View source for On the Sizes and Distances (Aristarchus)

{{short description|Work by Aristarchus of Samos, Greek astronomer}}
{{for|the work by Hipparchus|On Sizes and Distances (Hipparchus)}}
{{italic title}}
[[File:Aristarchus working.jpg|thumb|right|[[Aristarchus of Samos|Aristarchus's]] 3rd century BCE calculations on the relative sizes of, from left, the Sun, Earth and Moon, from a 10th-century CE Greek copy]]

'''''On the Sizes and Distances (of the Sun and Moon)''''' ({{langx|grc|Περὶ μεγεθῶν καὶ ἀποστημάτων [ἡλίου καὶ σελήνης]|{{grc-transl|Περὶ μεγεθῶν καὶ ἀποστημάτων [ἡλίου καὶ σελήνης]}}|}}) is widely accepted as the only extant work written by [[Aristarchus of Samos]], an [[ancient Greek astronomy|ancient Greek astronomer]] who lived circa 310–230 BCE. This work calculates the sizes of the [[Sun]] and [[Moon]], as well as their distances from the [[Earth]] in terms of Earth's radius.

The book was presumably preserved by students of [[Pappus of Alexandria]]'s course in mathematics, although there is no evidence of this. The ''[[editio princeps]]'' was published by [[John Wallis]] in 1688, using several medieval manuscripts compiled by Sir [[Henry Savile (Bible translator)|Henry Savile]].<ref>{{cite book|last1=Heath|first1=Thomas|title=Aristarchus of Samos, the Ancient Copernicus|date=1913|author-link=Thomas Little Heath|url=https://archive.org/details/aristarchusofsam00heat|publisher=Clarendon|location=Oxford|page=[https://archive.org/stream/aristarchusofsam00heat#page/323/mode/1up 323]}}</ref> The earliest Latin translation was made by [[Giorgio Valla]] in 1488. There is also a [https://www.loc.gov/resource/rbctos.2017gen18687 1572 Latin translation and commentary] by [[Frederico Commandino]].<ref>Berggren and Sidoli. 2007. 'Aristarchus's On the Sizes and Distances of the Sun and the Moon: Greek and Arabic Texts'. Arch. Hist. Exact Sci. 61(3), pp. 213–54. {{doi|10.1007/s00407-006-0118-4}}</ref><ref>Noack B. (1992) Aristarch von Samos: Untersuchungen zur Überlieferungsgeschichte der Schrif ''Περὶ μεγεθῶν καὶ ἀποστημάτων ἡλίου καὶ σελήνης'', Wiesbaden.</ref>

==Symbols==
The work's method relied on several observations:
* The apparent size of the Sun and the Moon in the sky.
* The size of the Earth's shadow in relation to the Moon during a [[lunar eclipse]]
* The angle between the Sun and Moon during a [[Lunar phase|half moon]] is 90°.

The rest of the article details a reconstruction of Aristarchus' method and results.<ref>[https://www.youtube.com/watch?v=LXHxx8L9YFo A video on reconstruction of Aristarchus' method] (in Turkish, no subtitles)</ref>  The reconstruction uses the following variables:
{| class="wikitable"
!Symbol!!Meaning
|-
|align = "center"|''φ''||Angle between the Moon and the Sun during a half moon (directly measurable)
|-
|align = "center"|''L''||Distance from the Earth to the [[Moon]]
|-
|align = "center"|''S''||Distance from the Earth to the [[Sun]]
|-
|align = "center"|''ℓ''||Radius of the [[Moon]]
|-
|align = "center"|''s''||Radius of the [[Sun]]
|-
|align = "center"|''t''||Radius of the [[Earth]]
|-
|align = "center"|''D''||Distance from the center of Earth to the vertex of Earth's shadow cone
|-
|align = "center"|''d''||Radius of the Earth's shadow at the location of the Moon
|-
|align = "center"|''n''||Ratio, ''d/ℓ'' (a directly observable quantity during a [[lunar eclipse]])
|-
|align = "center"|''x''||Ratio, ''S/L'' = ''s/ℓ'' (which is calculated from ''φ'')
|}

==Half Moon==
Aristarchus began with the premise that, during a [[Lunar phase|half moon]], the moon forms a [[right triangle]] with the Sun and Earth. By observing the angle between the Sun and Moon, ''φ'', the ratio of the distances to the Sun and Moon could be deduced using a form of [[trigonometry]].

