It may happen, once in a while, that two stars will collide. If
the collision is a grazing one, they say, a spiral nebula will
be formed. However, a fairly close approach of two stars will
occur in vastly greater frequency and the effect of this
approach will also be to form a spiral nebula or two such
nebulae. The authors recall that our Sun is constantly ejecting
materials to a considerable height to form the prominences, and
that the attractions of a great star passing fairly close to
our solar system would assist this process of expulsion of
matter from the Sun. A great outbreak or ejection of matter
would occur not only on the side of our Sun turned toward the
disturbing body, but on the opposite side as well, for the same
reason that tides in our oceans are raised on the side opposite
the Moon as well as on the side toward the Moon. As the Sun and
disturbing star proceeded in their orbits, the stream of matter
leaving our Sun on the side of the disturbing body would try to
follow the other star; and the stream of matter leaving the
other side of the Sun would shoot out in curves essentially
symmetrical with those in the first stream. As the disturbing
star approached and receded the paths taken by the ejected
matter would be successively along curves such as are
represented by the dotted lines in Fig. 28. At any given moment
the ejected matter would lie on the two heavy lines. The matter
would not be moving along the heavy lines, but nearly at right
angles to them, in the directions that the lighter curves are
pointing. As the ejections would not be continuous, but on the
contrary intermittent, because of violent pulsations of the
Sun"s body, there would be irregularities in the two spiral
streamers. The materials drawn out of the Sun would revolve
around it in elliptic orbits after the disturbing body had
passed beyond the distance of effective disturbance, as
illustrated in Fig. 29. The orbits of the different masses
would have different sizes and different eccentricities. There
would also be a wide distribution of finely-divided material
between the main branches of the spiral. All of the widespread
gaseous matter, hot when it left the Sun, would soon become
cold, by expansion and radiation; and only the massive nuclei
would remain gaseous and hot.
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