i »584 ) 
The Z}fes oftkefe Meridian hflrumnts. 
1. You may fee with all imaginable exaftnefs, when it 
is Noon even to i, 2, or at moft 3 Seconds of Time* For 
you may fee when the very Limb of theSuntoucheth the 
Meridian, and whilft all his Disk is paffing it. So that 
by much it exceedeth all Sun-Dials : fo far that if you 
once ufe this Inftrument, you vviU be ready to layafide 
all Sun-Dialb^ the beft of which (unlefs we except Mr 
MolineHx'%) can never (hew the Time to one or many 
Seconds. 
But befides all this, another vaft conveniency is, That 
it will j^^ moft LdtitHdes. So that there is no need of ha- 
ving a ftria regard to the Elevation of the Pole, nor 
any danger of error in making and fetting, as is in moft 
other Inftruments, but all is with eafe and certainty per- 
formed. Therefore, 
idly. Into whatfoever place you come, you mayea- 
fily fee the Errors of the Sun- Dials there, and which go 
trueft, and which falfe. 
gdly. As the Sun, fo alfo the fixt Stars may be feen to 
tranfit the Meridian , whereby the Hour of the Night may 
as exactly be known, as of the Day by the Sun, knowing 
the R. Afc of the Star that tranfits. For (as before for 
the Pole-Star) fobftraft the R. Afc. of the Sun from the 
R. Afc. of the Star, the Remainder converted into Time, 
is the time of that Star's Culmination or Southing. And 
if 13 hours be added or fubftraded (making due Allow- 
ance for the alteration of the Suns R. Afc. in that time) 
it (heweth the exafl: time of that Star's coming to the 
Meridiati Northward* 
4th!y, The Hour of the Day and Night being thus to 
I, 2 or 3 Seconds difcoverable by the aforelaid Inftru- 
mentSt, I doubt not but that they may be ufeful in finding 
the exaS: Difference of Meridians^ either by the Eclipfes 
