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Re: Chernaya dyra
13.10.2013 20:19 | A.P. Vasi

Repetition of the Leyden measurements

Povtorenie leidenskih izmerenii

Courvoisiers device for measuring the absolute speed of the earth

Ustroistvo Kurvuaz'e dlya izmereniya absolyutnoi skorosti Zemli

The double mirror experiments

Eksperimenty s dvoinymi zerkalami

The second method: Lorentz contraction

Vtoroi sposob: sokrashenie Lorenca

Comparison between measurements from different places

Sravnenie izmerenii, sdelannyh v raznyh mestah

Nadir observations

Nablyudeniya nadira

Other methods

Drugie metody

Plumb line motion

Dvizhenie linii otvesa

Bubble level

Puzyr'kovyi uroven'

Comparison between pendulum clocks at different places

Sravnenie mayatnikovyh chasov v raznyh mestah

Local comparison between pendulum clock and chronometer

Mestnoe sravnenie mayatnikovyh chasov i hronometrov

Gravimetric observations

Gravimetricheskie nablyudeniya

Eclipses of Jupiters satellites

Zatmeniya sputnikov Yupitera

Secular aberration of light

Vekovye aberracii sveta

Final comments

Zaklyuchitel'nye kommentarii

177
178	The Leyden measurements had used four stars close to the North Pole.	Pri izmereniyah v Leidene ispol'zovalis' chetyre zvezdy, blizkie k Severnomu polyusu.
179	The difference zz' was measured in a series of observations, at the times of upper and lower culmination of each star.	Raznica zz′ byla izmerena v serii nablyudenii v momenty verhnei i nizhnei kul'minacii kazhdoi zvezdy.
180	The observed values of the periodical components of zz' amounted to less than 1'', varying from 0.04'' for one of the stars to about 0.5″ for another.	Nablyudaemye znacheniya periodicheskih komponent zz′ sostavili menee 1″, s variaciei ot 0,04″ dlya odnoi iz zvezd do 0,5″ dlya drugoi.
181	The error of the measurements was estimated as 0.01″, therefore the effect was regarded as significant.	Pogreshnost' izmerenii byla ocenena kak 0,01″, poetomu effekt rascenen kak znachimyi.
182	From the Leyden data Courvoisier obtained the results:	Iz Leidenskih dannyh Kurvuaz'e byli polucheny rezul'taty:
183	A = 104 21; D = +39 27; v = 810 215 km/s	A = 104 21; D = +39 27; v = 810 215 km/s
184	{14} The estimated error of the speed amounted to about 25%.	Ocenivaemaya oshibka skorosti sostavila okolo 25%.
185	The errors of the right ascension and declination amounted to about 1/15 of the full circle.	Oshibki pryamogo voshozhdeniya i skloneniya sostavili okolo 1/15 polnogo kruga.
186	Between 1921 and 1922 Courvoisier repeated the Leyden measurements, but with a slight change of method.	Mezhdu 1921 i 1922 gg. Kurvuaz'e povtoril leidenskie izmereniya, no s nebol'shim izmeneniem metoda.
187	Instead of a meridian circle he used a Wanschaff vertical circle that enabled him to make measurements of the stars at any time during the night.	Vmesto meridiannogo kruga on ispol'zoval vertikal'nyi krug Vanshaffa, kotoryi pozvolil emu proizvesti izmereniya zvezd v lyuboe vremya v techenie nochi.
188	Therefore his measurements were not limited to two sidereal times for each star.	Poetomu ego izmereniya ne byli ogranicheny dvumya momentami zvezdnogo vremeni dlya kazhdoi zvezdy.
189
190	From 4 June to 14 December 1921 he made a series of 142 measurements of the polar star BD +89.3, and from 18 March to 23 May 1922 he made further 64 determinations of zz'.	S 4 iyunya po 14 dekabrya 1921 godu on proizvel seriyu iz 142 izmerenii Polyarnoi zvezdy BD 89,3 , a s 18 marta po 23 maya 1922 g. on vypolnil dal'neishie 64 opredeleniya zz′.
191	From those measurements Courvoisier obtained:	Iz etih izmerenii Kurvuaz'e poluchil:
192	A = 93 7; D = +27 12; v = 652 71 km/s	A = 93 7; D = +27 12; v = 652 71 km/s
193	The estimated relative error of the speed was reduced to about 10% and the errors of the right ascension and declination amounted to less than 1/30 of the full circle.	Raschetnaya otnositel'naya oshibka opredeleniya skorosti snizilas' do okolo 10%, a oshibki opredeleniya pryamogo voshozhdeniya i skloneniya sostavili menee chem 1/30 polnogo kruga.
194	Courvoisiers work called the attention of a French astronomer, the director of the Strasbourg observatory, Ernest Esclangon, who repeated those measurements.18	Rabota Kurvuaz'e obratila na sebya vnimanie francuzskogo astronoma, direktora Strasburgskoi observatorii, Ernesta Esklangona, kotoryi povtoril eti izmereniya. 18
