1bed circle ſhall be in the line F G, which let be the point I; and
becauſe that of ſuch lines as are drawn from the point G, which
is not the centre, unto the circumference of the circumſcribed
circle, the biggeſt is that which paſſeth by the centre, G F ſhall
be bigger than any other that is drawn from the point G, to the
circumference of the ſaid circle; and therefore that
rence will cut the line G H (which is equal to the line G F) and
cutting G H, it will alſo cut A H. Let it cut it in L, and
joyn the line L B. Theſe two angles, therefore, A F B and A L B
ſhall be equal, as being in the ſame portion of the circle
cumſcribed. But A L B external, is bigger than the internal H;
therefore the angle F is bigger than the angle H. And by the
ſame method we might demonſtrate the angle H to be bigger
than the angle E, becauſe that of the circle deſcribed about the
triangle A H B, the centre is in the perpendicular G F, to which
the line G H is nearer than the line G E, and therefore the
cumference of it cutteth G E, and alſo A E, whereupon the
poſition is manifeſt. We will conclude from hence, that the
ference of appearance, (which with the proper term of art, we
might call the Parallax of the fixed ſtars) is greater, or leſſe,
cording as the Stars obſerved are more or leſſe adjacent to the
Pole of the Ecliptick, ſo that, in concluſion of thoſe Stars that
are in the Ecliptick it ſelf, the ſaid diverſity is reduced to nothing.
In the next place, as to the Earths acceſſion by that motion to,
or receſſion from the Stars, it appeareth to, and recedeth from
thoſe that are in the Ecliptick, the quantity of the whole
ter of the grand Orb, as we did ſee even now, but that acceſſion
or receſſion to, or from the ſtars about the Pole of the Ecliptick,
is almoſt nothing; and in going to and from others, this
rence groweth greater, according as they are neerer to the
tick. We may, in the third place, know, that the ſaid difference
of Aſpect groweth greater or leſſer, according as the Star
ved ſhall be neerer to us, or farther from us. For if we draw
nother Meridian, leſſe diſtant from the Earth; as for example,
this D F I [in Fig. 7.] a Star placed in F, and ſeen by the ſame
ray A F E, the Earth being in A, would, in caſe it ſhould be
ſerved from the Earth in B, appear according to the ray B F, and
would make the angle of difference, namely, B F A, bigger
than the former A E B, being the exteriour angle of the
gle B F E.
becauſe that of ſuch lines as are drawn from the point G, which
is not the centre, unto the circumference of the circumſcribed
circle, the biggeſt is that which paſſeth by the centre, G F ſhall
be bigger than any other that is drawn from the point G, to the
circumference of the ſaid circle; and therefore that
rence will cut the line G H (which is equal to the line G F) and
cutting G H, it will alſo cut A H. Let it cut it in L, and
joyn the line L B. Theſe two angles, therefore, A F B and A L B
ſhall be equal, as being in the ſame portion of the circle
cumſcribed. But A L B external, is bigger than the internal H;
therefore the angle F is bigger than the angle H. And by the
ſame method we might demonſtrate the angle H to be bigger
than the angle E, becauſe that of the circle deſcribed about the
triangle A H B, the centre is in the perpendicular G F, to which
the line G H is nearer than the line G E, and therefore the
cumference of it cutteth G E, and alſo A E, whereupon the
poſition is manifeſt. We will conclude from hence, that the
ference of appearance, (which with the proper term of art, we
might call the Parallax of the fixed ſtars) is greater, or leſſe,
cording as the Stars obſerved are more or leſſe adjacent to the
Pole of the Ecliptick, ſo that, in concluſion of thoſe Stars that
are in the Ecliptick it ſelf, the ſaid diverſity is reduced to nothing.
In the next place, as to the Earths acceſſion by that motion to,
or receſſion from the Stars, it appeareth to, and recedeth from
thoſe that are in the Ecliptick, the quantity of the whole
ter of the grand Orb, as we did ſee even now, but that acceſſion
or receſſion to, or from the ſtars about the Pole of the Ecliptick,
is almoſt nothing; and in going to and from others, this
rence groweth greater, according as they are neerer to the
tick. We may, in the third place, know, that the ſaid difference
of Aſpect groweth greater or leſſer, according as the Star
ved ſhall be neerer to us, or farther from us. For if we draw
nother Meridian, leſſe diſtant from the Earth; as for example,
this D F I [in Fig. 7.] a Star placed in F, and ſeen by the ſame
ray A F E, the Earth being in A, would, in caſe it ſhould be
ſerved from the Earth in B, appear according to the ray B F, and
would make the angle of difference, namely, B F A, bigger
than the former A E B, being the exteriour angle of the
gle B F E.
An Indice in
the fixed ſtars like
to that which is
ſeen in the
nets, is an
ment of the Earths
annual motion.
the fixed ſtars like
to that which is
ſeen in the
nets, is an
ment of the Earths
annual motion.
The fixed ſtars
without the
tick elevate and
deſcend more or
leſſe, according to
their diſtance from
the ſaid Ecliptick.
without the
tick elevate and
deſcend more or
leſſe, according to
their diſtance from
the ſaid Ecliptick.
* i. e. of the
cliptick.
cliptick.
The Earth
proacheth or
deth from the
ed ſtars of the
cliptick, the
tity of the
ter of the Grand
Orb.
proacheth or
deth from the
ed ſtars of the
cliptick, the
tity of the
ter of the Grand
Orb.
The ſtars
er to us make
greater differences
than the more
more.
er to us make
greater differences
than the more
more.
SAGR. With great delight, and alſo benefit have I heard
your diſcourſe; and that I may be certain, whether I have
ly underſtood the ſame, I ſhall give you the ſumme of the
cluſions in a few words. As I take it, you have explained to us
the different appearances, that by means of the Earths annual
your diſcourſe; and that I may be certain, whether I have
ly underſtood the ſame, I ſhall give you the ſumme of the
cluſions in a few words. As I take it, you have explained to us
the different appearances, that by means of the Earths annual