A forgotten solar model
This paper analyses a kinematic model for the solar motion by Quṭb al-Dīn al-Shīrāzī, a thirteenth-century Iranian astronomer at the Marāgha observatory in northwestern Iran. The purpose of this model is to account for the continuous decrease of the obliquity of the ecliptic and the solar eccentrici...
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| Published in | Archive for history of exact sciences Vol. 70; no. 3; pp. 267 - 291 |
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| Main Author | |
| Format | Journal Article |
| Language | English |
| Published |
Berlin/Heidelberg
Springer
01.05.2016
Springer Berlin Heidelberg |
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| Abstract | This paper analyses a kinematic model for the solar motion by Quṭb al-Dīn al-Shīrāzī, a thirteenth-century Iranian astronomer at the Marāgha observatory in northwestern Iran. The purpose of this model is to account for the continuous decrease of the obliquity of the ecliptic and the solar eccentricity since the time of Ptolemy. Shīrāzī puts forward different versions of the model in his three major cosmographical works. In the final version, in his Tuḥfa, the mean ecliptic is defined by an eccentric of fixed mean eccentricity and a mean obliquity fixed with respect to the celestial equator, and the center of the epicycle, which is inclined to the eccentric, moves on the eccentric with an annual period. By an additional slow motion of the sun on the epicycle, the true eccentricity of the solar deferent, defined by the annual motion of the sun, and the sun's extreme declination from the equator change, accounting for the reduction of the eccentricity and the obliquity of the ecliptic since the time of Ptolemy. |
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| AbstractList | This paper analyses a kinematic model for the solar motion by Quṭb al-Dīn al-Shīrāzī, a thirteenth-century Iranian astronomer at the Marāgha observatory in northwestern Iran. The purpose of this model is to account for the continuous decrease of the obliquity of the ecliptic and the solar eccentricity since the time of Ptolemy. Shīrāzī puts forward different versions of the model in his three major cosmographical works. In the final version, in his
Tuḥfa
, the mean ecliptic is defined by an eccentric of fixed mean eccentricity and a mean obliquity fixed with respect to the celestial equator, and the center of the epicycle, which is inclined to the eccentric, moves on the eccentric with an annual period. By an additional slow motion of the sun on the epicycle, the true eccentricity of the solar deferent, defined by the annual motion of the sun, and the sun’s extreme declination from the equator change, accounting for the reduction of the eccentricity and the obliquity of the ecliptic since the time of Ptolemy. This paper analyses a kinematic model for the solar motion by Quṭb al-Dīn al-Shīrāzī, a thirteenth-century Iranian astronomer at the Marāgha observatory in northwestern Iran. The purpose of this model is to account for the continuous decrease of the obliquity of the ecliptic and the solar eccentricity since the time of Ptolemy. Shīrāzī puts forward different versions of the model in his three major cosmographical works. In the final version, in his Tuḥfa, the mean ecliptic is defined by an eccentric of fixed mean eccentricity and a mean obliquity fixed with respect to the celestial equator, and the center of the epicycle, which is inclined to the eccentric, moves on the eccentric with an annual period. By an additional slow motion of the sun on the epicycle, the true eccentricity of the solar deferent, defined by the annual motion of the sun, and the sun's extreme declination from the equator change, accounting for the reduction of the eccentricity and the obliquity of the ecliptic since the time of Ptolemy. |
| Author | Mozaffari, S. Mohammad |
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| Cites_doi | 10.2143/JA.297.1.2045781 10.1177/002182869502600202 10.1111/j.1600-0498.1969.tb00135.x 10.1086/350114 10.1007/978-1-4612-5559-8 10.1086/350144 10.1086/349635 10.1086/348774 10.1007/BF00343531 10.1142/3807 10.1111/j.1600-0498.1969.tb00146.x 10.1177/002182869402500302 10.1007/s00407-013-0130-4 10.2143/SI.36.2.2024100 10.1007/s00407-015-0153-0 10.1007/978-1-4613-8262-1 10.1111/j.1600-0498.1989.tb00851.x 10.1080/00033790802364429 10.1017/S0957423900001661 10.1016/j.hm.2013.04.001 10.1086/348609 10.1111/j.1600-0498.1971.tb00156.x 10.1023/A:1014994811867 10.2307/1006040 10.1007/s004070050008 10.1007/s00407-003-0072-3 10.2143/JA.292.1.556640 10.1007/978-3-642-61910-6 10.1111/j.1600-0498.1965.tb00625.x 10.1177/002182869802900201 10.1017/S095742390000151X 10.1017/S0957423912000070 10.1007/978-0-387-30400-7 10.1525/9780520312890-006 10.1177/002182868601700202 10.5962/bhl.title.19835 10.1017/S0269889701000072 10.2307/1005726 10.1515/9780691213361 10.1007/1-4020-3048-7_3 |
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| Snippet | This paper analyses a kinematic model for the solar motion by Quṭb al-Dīn al-Shīrāzī, a thirteenth-century Iranian astronomer at the Marāgha observatory in... |
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| StartPage | 267 |
| SubjectTerms | Astronomy Axial tilt Declination Eccentric behavior Ecliptic coordinate system History and Philosophical Foundations of Physics History of Mathematical Sciences History of Science Mathematics Mathematics and Statistics Obliquity of ecliptic Observational astronomy Observations and Techniques Philosophy of Science Precession Sun Venus |
| Title | A forgotten solar model |
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