195	He confirmed the existence of a systematic effect of the same order of magnitude, and computed the values of A=69 and D=44.	On podtverdil sushestvovanie sistematicheskogo effekta togo zhe poryadka velichiny, i vychislil znacheniya A=69 i D=44.
196	Esclangon did not publish the estimated errors of his evaluation, nor the estimated speed of the Earth.	Esklangon ne opublikoval ni raschetnye oshibki ego ocenki, ni ozhidaemuyu skorost' Zemli.
197
198	Other evaluations were later obtained by Courvoisier using measurements made at München (19301931) and Breslau (19331935), with the following results:	Drugie dannye byli pozdnee polucheny Kurvuaz'e s ispol'zovaniem izmerenii, provedennyh v Myunhene (1930-1931) i Breslavle (1933-1935), so sleduyushimi rezul'tatami:
199	München Breslau (1) Breslau (2) A = 73 6 A = 92 12 A = 80 4 D = +40 (estimated)19 D = +44 25 D = +30 10 v = 889 93 km/s v = 927 200 km/s v = 700 60 km/s	Myunhen Breslavl' (1) Breslavl' (2) A = 73 6 A = 92 12 A = 80 4 D = +40 (ocenka) 19 D = +44 25 D = +30 10 V = 889 93 km / s V = 927 200 km / s V = 700 60 km / s
200	The results obtained in the second Breslau series presented the smallest errors.	Rezul'taty, poluchennye vo vtoroi serii Breslavlya, predstavleny naimen'shimi oshibkami.
201
202	In 1945, after his retirement, Courvoisier made a final series of observations from Basel.	V 1945 godu, posle vyhoda na pensiyu, Kurvuaz'e vypolnil okonchatel'nye serii nablyudenii v Bazele.
203	He obtained the following results:	On poluchil sleduyushie rezul'taty:
204	A = 60 14; D = +40 (estimated); v = 656 157 km/s	A = 60 14 , D = +40 (ocenka), v = 656 157 km / s
205	{15} If we compare all the series of measurements, we notice that the right ascension varied between 60 and 104 (more than the estimated errors); the declination varied between 39 and 44 (within the estimated errors);20 and the speed varied between 652 and 927 km/s (within estimated errors).	Esli sravnit' vse serii izmerenii, my zamechaem, chto pryamoe voshozhdenie var'irovalas' mezhdu 60 i 104 (bolee chem raschetnaya oshibka); sklonenie ot 39 do 44 (v predelah raschetnyh oshibok), 20 i skorost' ot 652 do 927 km / s (v predelah raschetnyh oshibok).
206	Notice that it is very hard to explain away Courvoisier's results as due to instrument errors, because the observed effect varied with periods of one sidereal day and half sidereal day.	Obratite vnimanie, chto ochen' trudno ob'yasnit' rezul'taty Kurvuaz'e instrumental'nymi pogreshnostyami, tak kak nablyudaemyi effekt izmenyaetsya s periodami v odni zvezdnye sutki i polovinu zvezdnyh sutok.
207	All common causes of error (gravity changes, temperature changes, etc.) would vary with periods of one (or half) solar day.	Vse rasprostranennye prichiny oshibok (izmeneniya sily tyazhesti, izmeneniya temperatury i t.d.) dolzhny menyat'sya s periodom v odni (ili polovinu) solnechnyh sutok.
208	Tidal influences due to the Moon would have periods that could also be easily distinguished from the effects predicted by Courvoisier.	Prilivnye vliyaniya Luny budut imet' periody, kotorye takzhe mogut byt' legko otlichimy ot effektov, predskazannyh Kurvuaz'e.
209	Besides that, the data used by Courvoisier was obtained with different instruments at different places, and covered a time span of 80 years.	Krome togo, dannye, ispol'zuemye Kurvuaz'e, byli polucheny s pomosh'yu razlichnyh instrumentov v raznyh mestah, i ohvatyvali promezhutok vremeni v 80 let.
210	The results presented by Courvoisier are therefore highly impressive and cannot be dismissed lightly.	Rezul'taty, predstavlennye Kurvuaz'e, sledovatel'no, ves'ma vpechatlyaet i ne mogut byt' legko otvergnuty.
211
212
213	In the first method used by Courvoisier, the stars work as mere point-like light sources.	V pervom metode, kotoryi ispol'zoval Kurvuaz'e, zvezdy ispol'zuyutsya kak prostye tochechnye istochniki sveta.
214	There is nothing peculiarly astronomical in the observed effect because, according to Courvoisier's theory, this was ascribed to the principle of the moving mirror.	Tam net nichego specificheski astronomicheskogo v nablyudaemom effekte, potomu chto, soglasno teorii Kurvuaz'e, eto bylo opisano kak princip dvizhushegosya zerkala.
215	Therefore, similar effects should occur for terrestrial light sources, too.	Takim obrazom, podobnye effekty dolzhny takzhe voznikat' i dlya nazemnyh istochnikov sveta.
216