[[Image:AristarchusHalfLitMoon2.png]]

From the diagram and trigonometry, we can calculate that

: <math> \frac{S}{L} = \frac{1}{\cos \varphi} = \sec \varphi. </math>

The diagram is greatly exaggerated, because in reality, ''S = 390 L'', and ''φ'' is extremely close to 90°. Aristarchus determined ''φ'' to be a thirtieth of a quadrant (in modern terms, 3°) less than a right angle: in current terminology, 87°. Trigonometric functions had not yet been invented, but using geometrical analysis in the style of [[Euclid]], Aristarchus determined that

: <math>18 < \frac{S}{L} < 20.</math>

In other words, the distance to the Sun was somewhere between 18 and 20 times greater than the distance to the Moon. This value (or values close to it) was accepted by astronomers for the next two thousand years, until the invention of the telescope permitted a more precise estimate of [[solar parallax]].

Aristarchus also reasoned that as the [[angular size]] of the Sun and the Moon were the same, but the distance to the Sun was between 18 and 20 times further than the Moon, the Sun must therefore be 18–20 times larger.

==Lunar eclipse==
Aristarchus then used another construction based on a lunar eclipse:

[[Image:AristarchusLunar Eclipse2.png|600px]]

By similarity of the triangles, <math> \frac{D}{L} = \frac{t}{t-d} \quad </math>   and   <math>\quad \frac{D}{S} = \frac{t}{s-t}.</math>

Dividing these two equations and using the observation that the Sun and Moon appear the same size to people on Earth, <math>s/S = \ell/L</math>, yields

:<math>
\frac{\ell}{s} = \frac{t-d}{s-t} \ \ \implies \ \ 
\frac{s-t}{s} = \frac{t-d}{\ell}  \ \ \implies \ \ 
\frac{t}{\ell} + \frac{t}{s} = 1 + \frac{d}{\ell}.
</math>

The rightmost equation can either be solved for <math>\ell/t</math> or <math>s/t</math>

:<math>
\frac{\ell}{t} = \frac{1+\dfrac{\ell}{s}}{1 + \dfrac{d}{\ell}},\qquad
\frac{s}{t} = \frac{1+\dfrac{s}{\ell}}{1 + \dfrac{d}{\ell}}.
</math>

These equations can be made to appear simpler by expressing the lengths <math>d</math> and <math>s</math> in terms of the moon's radius <math>\ell</math> as a unit, defining <math>\hat{d} = d/\ell</math> and <math>\hat{s} = s/\ell.</math> Then

: <math>
\frac{\ell}{t} = \frac{1+\hat{s}}{\hat{s}(1+\hat{d})},\qquad
\frac{s}{t} = \frac{1+\hat{s}}{1+\hat{d}}</math>

The above equations give the radii of the Moon and Sun entirely in terms of observable quantities.

The following formulae give the distances to the Sun and Moon in terrestrial units:

: <math> \frac{L}{t} = \left( \frac{\ell}{t} \right) \left( \frac{180}{\pi \theta} \right) </math>

: <math> \frac{S}{t} = \biggl( \frac{s}{t} \biggr) \left( \frac{180}{\pi \theta} \right) </math>

where ''θ'' is the apparent radius of the Moon and Sun measured in degrees.

Aristarchus did not use these exact formulae, yet these formulae are likely a good approximation for those of Aristarchus.

==Results==
The above formulae can be used to reconstruct the results of Aristarchus.  The following table shows the results of a long-standing (but dubious) reconstruction using ''n'' = 2, ''x'' = 19.1 (''φ'' = 87°) and ''θ'' = 1°, alongside the modern day accepted values.

