Selected quad for the lemma: day_n

Word A	Word B	Word C	Word D	Occurrence	Frequency Band	MI	MI Band	Prominent
day_n	eclipse_n	minute_n	moon_n	12,931	5	12.8749	5	true

Text snippets containing the quad

ID	Title	Author	Corrected Date of Publication (TCP Date of Publication)	STC	Words	Pages
A44885	A learned treatise of globes, both cœlestiall and terrestriall with their several uses / written first in Latine, by Mr. Robert Hues, and by him so published ; afterward illustrated with notes by Jo. Isa. Pontanus ; and now lastly made English ... by John Chilmead ...; Tractatus de globis et eorum usu. English	Hues, Robert, 1553-1632.; Chilmead, Edmund, 1610-1654.; Pontanus, Johannes Isacius, 1571-1639.; Molyneux, Emery.	1659 (1659)	Wing H3298; ESTC R1097	145,949	311

a Cubic all and some a Pyramidall forme yet this opinion of it's Roundnesse with greatest consent of reason at length prevailed the rest being all exploded Now wee affirme it to be round yet so as that wee also admit of it's inequalities by reason of those so great eminences of hills and depression of vallies Eratosthenes as hee is cited by Strabo in his first book saith that the fashion of the Earth is like that of a Globe not so exactly round as an artificiall Globe is but that it hath certain inequalities The earth cannot be said to be of an exact orbicular forme by reason of somany high hilles and low plaines as Pliny rightly observes And Strabo also in his first book of his Geography saith that the Earth and the water together make up one sphaericall body not of so exact a forme as that of the Heavens although not much unlike it This assertion of the roundnesse of the Earth with the intervening Sea is confirmed also by these reasons For first that it is round from East to West is proved by the Sun Moon and the other Stars which are seen to rise and set first with those that inhabit more Eastwardly and afterward with them that are farther West The Sun riseth with the Persians that dwell in the Easterne parts foure hours soonner then it doth with those that dwell in Spaine more Westward as Cleomedes affirmes The same is also proved by the observing of Eclipses especially those of the Moon which although they happen at the same time are not yet observed in all places at the same houre of the day or night but the hour of their appearing is later with them that inhabite Eastward then it is with the more Westerne people An Eclipse of the Moon which Ptolomy reports lib. 1 Geogr. cap. 4. To have been seen in Arbela a town in Assyria at the fift houre of the night the same was observed at Carthage at the second houre In like manner an Eclipse of the Sun which was observed in Campania to be betwixt 7. and 8. of the Clock was seen by Co●…bulo a Captain in Armenia betwixt 10●… and 11. as it is related by Pliny Now that it is also of a sphaericall figure from North to South may be clearly demonstrated by the risings settings elevations and depressions of the Stars and Poles The bright Star that shines so resplendently in the upper part of the sterne of the Ship Argo and is called by the Greeeks 〈◊〉 〈◊〉 〈◊〉 〈◊〉 〈◊〉 is scarcely to bee seen at all in Rhodes unlesse it bee from some eminent high place yet the same is seen very plainly in Alexandria as being elevated above the Horizon about the fourth part of a signe as Proclus affirms in the end of his book de Sphaera For I read it Conspicuè cernitur not as it is commonly Prorsus non cernitur notwithst anding that both the Greek text and also the Latine translation are against it Another argument may bee taken from the figure of the shadow in the Eclipse of the Moon caused by the interposition of the Earths opacous body Which shadow being Sphaericall cannot proceed from any other then a round Globous body as it is demonstrated unto us out of Opticall principles But this one reason is beyond all exception that those that make toward the Land at the Sea shal first of all descry the tops of the hilles onely a●…d afterwards as they draw nearer to shore they see the lower parts of the same by little and little Which cannot proceed from any other cause then the gibbosity of the Earths superficies As for those other opinions of the hollow Cubicall Pyramidall and plaine figure of the Earth you have them all largely examined both in Theon Ptolomies Interpreter Cleomedes and almost in all our ordinary Authours of the Sphaere together with the reasons why they are rejected Yet that old conceit of the plainnesse of the Earths superficies is again now at last tanquam Crambe recocta set forth in a new dresse and thrust upon us by Franciscus Patricius who by some few eold arguments and misunderstood experiments endeavours to confirme his own and consequently to overthrow that other received opinion of the sphaericall figure of the Earth I shall onely lightly touch at his