Gravitational transformation of gaseous clouds: The formation of spiral galaxies and disk planets

Andrei Pavlov

Orvokkikatu 8, Naantali, Finland.

DOI: 10.4236/ns.2014.64020                

Abstract

Gravitation is one of the central forces playing an important role in formation of natural systems like galaxies and planets. Gravitational forces between particles of a gaseous cloud transform the cloud into spherical shells and disks of higher density during gravitational contraction. The density can reach that of a solid body. The theoretical model was tested to model the formation of a spiral galaxy and Saturn. The formations of a spiral galaxy and Saturn and its disk are simulated using a novel N-body self-gravitational model. It is demonstrated that the formation of the spirals of the galaxy and disk of the planet is the result of gravitational contraction of a slowly rotated particle cloud that has a shape of slightly deformed sphere for Saturn and ellipsoid for the spiral galaxy. For Saturn, the sphere was flattened by a coefficient of 0.8 along the axis of rotation. During the gravitational contraction, the major part of the cloud transformed into a planet and a minor part transformed into a disk. The thin structured disk is a result of the electromagnetic interaction in which the magnetic forces acting on charged particles of the cloud originate from the core of the planet.

Keywords

Gravitation; Planets; Saturn’s Rings; Computer Simulation; Planet’s Interior Structure; Formation of Galaxies; Spiral Galaxies; N-Body Simulations

Conflicts of Interest

The authors declare no conflicts of interest.

References

[1]	Newton I. (1687) Philosophiae naturalis principia mathematica (Mathematical principles of natural philosophy).
[2]	Kepler J. (1619) De harmonice monde (The harmony of the world).
[3]	Cuzzi, J.N., Lissauer, J.J., Esposito, L.W., Holberg, J.B., Marouf, E.A., Tyler, G.L. and Bouschot, A. (1984) Saturn’s rings: Properties and processes. In: Greenberg, R. and Brahic, A., Eds., Planetary Rings, University of Arizona Press, Tucson, 73-199.
[4]	Jeans Sir, J. (1902) The stability of spherical nebulae. Philosophical Transactions of the Royal Society of London, Series A, 199, 1. http://dx.doi.org/10.1098/rsta.1902.0012
[5]	Brahic, A. and Sicardy, B. (1981) Apparent thickness of Saturn’s rings. Nature, 289, 447-450. http://dx.doi.org/10.1038/289447a0
[6]	Sicardy, B., Lecacheux, J., Laques, P., Despiau, R. and Auge, A. (1982) Apparent thickness and scattering properties of Saturn’s rings from March 1980 observations. Astronomy & Astrophysics, 108, 296-305.
[7]	Lane, A.L., Hord, C.W., West, R.A., Esposito, L.W., Coffeen, D.L., Sato, M., Simmons, K.E., Pomphrey, R.B. and Morris, R.B. (1982) Photopolarimetry from Voyager 2: Preliminary results on Saturn, Titan, and the rings. Science, 215, 537-543. http://dx.doi.org/10.1126/science.215.4532.537
[8]	Rosen, P.A. and Lissauer, J. (1988) The Titan －1:0 nodal bending wave in Saturn’s ring C. Science, 241, 690-694. http://dx.doi.org/10.1126/science.241.4866.690
[9]	Chakrabarti, S.K. (1989) The dynamics of particles in the bending waves of planetary rings. MNRAS, 238, 13811394.
[10]	Rosen, P.A., Tyler, G. A. and Marouf, E.A. (1991) Resonance structures in Saturn’s rings probed by radio occultation: I. Methods and examples. Icarus, 93, 3-24. http://dx.doi.org/10.1016/0019-1035(91)90160-U
[11]	Sears, F.W. and Salihger, G.L. (1975) Thermodynamics, kinetic theory, and statistical thermodynamics. AddisinWesley Publishing Company, London.
[12]	Cuzzi, J.N., Lissauer, J.J., Esposito, L.W., Holberg, J.B., Marouf, E.A., Tyler, G.L. and Bouschot, A. (1984) The rings of Saturn. Planetary Rings, University of Arizona Press, Tucson, 73-199.
[13]	Esposito, L.W., Cuzzi, J.N., Holberg, J.B., Marouf, E.A., Tyler, G.L. and Porco, C.C. (1984) Saturn’s rings: Structure, dynamics, and particle properties. Saturn, University of Arizona Press, Tucson, 463-545.
[14]	Nicholson, P.D., Showalter, M.R., Dones, L., French, R.G., Larson, S.M., Lissauer, J.J., McGhee, C.A., Seitzer, P., Sicardy, B. and Danielson, G.E. (1996) Observations of Saturn’s ring-plane crossings in August and November 1995. Science, 272, 509-515. http://dx.doi.org/10.1126/science.272.5261.509
[15]	Benacchio, L. and Galletta, G. (1980) Triaxiality in elliptical galaxies. MNRAS, 193, 885-894.
[16]	Fasano, G. and Vio, R. (1991) Apparent and true flattening distribution of elliptical galaxies. MNRAS, 249, 629633.
[17]	Franx, M. and se Zeeuw, P.T. (1992) Elongated disks and the scatter in the Tully-Fisher relation. The Astrophysical Journal, 392, L47-L50. http://dx.doi.org/10.1086/186422
[18]	Lambas, D.G., Maddox, S. and Loveday, J. (1992) On the true shapes of galaxies. MNRAS, 258, 404-414.
[19]	Ryden, B.S. (1996) The intrinsic shapes of stellar systems. The Astrophysical Journal, 461, 146-154. http://dx.doi.org/10.1086/177043