{| class="wikitable"
!Qu|Quantity||Relation||Reconstruction||Modern
|-align = "center"
|''s/t''||Sun's radius in Earth radii||6.7||109
|-align = "center"
|''t/ℓ''||Earth's radius in Moon radii||2.85||3.67
|-align = "center"
|''L/t''||Earth-Moon distance in Earth radii||20||60.34
|-align = "center"
|''S/t''||Earth-Sun distance in Earth radii||380||23481
|}{{citation needed|reason = needs credible references for modern values|date=February 2016}}

The error in this calculation comes primarily from the poor values for ''x'' and ''θ''. The poor value for ''θ'' is especially surprising, since [[Archimedes]] writes that Aristarchus was the first to determine that the Sun and Moon had an apparent diameter of half a degree. This would give a value of ''θ'' = 0.25, and a corresponding distance to the Moon of 80 Earth radii, a much better estimate. The disagreement of the work with Archimedes seems to be due to its taking an Aristarchus statement that the lunisolar diameter is 1/15 of a "meros" of the zodiac to mean 1/15 of a zodiacal sign (30°), unaware that the Greek word "meros" meant either "portion" or 7°1/2; and 1/15 of the latter amount is 1°/2, in agreement with Archimedes' testimony.

A [[Hipparchus On Sizes and Distances|similar procedure]] was later used by [[Hipparchus]], who estimated the mean distance to the Moon as 67 Earth radii, and [[Ptolemy]], who took 59 Earth radii for this value.

==Illustrations==
Some interactive illustrations of the propositions in ''On Sizes'' can be found here:
* [https://www.geogebra.org/m/ZYFQqZa5 '''Hypothesis 4'''] states that when the Moon appears to us halved, its distance from the Sun is then less than a quadrant by one-thirtieth of a quadrant [that is, it is less than 90° by 1/30th of 90° or 3°, and is therefore equal to 87°] (Heath 1913:353).
* [https://www.geogebra.org/m/BcVB8g23 '''Proposition 1'''] states that two equal spheres are comprehended by one and the same cylinder, and two unequal spheres by one and the same cone which has its vertex in the direction of the lesser sphere; and the straight line drawn through the centres of the spheres is at right angles to each of the circles in which the surface of the cylinder, or of the cone, touches the spheres (Heath 1913:354).
* [https://www.geogebra.org/m/EsGKE5yA '''Proposition 2'''] states that if a sphere be illuminated by a sphere greater than itself, the illuminated portion of the former sphere will be greater than a hemisphere (Heath 1913:358).
* [https://www.geogebra.org/m/YEJ8GyaR '''Proposition 3'''] states that the circle in the Moon which divides the dark and the bright portions is least when the cone comprehending both the Sun and the Moon has its vertex at our eye (Heath 1913:362).
* [https://www.geogebra.org/m/dxJPXypp '''Proposition 4'''] states that the circle which divides the dark and the bright portions in the Moon is not perceptibly different from a great circle in the Moon (Heath 1913:365).
* [https://www.geogebra.org/m/MYdPsEku '''Proposition 6'''] states that the Moon moves [in an orbit] lower than [that of] the Sun, and, when it is halved, is distant less than a quadrant from the Sun (Heath 1913:372).
* [https://www.geogebra.org/m/u4EKJ5uQ '''Proposition 7'''] states that the distance of the Sun from the Earth is greater than 18 times, but less than 20 times, the distance of the Moon from the Earth (Heath 1913:377). In other words, the Sun is 18 to 20 times farther away and wider than the Moon.
* [https://www.geogebra.org/m/rDNQhNx9 '''Proposition 13'''] states that the straight line subtending the portion intercepted within the earth's shadow of the circumference of the circle in which the extremities of the diameter of the circle dividing the dark and the bright portions in the Moon move is less than double of the diameter of the Moon, but has to it a ratio greater than that which 88 has to 45; and it is less than 1/9th part of the diameter of the Sun, but has to it a ratio greater than that which 21 has to 225. But it has to the straight line drawn from the centre of the Sun at right angles to the axis and meeting the sides of the cone a ratio greater than that which 979 has to 10 125 (Heath 1913:394).
* [https://www.geogebra.org/m/nCqsrFSQ '''Proposition 14'''] states that the straight line joined from the centre of the Earth to the centre of the Moon has to the straight line cut off from the axis towards the centre of the Moon by the straight line subtending the [circumference] within the Earth's shadow a ratio greater than that which 675 has to 1 (Heath 1913:400).
* [https://www.geogebra.org/m/eChNpgEj '''Proposition 15'''] states that the diameter of the Sun has to the diameter of the Earth a ratio greater than 19/3, but less than 43/6 (Heath 1913:403). This means that the Sun is (a mean of) {{frac|6|3|4}} times wider than the Earth, or that the Sun is {{frac|13|1|2}} Earth-radii wide. The Moon and Sun must then be {{frac|20|1|4}} and 387 Earth-radii away from us in order to subtend an angular size of 2º.
* [https://www.geogebra.org/m/GrQBA2pf '''Proposition 17a'''] in al-Tusi's medieval Arabic version of the book ''On Sizes'' states that the ratio of the distance of the vertex of the shadow cone from the center of the Moon (when the Moon is on the axis [that is, at the middle of an eclipse] of the cone containing the Earth and the Sun) to the distance of the center of the Moon from the center of the Earth is greater than the ratio 71 to 37 and less than the ratio 3 to one (Berggren & Sidoli 2007:218).<ref name=Berggren>Berggren, J. L. & N. Sidoli (2007) {{cite web |url=http://individual.utoronto.ca/acephalous/Berggren_Sidoli_2007a.pdf |title='Aristarchus's On the Sizes and Distances of the Sun and the Moon: Greek and Arabic Texts', ''Archive for History of Exact Sciences,'' Vol. 61, no. 3, 213–254 |access-date=2011-11-07 |url-status=bot: unknown |archive-url=https://web.archive.org/web/20110428064826/http://individual.utoronto.ca/acephalous/Berggren_Sidoli_2007a.pdf |archive-date=April 28, 2011 }}.</ref> In other words, that the tip of the Earth's shadow cone is between 108/37 and four times farther away than the Moon.