chiefest arguments my present purpose and intention suffering mce not to insist long on the confutation of them And f●…rst of all the great beight of Hills and the depression of vallies so much disagreeing from the evennesse of the plain parts of the Earth scem to make very much against the roundnesse of the Earth Who can hear with patience saith hee that those huge high mountains of Norway or the mountaine Slotus which lies under the Pole and is the highest in the world should yet be thought to have the same superficies with ●…he Sealying beneath it This therefore being the chiefest reason that m●…y seem to overthrow the opinion of the Earth and Seas making up one sphaericall body let us examine it a little more nearly and consider how great this inequality may bee that seems to make so much against the evennessc of this Yerrestitall Globe Many strange and almost incredible things are reported by Aristotle Mela Pliny and Solinu●… of the unusuall height of Atho●… an Hill in Macedonia and of Casius in Syria as also of another of the same name in Arabia and of the monntaine Caucasus And among the rest one of the most miraculous things which they have observed of the mountain Athos is that whereas it is situate in Macedony it casts a shadow into the market place at Myrrhina a Town in the Island Lemnos from whence Athos is distant 86. miles But for as much as Athos lies Westward from Lemnos as may appeare out of Ptolomies Tables no marvail that it casts so large a shadow seeing that wee may observe by dayly experience that as well when the Sunriseth as when it sets the shadowes are always extraordinary long But that which Pliny and Solinus report of the same mountain I should rather account among the rest of their fabulous Stories where as they affirm it to be so high that it is thought to be above that region of the aire whence the rain is wont to fall And this opinion say they was first grounded upon a report that there goes that the ashes which are left upon the Altars on the top of this hill are never washed away but are found remaining in heapes upon the same To this may be added another testimony out of the Excerpts of the seventh booke of Strabo where it is said that those that inhabite the top of this mountain do see the Sun three hours sooner then those that live neare the Sea side The height of the mount●…in Caucasus is in like manner celebrated by Aris●…otle the top whereof is enlightned by the Suns b●…ames the third part of the night both morning and evening No lesle fabulous is that which is reported

yeare 1598. upon the eleventh day of February at foure of the Clock and sixteen minutes in the morning and that at Regiomont a City in Borussia whose longitude or distance from the Canary Islands is 41. gr 16. m. For this Longitude where these Tables calculated Now I set my self to observe this same Eclipse at Marpurg and find it to happen at three of the Clock and twelve minutes on the same day of February Now because the number of hours here is lesse it appeares that Marpurg is more Westward then Regiomont Therefore I take away a lesse number from the greater that is 3. h. 12. m. from 4. h. 16. m. and the remainder is 1 h. 4. minutes which sheweth the difference of longitude in hours which makes up sixteen degrees Therefore I again substract these degrees of difference from the longitude of Regiomont as being more Eastward then Marpurge and so I find the Latitude of Marpurge from the Canary Island to be 25. gr 16. minutes CHAP II. How to find the Latitude of any place THe latitude of a place is the distance of the Zenith or the verticall point thereof from the AEquator Now if you desire to find out the latitude of any place expressed in the Globe you must apply the same to the Meridian and reckon the number of the degrees that it is distant from the AEquator For so much is the Latitude of that place And this also you may observe that the Latitude of every place is alwayes equall to the elevation of the same place For look how many degrees the verticall point of any place is distant from the AEquator just so many is the Pole elevated above the Horizon as you may prove by the Globe if you so order it as that the Zenith of the place be 90. degrees distant every way from the Horizon PONT Seeing that the Latitude of every place is alwayes equall to the elevation of the Pole It will not be amisse to shew how the elevation of the Pole or the Latitude of any region may be found out by the observing of the same fixed Star in the Heavens which is so neare the Pole a●… that it never sets in that region which to doe you must work thus You must observe both the least and also the greatest altitude of the sad Star both which must necessarily happen in the Meridian the least whereof will be beneath the Pole and the greatest above it Which done you must adde the least