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                  Titre : Opera omnia. Vol. 7 / edidit Ch. Frisch...

                  Auteur : Kepler, Johannes (1571-1630)

                  Éditeur : Heyder et Zimmer (Frankofurti a. M.)

                  Date d'édition : 1858-1871

                  Contributeur : Frisch, Christian (1807-1882). Éditeur scientifique

                  Sujet : Astronomie

                  Type : monographie imprimée

                  Langue : Latin

                  Format : 8 vol. : fig. et pl. ; gr. in-8

                  Format : application/pdf

                  Droits : domaine public

                  Identifiant : ark:/12148/bpt6k949604

                  Source : Université de Paris Sud 11, B2-120-7

                  Relation : Notice d'ensemble : http://catalogue.bnf.fr/ark:/12148/cb30678038g

                  Relation : http://catalogue.bnf.fr/ark:/12148/cb30678038g

                  Provenance : bnf.fr

                  Date de mise en ligne : 15/10/2007

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                  Title : Opera omnia. Vol. 7 / edidit Ch. Frisch...

                  Author : Kepler, Johannes (1571-1630)

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                  Ex Ephemeridibus Kepleri.

                  604

                  orbitae, foeneratur vero latitudini verae 3' 2", ut sit jam vera CG 10' 26"
                  cum reductione 80", itaque C locus ecliptieus 20° 9' 57" et A locus Solis
                  jam 19° 9' 7" et superatio vera AC 10 0' 50". Ad superiorem etiam ascen-
                  sionem obliquam pro una hora adde 15° 2' 30", erit hic jam asc. obliqua
                  194° 9' 30", oriente 10° 23' ^£±, cujus angulus orientis est 64" 45' et Q)
                  a nonagesimo 10° 23' Q distabit 80" 13'. Methodo igitur eadem qua prius
                  inveniuntur parallaxes longitudinis 53' 7", latitudinis 25' 42", quarum illa,
                  quippe occidua, demta de superatione vera AC 0; 50" relinquit AE 7' 45",
                  superationem visam, ex quo constat, jam transivisse medium ista vero, dimi-
                  nuta latitudine secundi momenti CG, fit visa latitudo El 14' 58" australis,
                  cum priori momento major fuerit inventa. Sic Luna, quae motu vero FG
                  discessit a nodo N, viso HI videtur ad eum accedere, majoribus quidem decre-
                  raentis. Ex hac vero superatione AE et hac latitudine visa El invenitur AI
                  distantia centrorum 1G' 54".

                  Ex duabus igitur distantiis centrorum, AH, AI, et compositis in unum
                  priore antecessione visibili AD et praesenti superatione AE, ut sit DE 28' 19",
                  ad filura praecepti 170. Rudolph. inquiremus maximae obscurationis momentum
                  et quantitatem, si prius augeatur DE uno horario Solis, ut sit 30' 47", visa
                  vero Jatitudo minor El a majori ejusdem plagae DH auferatur et per difle-
                  rentiam HK 4' 2G" perque DE auctam indagetur distantia duorum Lunae
                  situum HI 31' G", ut sit hacc latus trianguli tertium, pars quasi viae Lunae
                  visibilis, latera vero duo reliqua minora seu ardua sint illaé inventae distan-
                  tiae centrorum visibiles AH, AI. Eas quidem jubet praeceptum prius augerc
                  portionibus sibi analogis de motu Solis intermedio, qui hic fuit unius horae;
                  sed id fit itrt-p'Mz nec citra damnum, nisi anguli AHI, AIH (ut in principiis
                  et finibuis centralium, ad quas respicit praeceptum) fuerint omnino parvi. Facie-
                  mus igitur id hoc loco magis ex arte: augebimus enim potius AD, AE et
                  per auctas de novo quaeremus AH, AI; additis illi 1' 50", huic 0' 40" fiunt
                  22' 24" et 8' 23", quae cum latitudine visibili HI) 19' 24" et El 14' 58"
                  compositis antilogarithmis dant ipsorum HA, AI corrcctarum distantiarmn cen-
                  trorum antilogarithmos 3.715 et 1.246. y differentia seu argumentum 2.469.
                  Hoc vero argumentum asscquimur, si latus tertium HI dirimamus in partes
                  HL 24' 56" et LI 6' 10"; horum enim antilogarithmi ablati ab antilogarithmis
                  arduorum HA et AI relinquunt communem 1.085 perpendiculi AL ir>' 1".
                  Tanta debebat evenire distantia centrorum in obscuratione niaxima Viennensi,
                  si parallacticus Proteus vincula trianguli rectilinei pateretur.

                  Quia igitur via Lunae obliqua in una hora inventa fuit 31' G", parti-
                  culae ejus 24' 5(>" conficientur (stante hac proportione) minutis 40. 20",
                  quare summa obscuratio esset h. 5. 32' 5" apparente Vinnnac. Computavi
                  etiam ad h. G. 32' ipsius occasus Solis invenique distantiam centrorum 33' 48",
                  tribus ferc scrupulis majorem summa semidiametrorum. Itaque Viennae desi-
                  neret eclipsis solis 6 minutis ante Solis occasum, hora se. 6. 20'.
                  Dcnique calculus ad haec tria momenta repetitus loci Lunae visibilis
                  repraesentavit distantias centrorum ad h. 4. 40' scr. 30. 40" ad h. 5. 31l/2'
                  scr. AL 15' 32", ad h. 6.28' scr. 30. 16", et Lunam quidern in medio
                  adhuc ante Solem uno scrupulo nondum ergo crat appropinquatio centrorum
                  proxima; in hac enim Luna Solem jam superaverit necesse est, quia versus
                  nodum visibilem movetur, miuuens visam latitudinem. Initium ergo correctis-
                  siraum Viennae h. 4. 3i)l/2, maxima obscuratio li. f>. 35 Va, finis h. G. 291/
                  defraudatque nos triangulum in distantia centrorum circa medium dimidio scru-


                  Source: gallica.bnf.fr / Université de Paris Sud 11, B2-120-7

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