217	Accordingly, Courvoisier was led to build a new instrument: an optical device for measuring absolute motion (.... 6).21 He used two small telescopes that were placed in an underground room where the temperature was fairly constant.	Sootvetstvenno, Kurvuaz'e eto privelo k sozdaniyu novogo instrumenta:. opticheskogo ustroistva dlya izmereniya absolyutnogo dvizheniya (ris. 6) 21 On ispol'zoval dva nebol'shih teleskopa, kotorye byli razmesheny v podzemnom pomeshenii, gde temperatura byla dovol'no postoyannoi.
218	Both telescopes pointed obliquely (zenithal distance = 60) to a mercury mirror that was placed between them.	Oba teleskopa byli nakloneny (zenitnoe rasstoyanie = 60 ) k rtutnomu zerkalu, kotoroe bylo pomesheno mezhdu nimi.
219	They were mounted in a vertical plane in the East-West direction.	Oni byli ustanovleny v vertikal'noi ploskosti v napravlenii Vostok-Zapad.
220	One of the telescopes had a small electric light close to its reticule, and this was the light source that was observed from the second telescope.	Odin iz teleskopov imel nebol'shoe elektricheskoe osveshenie vblizi ot ee kresta vizirnyh nitei, i eto bylo istochnikom sveta, kotoryi nablyudalsya vo vtoroi teleskop.
221	Both telescopes were first adjusted so that it was possible to see the reflection of the illuminated reticule of the first telescope from the second telescope.	Oba teleskopa snachala byli nastroeny takim obrazom, chtoby mozhno bylo uvidet' otrazhenie osveshennoi setki iz pervoi truby ot vtorogo teleskopa.
222	They were then fastened in those directions.	Zatem oni byli zakrepleny v etih napravleniyah.
223	Of course, the angles of the telescopes with the local vertical were sensibly equal.	Konechno, ugly teleskopov s mestnoi vertikali byli ochevidno ravny.
224	The experiment did not try to measure any difference between those angles.	Eksperiment ne pytalsya izmerit' kakoe-libo razlichie mezhdu etimi uglami.
225	It attempted to detect small periodical changes of the position of the image of the first telescope reticule as observed from the second one.	On byl prednaznachen dlya obnaruzheniya nebol'shih periodicheskih izmenenii v polozhenii kresta vizirnyh nitei pervogo teleskopa, pri ih nablyudenii iz vtorogo teleskopa.
226	The apparent motion of {16} the reticule was measured with the aid of the ocular micrometer of the second telescope.	Vidimoe dvizhenie perekrestiya bylo izmereno s pomosh'yu okulyarnogo mikrometra vtorogo teleskopa.
227
228	Using this device, Courvoisier made two series of observations in 1926 and 1927.	S pomosh'yu etogo ustroistva Kurvuaz'e vypolnil dve serii nablyudenii v 1926 i 1927 godah.
229	Afterwards, he had a special instrument built for this purpose, and made a third series of observations in 1932.	Vposledstvii, on postroil special'nyi instrument dlya etoi celi, i vypolnil tret'yu seriyu nablyudenii v 1932 godu.
230
231	In his first experiments the telescopes were placed in a vertical plane in the East-West direction.	V ego pervyh eksperimentah teleskopy byli razmesheny v vertikal'noi ploskosti v napravlenii vostok-zapad.
232	In 1926 and 1928 Courvoisier built two new instruments that could be rotated.	V 1926 i 1928 godah Kurvuaz'e postroil dva novyh instrumenta, kotorye mogli vrashat'sya.
233	He expected that this would improve his measurements.	On ozhidal, chto eto budet sposobstvovat' uluchsheniyu ego izmerenii.
234	However, he found out that it was impossible to compare measurements when the device was rotated, due to mechanical problems, and the instruments could only be effectively used in a fixed position.	Tem ne menee, on vyyasnil, chto okazalos' nevozmozhnym sravnivat' izmereniya, kogda ustroistvo povorachivalos', iz-za mehanicheskih problem, i instrumenty mogut byt' effektivno ispol'zovany tol'ko v fiksirovannom polozhenii.
235
236	The equation used to compute the effect was similar to that used in the case of the observation of stars, but instead of the North component of the speed, it was necessary to take into account the West component.	Uravnenie, ispol'zuemoe dlya vychisleniya effekta, byl analogichno tomu, kotoroe ispol'zovalos' v sluchae nablyudeniya zvezd, no vmesto severnoi komponenty skorosti, bylo neobhodimo prinimat' vo vnimanie zapadnuyu komponentu.
237	As in the former case, the resulting equation has a constant term plus variable components with periods of one sidereal day and half sidereal day.	Kak i v predydushem sluchae, rezul'tiruyushee uravnenie imeet postoyannyi chlen plyus peremennye sostavlyayushie s periodami v odni zvezdnye sutki i polovinu zvezdnyh sutok.