altitude of it to the greatest and so the halfe of the degrees thus numbered together will bee the latitude of the Pole and latitude of that plaee An example whereof may be this The first Star of the three in the taile of the great Beare is in his least altitude observed at London to be about 11. gr and the greatest altitude of the same when it is above the Pole is found to be neare upon 92. degrees Both which numbers being added together do make up 103. halfe of which Summ namely 51⅓ is the true elevation ond Latitude of London CHAP. III. How to find the distance of two places and angle of position or situation IF you set your Globe in such sort as that the Zenith of one of the places bee 90. gr distant every way from the Horizon and then fasten the Quadrant of Altitude to the Verticall point and so move it up and down untill it passe through the Vertex of the other place the number of degres intercepted in the Quadrant betwixt the two places being resolved into furlongs miles or leagues as you please will shew the true distance of the places assigned And the other end of the Quadrant that toucheth upon the Horizon will shew on what wind or quarter of the World the one place is in respect of the other and what Angle of Position as they call it it hath For the Angle of Position is that which is comprehended betwixt the Meridian of any place and a greater circle passing through the Zeniths of any two places assigned and the quantity of it is to be numbred in the Horizon As for example The Longitude of London is twenty six degrees and it hath in Northern latitude 51. degrees and an halfe Now if it be demanded what distance and angle of position it beareth to Saint Michaels Island which is one of the Azores we must proceed thus to find it First let the Northern Pole be elevated 51½ degrees which is the latitude of London Then fastening the Quadrant of Altitude to the Zenith of it that is to say fifty one degrees and an halfe Northward from the AEquator wee must turne it about till it passe through Saint Michaels Island and wee shall find the distance intercepted betwixt these two places to be 11. gr 40. m. or thereabout which is 280 of our leagues And if we observe in what part of the Horizon the end of the Quadrant 〈◊〉 we shal find the Angle of Position ●…o sall neare upon 50. gr betwixt Southwest and by-west And this is the situation of this 〈◊〉 in respect of London PONT The 〈◊〉 of places ●…ring only in latitude may bee found after this manner First you must substract the lesser Latitude from the greater resolving a degree in minutes if the substraction cannot be done otherwise conveniently Then multiply the degrees by 15. and divide the minutes by 4. and the summ produced will be the distance of those two places in common Germane miles one whereof containeth foure of our English miles As for example Basile in Germany and Geneva have both the same longitude but differ in Latitude which at Basile is 47. gr 30. m. and at Geneva 45. gr 45. m. Therefore substracting the lesser from the greater the remainder will bee 1. gr 45. m. which being reduced into Germane miles will amount to 26. and a quarter or a mile which is the distance of these two places assigned Now if the place proposed bee in diverse Hemispheres then the degrees and minutes of Latitude must first be added together and so the whole resolved into miles as formerly hath been said As for example The Cape of good hope in Africa and Constantinople are almost situate under the same meridian but in diverse Hemisphaeres Now the elevation of the Pole Articke at Constantinople is 43. gr or thereabout and at the Cape of good hope the Antarctick Pole is elovated aboue 35. gr the whole summ therefore is 73. degrees that is to say 1170. Germane miles The distance of places differing onely in longitude is found thus First substract the lesse number from the greater then look in the Table here under written how many miles answere to a degree 〈◊〉 every Parallel seeking for the degree of Latitude in the first columne descending and the number of miles over against it Then lastly let the difference of longitude be multiplyed into miles and minutes and you have your desire As for example Naples and Ilium or Troy are in

