimedean Spiral |
where a is another constants of integration. Eq.(18) expresses the trajectory of an Archimedean spiral (see curve on the left of Figure 16). So far there is no restriction on whether the movement is to plunge inward or to expand. |

- The appearance of the spiral is determined by the constants of integration:
- The value of b determines the winding of the spiral. As b = dr/d is the relative rate of change between r and , a small value of b makes the winding very tight and vice versa.
- The solution also admits another spiral arm with - or 180
^{o}out of phase (see curves on the right of Figure 16). - With variation of orientation at r 0, the spiral assumes a broad sweeping pattern much like the hurricane in Figure 15 instead of one slim locus.
- The sign of b, i.e., b > 0 or b < 0, has the effect on the winding direction - whether it turns to the left or right.
- For the barred spiral like the Milkyway in Figure 14, the constant a > 0, while a = 0 is for the case of true spiral galaxy such as NGC2997. It turns out that the formation of spiral arms in galaxy is more complicated than this simple minded approach, which would produce tightly wound spirals (within 500 million years) in contrary to observation (see more in Theory of Spiral Arm Formation).

u

On the disk of the spiral galaxy F

with M to be the mass of the central black hole, while the mass on the disk within r is given by M' = 2 _{} r dr, where = _{0} (r_{0}/r) is the surface density in unit of gm/cm^{2}, _{0} is its cutoff value at the edge of the galaxy r = r_{0}, and the third term is the centrifugal force. Thus, the radial and rotational components of the velocity can be expressed as:u _{r}^{2} = GM / r + 2G_{0}r_{0} - r^{2}u_{}^{2} ---------- (19b),r ^{2}u_{}^{2} = r (GM + 2G _{0}r_{0} r) / (b^{2} + r^{2}) ---------- (19c),
| |

## Figure 17a Rotation Curve for Milky Way [view large image] |
which has the same profile of the rotation curve for the disk as shown in Figure 17a with a peak at r_{m} (4_{0}r_{0}b/M) b for 4_{0}r_{0}b >> M. The observed curve takes into account of the dark matter in the halo. |

2r

M 3x10

r

r

the followings can be derived:

b 0.015 kpc, which implies tightly wound arms, and

(4

The calculated rotation and radial velocities at r

At the event horizon of the central black hole r

To check the winding of the Milkyway spiral arms, it is noticed that the rotation velocity is in the order of 100 km/sec for a wide range of distance outside the core. Following this simplification, the spiral arms wind through a cycle of 360

The derivation is a little bit more involved for the hurricane. The attractive force F

dp/dr (which has overwhelmed the Coriolis and centrifugal forces in this case): u _{r}^{2} / r = (1/_{}) dp/dr ---------- (20). The dependence of p on r is shown in Figure 17b. The observational data (for the "Charlie" type hurricane) can be approximated by the empirical formula: p = p _{0} [5.5 - e^{-k(r - re)}] ---------- (21) for r _{} r_{e}, where r _{e} is the distance from the center to the wall of the eye (Figure 17b), p_{0} = 220 mb and k is a constant related to the steepness of the pressure gradient. Thus, the pressure gradient is:dp/dr = kp _{0}e^{-k(r - re)} ---------- (22) for r _{} r_{e}or u _{r}^{2} = (krp_{0}/_{}) e^{-k(r - re)} ---------- (23) for r _{} r_{e}.At the wall of the eye, r = r _{e}, and u_{r}^{2} = kr_{e}p_{0}/_{}.
| |

## Figure 17b Pressure Gradient of Hurricane |
The rotation curve is given by r^{2}u_{}^{2} = (kr^{3}p_{0}/b^{2}_{}) e^{-k(r - re)}, which reproduces a profile similar to the curve in Figure 17b with a maximum at r_{m} = 3/k. This kind of analysis is also applicable to the drain in the sink although on a much smaller scale. |

r

r

and u

The followings can be derived from these data:

k = 3/r

b = [u

Thus the radial distance changes by about 125 km covering about 2/3 of the average hurricane size when turns one cycle. There is no tightly wound arms. This model seems to represent the actual system quite well. Meanwhile, the calculated radial and circular velocities at the wall of the eye are u_{r} 4.6 m/h and r_{e}u_{} 2.3 m/h respectively indicating a calm region there.Figure 17c is a vivid example from a small scale hurricane (a thunderstorm supercell) over Montana, USA showing the wall, as well as the dark cloud spiralling inward. | |

## Figure 17c Thunderstorm Supercell [view large image] |

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