Тепловые и избыточные механические шумы в экспериментах с пробными телами (1097893), страница 5
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Íà åãî îñíîâå ñîçäàíà óñòàíîâêàäëÿ èññëåäîâàíèÿ ôëóêòóàöèé íàòÿæåíèÿ â êâàðöåâûõ íèòÿõ. Åå ÷óâñòâèòåëüíîñòü ê îòíîñèòåëüíûì âàðèàöèÿì íàòÿæåíèÿ ñîñòàâèëà δσmin /σ '√1 · 10−11 1/ Ãö â äèàïàçîíå ÷àñòîò îò 10 äî 100 êÃö äëÿ íèòåé òîëùèíîéîò 10 äî 200 ìêì.Ïðîâåäåííûå èçìåðåíèÿ ïîêàçàëè, ÷òî ñîáñòâåííûå ôëóêòóàöèè íàòÿæåíèÿ â êâàðöåâûõ íèòÿõ ïðè íàòÿæåíèÿõ äî 50% îò ðàçðûâíîãî ìåíüøåóêàçàííîãî óðîâíÿ.5.
Ñîçäàíà óñòàíîâêà äëÿ èññëåäîâàíèÿ ìåõàíè÷åñêèõ øóìîâ â ïðîòîòèïàõïîäâåñîâ çåðêàë äëÿ ãðàâèòàöèîííî-âîëíîâûõ àíòåíí âòîðîãî ïîêîëåíèÿ,ïðåäñòàâëÿþùèõ ñîáîé íèòè èç âûñîêî÷èñòîãî ïëàâëåíîãî êâàðöà ñ ìèíèàòþðíûì çåðêàëîì, ñìîíòèðîâàííûì â öåíòðå.Ðàçðàáîòàíà òåõíîëîãèÿ èçãîòîâëåíèÿ îáðàçöîâ, ïîçâîëÿþùàÿ ñîõðàíèòüêàê âûñîêóþ (Q ≥ 107 ) äîáðîòíîñòü ìåõàíè÷åñêèõ ìîä, òàê è áîëüøóþ îòðàæàþùóþ ñïîñîáíîñòü (1−R ≤ 10−2 ) çåðêàë. Ïðèìåíåíèå èíòåðôåðîìåò√ðà Ôàáðè-Ïåðî ïîçâîëèëî äîñòèãíóòü ÷óâñòâèòåëüíîñòè îò 1·10−12 ñì/ Ãö√âáëèçè ÷àñòîòû 700 Ãö äî 9 · 10−14 ñì/ Ãö âáëèçè ÷àñòîòû 2 êÃö, ÷òî ïîçâîëèëî ðåãèñòðèðîâàòü âàðèàöèè àìïëèòóäû òåïëîâûõ êîëåáàíèé ñ òî÷íîñòüþ ∼ 1% îò ñðåäíåêâàäðàòè÷íîé àìïëèòóäû ðàâíîâåñíûõ òåïëîâûõêîëåáàíèé.Ïðîâåäåí öèêë èññëåäîâàíèé ðàçëè÷íûõ ìîä êîëåáàíèé äëÿ êâàðöåâûõîáðàçöîâ ñ íèòÿìè äèàìåòðîì îò 50 äî 200 ìêì ïðè íàãðóçêàõ îò ∼ 4%28äî ∼ 50% îò ðàçðûâíîé îáùåé äëèòåëüíîñòüþ áîëåå 100 ÷àñîâ.