Ancient Greekes who first of all observed the places and situation of the fixed Starrs and expressed the same by Asterismes and constellations the first Star of Aries was then a very smal space distant from the very Intersection For in Thales Milesius his time it was two degrees before the Intersection in the time of Meton the Athenian it was in the very Intersection in Timocharis his time it came two degrees after the Intersection And so by reason of it's vicinity the Ancients assigned the first part of the Zodiack to Aries the second to Tauru●… and so the rest in their order as it is observed by succeeding ages euen to this very day PONT Thales Milesius was the first that calculated the time of the AEquinoxe and Eclipses and he flourished about the yeares of the Creation 3370. which was about 634. yeares before Christ Meton lived about 431 yeares before Christ in the yeare of the Creation 3517. He was the Son of 〈◊〉 and was a man of excellent knowledg in Astronomy He also first invented the Moones Circle of 19 yeares whose first new Moon fell upon the 13 day of the month Scriophorion which is the same with our 16 of June being on a Friday Vid D●…dorum Siculum Censorinus writes of him thus Praeterea sunt c. There are saith he besides many other great yeares as the Metonicall yeare which Meton the Athenian invented and consisted of 19. common yeares c. Timochares was by nation an Alexandrian and he lived 300 yeares before Christ. Vnder this Circle the Sun and the rest of the Plane●…s finished their severall courses and periods in their severall manner and time The Sun keepes his course in the midedst of the Zodiaque and therewi●…h describeth the Ecliptick circle But the rest h●…ve all of them their latitude and deviations ●…rom the Suns course or Ecliptick By reaso of which their digressions and extravagations the ancients assigned the Zodiaque 12. Degrees of Latitude But our moderen Astronomers by reason of the Evagations of Mars and Venus have added on each side two degrees more so that the whole latitude of the Zodiaque is confined within 16. degrees But the Ecliptick onely is described on the Globe and is divided in like manner as the other circles into 360. degrees PONT The whole latitude of the Zodiaqu●… is divided into two parts by the Ecliptick which is the circle or Circumference under which the Sun steeres his course continually whence it is called in Latine Via Solis Orbita Solis the Sun●… high way And in G●…eek 〈◊〉 〈◊〉 〈◊〉 〈◊〉 〈◊〉 a Circle divideing the Zodiack in the middest And it is called the Ecliptick because the Eclipses of the Sun and Moon never haeppen but when they are either in conjunction or opposition under this line or very near the same The Sun runneth thorough this Circle in his yearly motion finishing every day in the yeare almost a degree by his Meane motion that is 59. minutes 8. seconds And in this space he twice cro●…seth the AEquator in two points equally distant from each other So that when he passeth over the AEquator at the beginnings of Aries and Libra the dayes and nights are then of equall length And so likewise when the Sun is now at the farthest distance from the AEquator and is gotten to the begining of Cancer or Capricorne hee then causeth the Winter and Summer So Istice●… I am not ignorant that Vitruvius Pliny Thco●… Alexandrinus Censorinus and Columolla are of another opinion but they are upon another ground when as they say that the AEquinoxes are when as the Sun passeth through the eighth degree of Aries and Libra and then it was the midst of Summer and winter when the Sun entered into the same degree of Cancer end Capricorne But all these Authors defined the Solstices by the returning of the shadow of Dials which shadow cannot bee perceived to return back again as Theon saith till the Sun is entered into the eighth degree of Libra and A●…ies PONT The office and use of the Zodiack is Fi●…st in that it is a rule or measure of the proper motion of the Planets Secondly By the helpe of the Zodiack the true place of all the Starrs are sound besides it may be knowne in what signe any fixed Starr or Planet may be said to be Thirdly It sheweth the Latitude of the Planets and fixed Starrs Fourthly All Eclipses happen when the Sun and Moon are under the Ecliptique Fifthly The obliquity of the Ecliptique is the cause of the inequality of the artificial dayes and nights The space wherein the Sun is finishing his course through the Zodiack is defined ●…o be a Yeare which consists of 365. dayes and almost 6. hours But they that thinke to find the exact measure of this period will find themselves frustrate for it is finished in an unequall time It hath been alwayes a controversie very much agitated among the Ancien●… Astronomers and not yet determined Philolaus a Pythagoraean determines it to bee 365. d●…yes but all the rest have added something more to this number Harpalus would have it to be 369. dayes and a halfe Democritus 365. dayes and a quarter adding besides the 164 parts of a day Oenopides would have it to be 365. dayes and almost 9. hours Meton the Athenian determineth it to be 365. dayes 6. hours and almost 19. minutes After him Calipius reduced it to 365. dayes and 6. hours which account of his was followed by Aristarchus of Samos and Archimedes of Syracusa And according to this determination of theirs Julius Caesar defined the measure of his Civile yeare having first consulted as the report goes which one