Stellar Evolution and Its Relations to Geological TimeCroll, James
Science
Stellar Evolution and Its Relations to Geological Time
Croll, James
Cosmogony; Geological time; Stars -- Evolution
The impact theory seems to remove all these difficulties. It is just as
likely _à priori_, if not more so, that the primitive form of the
protyle should have been that of large cold masses moving through space
in all directions, with excessive velocities, as that it should have
been that of a gaseous mass in a state of unstable equilibrium. If we
assume the former condition, then the colliding of these masses would
account not only for the ultra-gaseous state, but also for its
inconceivably high temperature. Besides, in this case we are not called
upon to account for any other antecedent state of the masses before
collision, for they may have existed from the beginning of creation in
the form of masses in motion through space.
Had space and time permitted, it might have been shown that there are
other obscure points on which the theory seems to shed additional light.
I shall now, in conclusion, refer to a point wherein the theory differs
radically from that of all other theories of stellar evolution. But
before doing so I may briefly refer to an objection which has been
frequently urged against the theory.
_Objection considered._—The objection to which I refer is this, that,
had the nebulæ been produced by impact in the way implied in the theory,
then we ought to have had some historical record of such an event. I can
perceive no force in such an objection. Our historical records, I
presume, do not extend much farther back than about 3,000 years, and we
have no evidence to conclude that a new nebula makes its appearance in
the visible firmament with such frequency; and supposing it did, we have
no grounds for assuming that its production by impact in the way
supposed by the theory would attract general notice. It is doubtful if
the nebula produced would, in the first instance, be actually visible. I
have shown that the temperature of the nebula could not have been less
than about 300,000,000° C., and it is very doubtful if the gaseous mass
enveloping all that was solid in the nebula would, at such a
temperature, be self-luminous. The probability is that all the chemical
elements composing it would be in a state of utter dissociation, and
converted back into the original protyle from which they were derived,
again to be slowly reconverted into their former atomic condition as the
temperature fell.
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