File:Transactions of the Royal Society of New Zealand (1880) (14795165683).jpg

Identifier: transactionsofro80roya (find matches)
Title: Transactions of the Royal Society of New Zealand
Year: 1880 (1880s)
Authors: Royal Society of New Zealand
Subjects: Science
Publisher: Wellington, N.Z. : The Society
Contributing Library: Brigham Young University Hawaii, Joseph F. Smith Library
Digitizing Sponsor: Consortium of Church Libraries and Archives

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y the dotted ellipse fig. 6. After the first return, were the nebulauniform, it would tend to make a larger ellipse, that is increase its averagedistance from the centre, thus the potential energy of the planet would beincreased, and this increase is done at the expense of the planets rotation.It might be supposed that this would be a very small matter, but it must beremembered that all the time the body is contracting from a more or lessdense gaseous to a liquid state the whole of this potential energy will beconverted into rotation, thus the total effect may be very considerable, butas this action will be chiefly at perihelion it will tend materially to alter theeccentricity. It must be clearly understood that it is the differentialresistance on the sides of the planet towards and away from the sun that isdiscussed in this paragraph ; its general retarding action was studied in thelast problem. * Trans. N.Z. Inst., Vol. XII., Art. XIV. TRANS.NZJNSTITUTE,VOLini.PlIFy.Z. STRAIGHT LINE
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To illustrate JPtyoer hy Professor Bickerton. Bickerton.—Causes tending to alter Eccentricity of Planetary Orbits, 153 On the Accretion of Particles. When the nebula has become stable, that is no longer expanding, muchof its elementary matter will be at a sufficiently low temperature to com-bine ; and these compound molecules will tend to aggregate into groups,and it may be shown that these masses may ultimately become so consider-able as to form star clusters, associated by gravitation but not coalescing. Ipropose discussing this difficult question in a paper on star clusters ; but inthis paper I shall simply state that these little bodies will in all probabilityrevolve in independent orbits at all eccentricities around the centre of themass ; these and other masses will be occasionally picked up by the planet.The following problem shows that component to and from the centretends to be destroyed, and only a circular orbit left. Problem 4.—Given two bodies revolving in eccentric o

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