Sosigines a Peripatetick and a great Mathematician But all these ●…xcept Philolaus who came short of the just measure assigned too much to the quantity of a yeare For that it is somewhat less then 365. dayes 6. houres is a truth confirmed by the most accurate observations of all times and the skilfullest Artists in Astronomicall affaires But how much this space exceedeth the just quantity of a yeare is not so easie a matter to determine Hipparchus and after him Ptolomy would have the 300. part of a day substracted from this measure for Jacobus Christmannus was mistaken when he affirmed that a Tropicall 〈◊〉 according to the opinion of Hipparchus and Ptolomy did consist of 365. dayes and the 300 part of a day For they doe not say so but that the just quantity of a yeare is 365. dayes and 6. hours abating the 300. part of a day as may be plainly gathered out of Ptolomy Almagest lib. 3. Cap. 2. and a●… Christmannus himselfe hath else where rightly observed Now Ptolomy would have this to be the just quantity of a yeare perpetually and immutably neither would he be perswaded to the contrary notwithstanding the observati●…s of Hipparchus conc●…ning the inequality of the Suns periodiacall revolution But yet the observations of succeeding times compared with those of Hipparchus

Starrs and fixed not as if these were indeed fixed in one certain place and altogether without motion and the other only moveable and erraticall but these appellations are onely given then comparatively in which sence also they are to be understood For seeing that the fixed Starrs were observed alwayes to keep the same places in the eighth Sphaere and the same distance srom each other notwithstanding that they are alwayes in continuall motion caused by the vertue of the first Moveable which carrieth them about in the space of twenty foure hours But the Planets besides this motion have a proper motion of their owne so that they keep neither their the same distance from the fixed Starrs nor yet the same aspect to each other for these reasons were the one called Fixed and the other Planets For otherwise if the Planets be considered severally each one by himselfe there is nothing more certain then their periodicall motion So that Tully alluding hereto would have the Planets to bee called Errantes by Antiphrasis quam minimè errantes The Planets exceeding those two greater lights the Sun and Moon are five in number A●… which beside the Diurnal motion by which they are carried about from East to West by the Rapture of the first Moveable have also a free proper motion of their owne which finish from West to East according to the succession of the Signes upon the Poles of the Zodiaque each of them in a severall manner and space of time Their order in the Heavens and periods of their motions being such as followeth Saturne called in Greek 〈◊〉 〈◊〉 〈◊〉 〈◊〉 〈◊〉 or 〈◊〉 〈◊〉 〈◊〉 〈◊〉 〈◊〉 and by Julius Higinus Stella Solis the Star of the Sun is the highest of all the Planets and 〈◊〉 about the greatest 〈◊〉 but doth not therefore appear to be the least of all the Planets as Pliny hence conjectured Hee finisheth his Periodical course in twenty nine yeares five months fifteen dayes according to Alfraganus Jupiter in Greek Zeus and 〈◊〉 〈◊〉 〈◊〉 〈◊〉 〈◊〉 moveth through the Zodiaque in the space of eleven yeares ten moneths and almost 16. dayes Mars 〈◊〉 〈◊〉 〈◊〉 〈◊〉 〈◊〉 and 〈◊〉 〈◊〉 〈◊〉 〈◊〉 〈◊〉 which is also cal-called by some Hercules his Star finisheth his course in two yeares Sol the Sun in Greek 〈◊〉 〈◊〉 〈◊〉 〈◊〉 〈◊〉 performeth his course in a yeare that is to say three hundered sixty five dayes and almost sixe hours Venus 〈◊〉 〈◊〉 〈◊〉 〈◊〉 〈◊〉 called by some June's Starr by thers Isis and by others The Mother of the Gods when it goeth before the Sun it is called 〈◊〉 〈◊〉 〈◊〉 〈◊〉 〈◊〉 the day Star appearing like another 〈◊〉 Sun and as it were matu●…g the day But when it followeth the Sun in the Evening p●…otracting the light after the Sun is ●…er and supplying the place of the Moone it is then called 〈◊〉 〈◊〉 〈◊〉 〈◊〉 〈◊〉 the Evening Star The names of which Star Pythagoras Samius 〈◊〉 〈◊〉 first to have observed about the thi●… ie 2d. Olympiad as Pliny relates lib. 2. cap. 8. It p●…meth its course in a yeares space or thereabout and is never distan●… from the Sun above forty six degrees according to Timaeus his computation Notwithstancing our later Astronomers herein much more 〈◊〉 then h●… allow it two whole signes or 60 degrees which is the utmost limit of its deviation from the Sun Mercury in Greek 〈◊〉 〈◊〉 〈◊〉 〈◊〉 〈◊〉 and 〈◊〉 〈◊〉 〈◊〉 〈◊〉 〈◊〉 called by some Appollo's Star 〈◊〉 his course through the Zodiaque in a yeare also And according to the opinion of Timeus and Sosigenes 〈◊〉 ever distant from the Sun above 25. gr or 〈◊〉 our later writers will have it not above a who●…e 〈◊〉 or 30. degrees Luna 〈◊〉 〈◊〉 〈◊〉 〈◊〉 〈◊〉 the