Âàðèàöèé,çíà÷èìî ïðåâûøàþùèõ ðàâíîâåñíûå òåïëîâûå, íå îáíàðóæåíî. Ýêñòðàïîëÿöèÿ ïîëó÷åííûõ ðåçóëüòàòîâ ïîçâîëÿåò óòâåðæäàòü, ÷òî èçáûòî÷íûéìåõàíè÷åñêèé øóì â ïîäâåñàõ çåðêàë ãðàâèòàöèîííûõ àíòåíí âòîðîãî ïîêîëåíèÿ íå áóäåò îãðàíè÷èâàòü èõ ïëàíèðóåìóþ ÷óâñòâèòåëüíîñòü.6. Èññëåäîâàíà çàâèñèìîñòü òàíãåíñà óãëà ìåõàíè÷åñêèõ ïîòåðü îò äèàìåòðàêâàðöåâûõ íèòåé äëÿ ìàÿòíèêîâîé, êðóòèëüíîé è ñòðóííûõ ìîä êîëåáàíèéìåõàíè÷åñêèõ îñöèëëÿòîðîâ â îáëàñòè çíà÷åíèé îò 1.5 äî 40 ìêì. Îáíàðóæåíî, ÷òî äëÿ íèòåé äèàìåòðîì ìåíåå 5 ìêì çàòóõàíèå ñ óìåíüøåíèåìäèàìåòðà ðàñòåò áûñòðåå, ÷åì ïðåäñêàçûâàåò ýêñòðàïîëÿöèÿ ðåçóëüòàòîâ,ïîëó÷åííûõ äëÿ êâàðöåâûõ íèòåé äèàìåòðîì áîëåå 40 ìêì. Äëÿ îñöèëëÿòîðîâ, ïðåäñòàâëÿþùèõ ñîáîé ãðóç, ïîäâåøåííûé íà êâàðöåâîé íèòèäèàìåòðîì â íåñêîëüêî ìèêðîí, âïåðâûå äîñòèãíóòû çíà÷åíèÿ äîáðîòíîñòè îñíîâíîé ñòðóííîé ìîäû êîëåáàíèé (9.2 ± 0.9) · 106 (äèàìåòð 2.5 ± 0.5ìêì) è ìàÿòíèêîâîé ìîäû (1.9 ± 0.2) · 107 (äèàìåòð 1.7 ± 0.2 ìêì).7.
Ðàçðàáîòàíà è ñîçäàíà óñòàíîâêà äëÿ äèàãíîñòèêè îïòè÷åñêèõ íåîäíîðîäíîñòåé â ìíîãîñëîéíûõ îòðàæàþùèõ äèýëåêòðè÷åñêèõ ïîêðûòèÿõ ñ ïðîñòðàíñòâåííûì ðàçðåøåíèåì ïîðÿäêà äëèíû âîëíû (1 ìêì), ïîçâîëÿþùàÿðåãèñòðèðîâàòü îòêëîíåíèÿ êîýôôèöèåíòîâ ïðîïóñêàíèÿ è ðàññåÿíèÿ âåëè÷èíîé ïîðÿäêà 0.5%. ñòðóêòóðàõ SiO2 /T a2 O5 îáíàðóæåíû íåîäíîðîäíîñòè ñ õàðàêòåðíûìèðàçìåðàìè îò 2 äî 50 ìêì, â êîòîðûõ îòëè÷èå êîýôôèöèåíòîâ ïðîïóñêàíèÿ è ðàññåÿíèÿ îò ñðåäíèõ çíà÷åíèé ñîñòàâëÿëî îò 1-2% äî 2-2.5 ðàç.Ïîëó÷åííûå äàííûå î ïëîòíîñòè è õàðàêòåðå íåîäíîðîäíîñòåé ïîçâîëÿþòñäåëàòü îöåíêè èõ âëèÿíèÿ íà ÷óâñòâèòåëüíîñòü ïðåöèçèîííûõ èçìåðèòåëüíûõ ñèñòåì, èñïîëüçóþùèõ ðåçîíàòîðû Ôàáðè-Ïåðî ñ äèýëåêòðè÷åñêèìè çåðêàëàìè, âêëþ÷àÿ èíòåðôåðîìåòðè÷åñêèå äåòåêòîðû ãðàâèòàöèîííûõ âîëí.29Îñíîâíûå ðåçóëüòàòû äèññåðòàöèîííîãî èññëåäîâàíèÿîïóáëèêîâàíû â ñëåäóþùèõ ðàáîòàõ:1.