==Known copies==
* Library of Congress Vatican Exhibit.

== See also ==

* [[Aristarchus of Samos]]
* [[Eratosthenes]] ({{circa|276|194/195&nbsp;BC|lk=on}}), a Greek mathematician who [[On the measure of the Earth|calculated]] the circumference of the Earth and also the distance from the Earth to the Sun.
* [[Hipparchus]] ({{circa|190|120&nbsp;BC|lk=on}}), a Greek mathematician who [[On Sizes and Distances (Hipparchus)|measured]] the radii of the Sun and the Moon as well as their distances from the Earth.
* [[On Sizes and Distances (Hipparchus)|''On the Sizes and Distances'' (Hipparchus)]]
* [[Posidonius]] ({{circa|135|51&nbsp;BC|lk=on}}), a Greek astronomer and mathematician who [[Posidonius#Calculation of Earth's circumference|calculated]] the circumference of the Earth.

== Notes ==
{{reflist}}

==Bibliography==
* {{cite book|last=Gomez |first=Alberto |title=Decoding Aristarchus |publisher=[[Peter Lang Verlag]] |location=[[Berlin]] |date=2023|isbn=9783631892619 |url=https://www.peterlang.com/document/1288830}}
*{{cite book|last1=Heath|first1=Thomas|title=Aristarchus of Samos, the Ancient Copernicus|date=1913|author-link=Thomas Little Heath|url=https://archive.org/details/aristarchusofsam00heat|publisher=Clarendon|location=Oxford}}  This was later reprinted, see ({{ISBN|0-486-43886-4}}).
* van Helden, A. ''Measuring the Universe: Cosmic Dimensions from Aristarchus to Halley''.  Chicago: Univ. of Chicago Pr., 1985. {{ISBN|0-226-84882-5}}.

{{Greek astronomy}}
{{Greek mathematics}}

[[Category:Ancient Greek astronomical works]]
[[Category:Astronomy books]]