Moon is the lowest of all the Planets and finisheth her course in twenty seven dayes and almost eight hours The various shapes and appearances of which Planets seeming sometimes to bee ●…ned sometimes equally divided into two halfes sometimes finished like an Imperfect circle and sometimes in a respect circular 〈◊〉 together with the other diversities of this Star were first of all observed by Endymion as it is related by Pliny whence sprung that Poëticall fiction of his being in love with the M●…on All the●…e Planets are carried in Orbes which are Eccentrical to the earth that is which have not the same center with the earth The Semidiameter of which Orbes compared to the Semidiameter of the earth have this proportion as is here set down in this Table Of what parts the ●…emidiameter of the Earth i. 1. Of t●…e same the 〈◊〉 ter of the Orbe of Luna 1. 48. 56 m. Mercury 116. 3 m. Venus 641. 45. m Sol 1165. 23. m. Mars 5022. 4. m Jupiter 11611. 31. m. Saturne 17225. 16. m The Eccentricities of the Orbes compared to the Orbs themselves have this proportion Of whatparts the Semidiameter of the Deferent is 60. Of the same the Eccentricity of Luna 18 12. 28. m. 30 sec Maurolycus out of Alphons Mercury 2. 0. m. Venus 1. 8. m. Sol 2. 16. m 6. sec. Mars 6. 0 m. Jupiter 2. 45 m. Saturne 3. 25 m. The Eccentricities of some of the Planets especially of the Sun are found to have decreased and growne less since Ptolomyes●…ime ●…ime For Ptolomy sets down the Eccentricity of the Moon to be 12. gr 3●… m. but by Alphonsus it was found to be but 13 gr 28. m. and an halfe Ptolomy assigned Eccentricity to Venus 1 gr 14. m Alphonsus 1. gr 8. m. Ptolomy found by his owne observations and also by those that Hipparchus had made that the Eccentricity of the Sun was 2 gr 30. m. Alphonsus observed it in his time to be but 2 gr 16. m. and the 10th part of a minute In the year of ou●… Lord 1312 it was found to be 2. gr 2. m. 18. sec. Copernicus found it to be lesse yet then that and to be but 1 gr 56 m 11. sec. So that without just cause did the Illustrious Julius Scaliger think Copernicus his writings for this reason to deserve the Sponge and the Author himself the Bastinado he●…ein dealing more hardly with Copernicus then he deserves PONT Besides the Eccentricities of the Planets it is worth our paines also to observe their Magnitudes And this consists especially in the knowledge of their Diameters and what proportion they beare to each other For the Diameter of a Planet compared to the Diameters of the Earth is after this manner following The Diameter of Saturne Compared ●…o the Diameter of the Earth is as 9 10 2 Jupiter 32 7 Mars 7 6 Sol 11 2 Venus 3 10 Mercury 1 28 Luna 5 17 The Diameter of the Sun compared to the Diameter of the Moon beareth the same proportion that is betwixt 187. and 10. And now that which is said may be demonstrated by an example let us suppose the Diameter of the Sun in proportion to the Diameter of the Earth to be

reach to the 30 gr and be called the AEgyptian The fourth the Syrian ending at the 40. gr The fifth the Italian to the 50. gr The 6. the English or Germane extending to the 60. gr The seventh the Suecian or Lapland Climate reaching to the 70. gr The eighth the Frozen Climate ending at the 80. gr And the Ninth and last the Polar Climate reaching to the Pole it selfe So likewise the same Method might bee observed on the othes side of the AEquinoctiall and then by this meanes each Hemisphaere should have nine Climates whereof seven would be convenient for habitation and the Parallels might passe through every fifth degree And the situation of any place might be known by the number of degrees of the Poles elevation So Rome because it hath above 40. gr of latitude is in the fourth Westphalia in the fifth Sicily in the third Calecur the chiefe City in India in the second Zeilan in the first and so of the rest CHAP. I. How to find the Longitude Latitude Distance and Angle of Position or situation of any place expressed in the Terrestriall Globe THe Ancient Geographers from Ptolomies time downward reckon the longitude of places from the Meridian which passeth through the Fortunate Islands which are the same that are now called the Canary Islands as the most men do generally believe but how ●…ightly I will not here stand to examine I shall ●…nely here advertise the reader by the way that the latitude assigned by Ptolomy to the Fortunate Islands falleth something of the widest of the Canary Islands and agreeth a great deal nearer with the Latitude of those islands which are known by the name of Cabo Verde For Ptolomy placed all the Fortunate Islands within the 10 gr 30. m. and the 16. gr of Northern latitude But the Canary Islands are found to bee distant from the AEquator at the least 27 degrees The Arabians began to reckon their Longitude at that place where