Worlds in the making: The evolution of the universeArrhenius, Svante
Science
Worlds in the making: The evolution of the universe
Arrhenius, Svante
Cosmogony
Lane has proved, what the above calculations also indicate, that the
temperature of such nebula will rise when it contracts in consequence
of its losing heat. If heat were introduced from outside, the nebula
would expand under cooling. A nebula of this kind presumably loses
heat and gradually raises its own temperature until it has changed
into a star, which will at first have an atmosphere of helium and of
hydrogen like that of the youngest stars (with white light). By-and-by,
under a further rise of temperature, the extremely energetic chemical
compounds will be formed which characterize the interior of the sun,
because helium and hydrogen—which were liberated when the nebula was
re-formed and which dashed out into space—will diffuse back into the
interior of the star, where they will be bound under the formation of
the compounds mentioned. The atmosphere of hydrogen and of helium will
disappear (helium first), the star will contract more and more, and the
pressure and the convection currents in the gases will become enormous.
There will be a strong formation of clouds in the atmosphere of the
star, which will gradually become endowed with the properties which
characterize our sun. The sun behaves very differently from the gaseous
nebulæ for which the calculations of Lane, Ritter, and Schuster hold.
For when the contraction of a gas shall have proceeded to a certain
limit, the pressure will increase in the ratio 1: 16, while the volume
will decrease in the ratio 8: 1, provided there be no change in the
temperature. When the gas has reached this point and is still further
compressed, the temperature will remain in steady equilibrium. At still
higher pressures, however, the temperature must fall if equilibrium
is to be maintained. According to Amagat, this will occur at 17° C.
(290° absolute) in gases like hydrogen and nitrogen, which at this
temperature are far above their critical points, and at a pressure of
300 or 250 atmospheres. When the temperature is twice as high on the
absolute scale, or at 307° C., twice the pressure will be required.
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