Áèëåíêî È.À., Ìèòðîôàíîâ Â.Ï., Îõðèìåíêî Î.À. Óñòàíîâêà äëÿ èçìåðåíèÿ âðåìåíè çàòóõàíèÿ êîëåáàíèé â ìàÿòíèêàõ ñ ìàëîé äèññèïàöèåéýíåðãèè, ÏÒÝ, N5 ñ. 188-191, 1993.2. Bilenko I.A., Ivanov E.N., Tobar M.E. and Blair D.G., Sapphire high-Q lowtemperature transducer for resonant bar gravitational wave antennas, Phys.letters A v. 211, p. 139, 1996.3. Bilenko I.A., Braginsky V.B., Measurements of the excess noise in the test masssuspensions for the Gravitational Wave Antennas, in: '9th Marsel Grossmannmeeting on General Relativity and Gravitation', Jerusalem, 1997.4. Bilenko I.A. Ageev A.Yu., Braginsky V.B., Vyatchanin S.P., Measurement ofthe Excess Noise in the Suspension Fiber for the Gravitational Wave Detector,Phys. letters A, v.
227, p. 159 1997.5. Bilenko I.A. Ageev A.Yu., Braginsky V.B., Excess Noise in the Steel SuspensionWires for the Laser Gravitational Wave Detector, Phys. letters A, v. 246, p.479, 1998.6. Áèëåíêî È.À., Ãîðîäåöêèé Ì.Ë., Ìåòîä èçìåðåíèÿ ìàëûõ êîëåáàíèé îïòè÷åñêè ïðîçðà÷íûõ îáúåêòîâ, ÄÀÍ 368, 612, 1999.7. Bilenko I.A., Ilchenko V.S., Samoilenko A.A., The application of whisperinggallery mode microcavity on the measurement of internal strain uctuationsin optical bers, LASE 2002 Symposium, Photonics West, San Jose Jan 21-25,2002.8. Bilenko I.A., Lourie S.L., Measurements of eective noise temperature in fusedsilica ber violin modes, Phys.
Letters. A, v. 305, p. 31, 2002.9. Bilenko I.A., Ju L., Paget D. and Blair D.G., Niobium exure suspensiondesign for high Q sapphire test masses for future gravitational wave detectors,Meas. Sci. Technol. v. 13, p. 1173-1177, 2002.3010. Bilenko I.A., Braginsky V.B., Markova N.Yu., Thermal and excess noise insuspension bres, Class. Quantum Grav. v.
19, p. 2035, 2002.11. Áèëåíêî È.À., Ñàìîéëåíêî À.À., Ýôôåêò îïòè÷åñêîé æåñòêîñòè â ðåçîíàòîðå Ôàáðè-Ïåðî, Âåñòíèê Ìîñêîâñêîãî óí-òà, ñåð. 3: ôèçèêà è àñòðîíîìèÿ, N 4 c. 39, 2003.12. Bilenko I.A., Braginsky V.B., and Lourie S.L., Mechanical losses in thin fusedsilica bres. Class. Quantum Grav., v. 21, p. S1231, 2004.13. Abbott B., Abbott R., Adhikari R., Bilenko I.A. et al., Detector descriptionand performance for the rst coincidence observations between LIGO andGEO. Nucl. Instrum. and Methods in Phys. Research A, v. 517, p.
154-179,2004.14. Áèëåíêî È.À., Ëÿñêîâñêàÿ Í.Þ. Äàò÷èê ìàëûõ ñìåùåíèé íà îñíîâå ðåçîíàòîðà Ôàáðè-Ïåðî äëÿ èññëåäîâàíèÿ ìåõàíè÷åñêèõ øóìîâ â ïðîòîòèïàõïîäâåñîâ çåðêàë ãðàâèòàöèîííûõ àíòåíí, Âåñòíèê Ìîñêîâñêîãî óí-òà, ñåð.3: ôèçèêà è àñòðîíîìèÿ, N. 3, c. 47-50, 2004.15. Áèëåíêî È.À., Ëóðüå Ñ.Ë. Èññëåäîâàíèå äèññèïàöèè â êðóòèëüíûõ ìîäàõîñöèëëÿòîðîâ íà òîíêèõ íèòÿõ èç ïëàâëåíîãî êâàðöà, Âåñòíèê Ìîñêîâñêîãî óí-òà, ñåð. 3: ôèçèêà è àñòðîíîìèÿ, N. 4, c. 68-70, 2004.16. Abbott B., Abbott R., Adhikari R., Bilenko I.A.
et al., First Upper Limitsfrom LIGO on GW Bursts Phys. Rev. D, v. 69, p. 102001, 2004.17. Abbott B., Abbott R., Adhikari R., Bilenko I.A. et al., Setting Upper Limits onthe Strength of Periodic GW from PSR J1939 + 2134 Using the First ScienceData from the GEO600 and LIGO Detectors, Phys. Rev. D, v. 69, p. 082004,2004.18.
