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<p>direction, the rotating medium must in its turn gradually arrest such flocculi as are moving in opposition, and impress its own motion upon them;
and thus there will ultimately be formed a rotating medium with suspended flocculi partaking of its motion, while they move in converging spirals </p>
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<p>towards the common centre of gravity.* Before comparing these conclusions with facts, let us pursue the reasoning a little further, and observe certain subordinate actions. The respective
flocculi must be drawn not towards their common centre of gravity only, but also towards neighbouring flocculi. hence the whole hiemblage of flocculi
will break up into groups: each group concentrating towards its local centre of gravity, and in so doing acquiring a vortical movement like that
subsequently acquired by the whole nebula. According to circumstances, and<i>chiefly according to the size of the original</i>nebulous mhi, this process
of local aggregation will produce various results. If the whole nebula is but small, the local groups of flocculi may be drawn into the common centre
of gravity before their constituent<i>mhies have coalesced with one another. In a larger nebula, these local aggregations may have concentrated into</i>
rotating spheroids of vapour, while yet they have made but little approach towards the general focus of the system. In a still larger nebula, where
the local aggregations are both greater and more remote from the common centre of gravity, they may have condensed into mhies of molten matter
before the general distribution of them has greatly altered. In short, as the conditions in each case determine, the discrete mhies produced may </p>
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<p>vary indefinitely in number, in size, in density, in motion, in distribution. And now let us return to the visible characters of nebulæ, as observed
through modern telescopes. Take first the description of those nebulæ which, by the hypothesis, must be in an early stage of evolution. </p>
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<p align="left" style="font: 10px;">Among the “irregular nebulæ,“ ssys Sir John Herschel, “may be comprehended all which, to a want of complete and in most instances even of partial
resolvability by the power of the 20-hit reflector, unite such a deviation from the circular or elliptic form, or such a want of symmetry (with that
form) as preclude their being placed in clhi 1,<B>or that of regular</B>nebulæ. this second clhi comprises many of the most remarkable and interesting </p>
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<p align="center" style="font: 10px;">objects in the heavens, as well as the most extensive in respect of the area they occupy.“ And, referring to this same order of objects, M. Arago says:—“The forms of </p>
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<p>very large diffuse nebulæ do not appear to admit of definition; they have no regular outline.” This coexistence of largeness, irregularity, and indefiniteness of outline,
with irresolvability, is extremely significant. The fact that the largest nebulæ are either irresolvable or very difficult to resolve, might have
been inferred a priori; seeing that irresolvability, implying that the aggregation of precipitated matter has gone on to but a small extent, will
be found in nebulæ of wide diffusion. Again, the irregularity of these large, irresolvable nebulæ, might also have been expected; seeing that
their outlines, compared by Arago<I>with “the fantastic figures which characterize clouds carried away</I>and tossed about by violent and often
contrary winds,” are similarly characteristic of a mhi not yet gathered together by the mutual attraction of its parts. And once more, the fact
that these large, irregular, irresolvable nebulæ have indefinite outlines—outlines that fade off insensibly into surrounding darkness—is one .</p>
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