Difference between revisions 4794929 and 4794931 on mswiki

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[[Fail:2064 aryabhata-crp.jpg|thumb|300px|Arca Aryabhata di tapak [[Inter-University Centre for Astronomy and Astrophysics|IUCAA]], [[Pune]]. Dengan tiadanya maklumat diketahui mengenai rupawannya, apa-apa imej Aryabhata berasal dari konsepsi artis.]]
(contracted; show full)Astronomy and History: Selected Essays,'' New York: Springer-Verlag, 1983, pp. 129–156. ISBN 0-387-90844-7</ref> Another element in Aryabhata's model, the ''śīghrocca'', the basic planetary period in relation to the Sun, is seen by some historians as a sign of an underlying [[heliocentric]] model.<ref>Hugh Thurston, ''Early Astronomy,'' New York: Springer-Verlag, 1996, pp. 178–189. ISBN 0-387-94822-8</ref>

=== Gerhana ===

Aryabhata 
states that the [[Moomenyatakan bahawa [[Bulan]] dand planets shine by reflected sunlight. Instead of the prevailing cosmogony in which eclipses were caused by pseudo-planetary nodes bersinar oleh cahaya matahari yang dipantulkan. Daripada kosmogoni yang berlaku di mana gerhana disebabkan oleh node planet-planet pseudo [[Rahu]] dand [[Ketu]], he explains eclipses idia menjelaskan tgerms of shadows cast by and falling on Earth. Thus, the lunar eclipse occurs when the moon enters into the Earth's shadow (verse gola.37). He discusses at length the size and extent of the Earth's shadow (verseshana dari segi bayang-bayang yang dilemparkan dan jatuh di Bumi. Oleh itu, gerhana bulan berlaku ketika bulan memasuki bayangan Bumi (ayat gola.37). Dia membincangkan panjang lebar tentang ukuran dan luas bayangan Bumi (ayat gola.38–48) dand then provides the computation and the size of the eclipsed part during an eclipse. Later Indian astronomers improved on the calculations, but kemudian memberikan pengiraan dan ukuran bahagian yang gerhana semasa gerhana. Kemudian ahli astronomi India meningkatkan perhitungan, tetapi kaedah Aryabhata's methods provided the core. His computational paradigm was so accurate that 18th century scientist [[Guillaume Le Gentil]], during a visit to Pondicherry, India, found the Indian computations of the duration of the [[lunar eclipse]] of [[1765-08-30]] to be short by 41 seconds, whereas his charts (by Tobias Mayer, 1752) were long by 68 seconds.<ref name=Ansari/>

Aryabhata's computation of the Earth's [[circumference]] as 39,968.0582 kilometres was only 0.2% smaller than the actual value of 40,075.0167 kilometres. This approximation was a significant improvement over the computation by [[Greek mathematics|Greek mathematician]] [[Eratosthenes]] (c. 200 BCE), whose exact computation is not known in modern units but his estimate had an error of around 5–10%.<ref>[http://www.nasa.gov/lb/audience/forstudents/5-8/features/F_JSC_NES_School_Measures_Up.html "JSC NES School Measures Up"], ''NASA'', 11th April, 2006, retrieved 24th January, 2008.</ref><ref>[http://www-istp.gsfc.nasa.gov/stargaze/Scolumb.htm "The Round Earth"], ''NASA'', 12th December, 2004, retrieved 24th Januarymberikan intinya. Paradigma komputasinya begitu tepat sehingga saintis abad ke-18 [[Guillaume Le Gentil]], semasa lawatan ke Pondicherry, India, menemui pengiraan India mengenai tempoh [[gerhana bulan]] [[1765-08-30] ] menjadi pendek 41 saat, sedangkan carta (oleh Tobias Mayer, 1752) panjang 68 saat.<ref name=Ansari/>

Pengiraan Aryabhata terhadap [[lilitan]] Bumi sejauh 39.968.0582 kilometer hanya 0.2% lebih kecil daripada nilai sebenar 40.075.0167 kilometer. Pendekatan ini merupakan peningkatan yang ketara berbanding pengiraan oleh [[Matematik Yunani|ahli matematik Yunani]] [[Eratosthenes]] (sekitar 200 SM), yang mana pengiraannya tidak diketahui dalam unit moden tetapi anggarannya mempunyai kesalahan sekitar 5– 10%.<ref>[http://www.nasa.gov/lb/audience/forstudents/5-8/features/F_JSC_NES_School_Measures_Up.html "JSC NES School Measures Up"], ''NASA'', 11th April, 2006, retrieved 24th January, 2008.</ref><ref>[http://www-istp.gsfc.nasa.gov/stargaze/Scolumb.htm "The Round Earth"], ''NASA'', 12 Disember, 2004, diperolehi 24 Januari, 2008.</ref>

=== Tempoh sidereal ===

Dipertimbangkan dalam unit masa Inggeris moden, Aryabhata mengira [[putaran sisi]] (putaran bumi merujuk bintang tetap) sebagai 23 jam, 56 minit, dan 4.1 saat; nilai moden ialah 23: 56: 4.091. Begitu juga, nilainya untuk [[sidereal year]] pada 365 hari, 6 jam, 12 minit, dan 30 saat adalah kesalahan 3 minit dan 20 saat sepanjang satu tahun. Pengertian waktu sidereal diketahui di kebanyakan sistem astronomi lain pada masa itu, tetapi pengiraan ini mungkin yang pal(contracted; show full)
[[Kategori:Kelahiran 476]]
[[Kategori:Kematian 550]]
[[Kategori:Ahli matematik abad ke-5]]
[[Kategori:Ahli matematik abad ke-6]]
[[Kategori:Ahli astronomi India]]
[[Kategori:Ahli matematik India silam]]
[[Kategori:Ahli astronomi zaman pertengahan]]