the Atlantick Ocean driveth farthest into the maine land which place is tenn degrees distant Eastward from the Fortunate Islands as Jacobus Christmannus hath observed out of Abilfedea Our Modern Geographers for the most part beginn to reckon the Longitude of places from these Canary Islands yet some beginn at those Islands which they call Azores and from these bounds are the Longitude of places to be reckoned in these Globes whereof we speake Now the Longitude of any place is defined to be an Arch or portion of the AEquator intercepted betwixt the Meridian of any place assigned and the Meridian that passeth through Saint Michales Island which is one of the Azores or of any other place from whence the Longitude of places is wont to bee determined Now if you desire to know the Longitude of any place expressed in the Globe you must apply the same place to the Meridian and observe at what place the Meridian cutteth the AEquator reckon the degree of the AEquator from the Meridian of Saint Michaels Island to that place for so many are the degrees of longitude of the place you look for In the same manner may you measure the distance of longitude betwixt any other two places that are described in the Globe For the difference of Longitude is nothing else but an Arch of the AEquator intercepted betwixt the Meridian of the same places Which difference of Longitude many have endeavoured to set down diverss wayes how to find by observation But the most certain way of all for this purpose is confessed by all learned Writers to be by the Eclipses of the Moon But now these Eclipses happen but seldom but are more seldom seen yet most seldome and in very few places observed by the skilfull Artists in this Science So that there are but few Longitudes of places designed out by this meanes Oro●…us Fin●…us and Johannes Wernerus before him conceived that the difference of Longitude might be assigned by the known as they presuppose it motion of the Moon and the passing of the same through the Meridian of any place But this is an uncertaine and ticklish way and subject to many difficulties Others have gon other wayes to work as namely by observing the space of the AEquinoctiall hours betwixt the Meridians of two places which they conceive may be taken by the help of Sun Dials or Clocks or Houre-glasses either with water or sand or the like But all these conceits long since de●…ed having been more strictly and accurately examined have been disallowed and rejected by all learned men at least those of riper judgments as being altogether unable to performe that which is required of them But yet for all this there are a kind of trifling Impostors that make publick sale of these toyes or worse and that with great ostentation and boasting to the great abuse and expense of som men of good note and quality who are perhaps better stored with money then either learning or judgment But I shall not stand here to discover the errours and uncertainties of these instruments Only I admonish these men by the way that they beware of these fellows least when their noses are wiped as we say of their money they too Iate repent them of their ill-bought bargaines Away with all such trisling cheating rascals PONT If you would know how to find out the longitude of any place by the Eclipse of the Moon you must first goe to some Ephemerides as the 〈◊〉 Tables or of any other learned Mathematicians calculation and see what hour such an Eclipse of the Moon shall happen at that place for which the said Tables or Ephemerides were made Then afterward you must observe the same Eclipse in that place whose longitude you desire to know Now if the time of the Eclipse agree with that other for which the Tables were made then you may conclude that both places have the same latitude and are situate under the same Meridian But is the number of the hours be more then the place you are in is suuate more Eastward you must therefore substract the less number out of the greater and the remainder must be converted into degrees and minutes multiplying the hours by fifteen and deviding the minutes of hours if there be any by foure for so will the number of degrees arise and if there remain any minutes after the division they must bee multiplyed again by fifteen and so will the number of the minutes of degrees arise by which these places are distant from each other which distance is called the difference of longitude This difference must bee added to the Longitude of that place for which the Tables were calculated if the other place be more Eastward otherwise if it bee more Westward it is to bee substracted from the longitude of the other An example herof is thus proposed by Adrianus Metius in his Doctrina Sphaerica I find saith hee out of the Prutenick Tables by exact calculation that there will be an Eclipse of the Moon in the