Abbott B., Abbott R., Adhikari R., Bilenko I.A. et al., Upper Limits on aStochastic Background of Gravitational Waves, Phys. Rev. Lett. v. 95, p.221101, 2005.3119. Abbott B., Abbott R., Adhikari R., Bilenko I.A. et al., First All-sky UpperLimits from LIGO on the Strength of Periodic Gravitational Waves Using theHough Transform, Phys. Rev. D, v. 72, p. 102004, 2005.20. Abbott B., Abbott R., Adhikari R., Bilenko I.A. et al., Limits on GravitationalWave Emission from Selected Pulsars Using LIGO Data, Phys. Rev. Lett. v.94, p. 181103, 2005.21. Abbott B., Abbott R., Adhikari R., Bilenko I.A.
et al., Upper Limits fromLIGO and TAMA Detectors on the Rate of Gravitational Wave Bursts, Phys.Rev. D, v. 72, p. 122004, 2005.22. Abbott B., Abbott R., Adhikari R., Bilenko I.A. et al., Upper Limits onGravitational Wave Bursts in LIGO's Second Science Run, Phys. Rev. D, v.72, p. 062001, 2005.23. Bilenko I.A.,Lyaskovskaya N.Yu., The investigation of thermal and non-thermalnoises in fused silica bers for Advanced LIGO suspension, Phys. Letters A,v. 339, p. 181, 2005.24. Abbott B., Abbott R., Adhikari R., Bilenko I.A.
et al., Search for gravitationalwave bursts in LIGO's third science run, Class. and Quantum Grav., v. 23, p.S29-S39, 2006.25. Abbott B., Abbott R., Adhikari R., Bilenko I.A. et al., Search for gravitationalwaves from binary black hole inspirals in LIGO data, Phys. Rev. D, v. 73, p.062001, 2006.26. Abbott B., Abbott R., Adhikari R., Bilenko I.A. et al., Upper limit map of abackground of gravitational waves, Phys. Rev.
D, v. 76, 2007.27. Abbott B., Abbott R., Adhikari R., Bilenko I.A. et al., Search for gravitationalwave bursts in LIGO data from the fourth science run, Class. and QuantumGrav., v. 24 p. 5343-5369 2007.28. Abbott B., Abbott R., Adhikari R., Bilenko I.A. et al. Search for gravitationalwave radiation associated with the pulsating tail of the SGR 1806 20 hyperareof 27 December 2004 using LIGO, Phys. Rev.
D, v. 76, p. 062003, 2007.3229. Abbott B., Abbott R., Adhikari R., Bilenko I.A. et al. First cross-correlationanalysis of interferometric and resonant-bar gravitational-wave data for stochasticbackgrounds, Phys. Rev. D, v. 76, p. 022001, 2007.30. Abbott B., Abbott R., Adhikari R., Bilenko I.A. et al., Upper limits on gravitationalwave emission from 78 radio pulsars, Phys. Rev. D, v. 76, p. 042001, 2007.31. Abbott B., Abbott R., Adhikari R., Bilenko I.A. et al., Searching for a stochasticbackground of gravitational waves with the laser interferometer gravitationalwave observatory, Astrophysical Journal, v. 659, p.
918-930, 2007.32. Abbott B., Abbott R., Adhikari R., Bilenko I.A. et al., Beating the spindown limit on gravitational wave emission from the Crab pulsar, AstrophysicalJournal Letters, v. 683, p. L45-L49, Aug. 2008.33. Áèëåíêî È.À., Ãðîìîâà Å.Ñ., Èññëåäîâàíèå îïòè÷åñêèõ íåîäíîðîäíîñòåéìíîãîñëîéíûõ îòðàæàþùèõ ïîêðûòèé ñ âûñîêèì ïðîñòðàíñòâåííûì ðàçðåøåíèåì, Âåñòíèê Ìîñêîâñêîãî óí-òà, ñåð.
3: ôèçèêà è àñòðîíîìèÿ, N. 5,c. 65-67, 2008.33.
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