Ebe a na-enyocha ụzarị ike ndọda

A gravitational-wave detector (nke a na-eji na gravitational's wave observatory) bụ ngwaọrụ ọ bụla emebere iji tụọ obere mgbagha nke oge oghere a na-akpọ ebili mmiri ndọda. Kemgbe afọ ndị 1960, a na-ewu ụdị ihe nchọta ike ndọda dị iche iche ma na-emeziwanye ya mgbe niile. Ọgbọ nke laser interferometers nke oge a eruola mmetụta dị mkpa iji chọpụta ebili mmiri ndọda site na isi mmalite nke mbara igwe, si otú a na-etolite ngwa ọrụ bụ isi nke mbara igwe-ebili mmiri.

Nnyocha mbụ nke ebili mmiri nke ike ndọda mere na Septemba 2015 site na Advanced LIGO observatories, na-achọpụta ebili mmiri na-adọkpụ nke nwere ogologo nke puku kilomita ole na ole site na njikọta abụọ nke oghere ojii kpakpando. ^[1] June 2023, njikọ aka anọ nke usoro oge pulsar gosipụtara ihe akaebe mbụ siri ike maka ndabere nke ebili mmiri nke ogologo ebili mmiri na-agafe afọ ìhè, o yikarịrị ka ọ sitere n'ọtụtụ ọnụọgụ abụọ nke nnukwu oghere ojii.

Nchọpụta kpọmkwem nke ebili mmiri na-adọkpụ na-agbagwoju anya site na obere mmetụta nke ebili ikuku na-emepụta na ihe nchọpụta. Nnukwu ebili mmiri na-agbadata dị ka ihe megidere anya site na isi iyi. Ya mere, ọbụna ebili mmiri sitere na usoro ndị dị oke egwu dị ka njikọta nke oghere ojii abụọ na-anwụ na obere oke mgbe ha rutere n'ụwa. Ndị -ahụ maka IHE NDỊ dị na mbara igwe buru amụma na ụfọdụ ebili mmiri na-agafe n'ụwa nwere ike ịmepụta mmegharị dị iche iche na usoro 10⁻¹⁸ m na ngwá ọrụ LIGO.

Ụdị mbụ bụ antenna dị ka ogwe okpomọkụ nke a na-akpọ ogwe Weber; ndị a na-achịkwa na 1960s na 1970s ma wuo ọtụtụ gburugburu ụwa. Weber ^[2] ụfọdụ ndị ọzọ kwuru na ngwụcha afọ 1960 na mmalite afọ 1970 na ngwaọrụ ndị a chọpụtara ebili mmiri nke ike ndọda; Otú ọ dị, ndị ọzọ na-eme nnwale enweghị ike ịchọpụta ebili mmiri na-eji ha eme ihe, nkwekọrịta mepụtara na ogwe Weber agaghị abụ ụzọ bara uru iji chọpụta ebili mmiri.

Ọgbọ nke abụọ nke resonant mass antennas, nke e mepụtara na 1980 na 1990, bụ antennas bar cryogenic nke a na-akpọkwa Weber Bars mgbe ụfọdụ. N'afọ 1990, e nwere nnukwu antennas bar cryogenic ise: AURIGA (Padua, Italy), NAUTILUS (Rome, Italy), EXPLORER (CERN, Switzerland), ALLEGRO (Louisiana, US), na NIOBE (Perth, Australia). Na 1997, antennas ise a nke otu nyocha anọ na-agba hiwere International Gravitational Event Collaboration (IGEC) maka imekọ ihe ọnụ. Ọ bụ ezie na e nwere ọtụtụ ikpe nke ngbanwe na-akọwaghị site na mgbaàmà ndabere, ọnweghị ihe ọ bụla ekwenyesiri ike na nlele nke ebili mmiri ndọda na ihe nchọpụta ndị a.

N'afọ ndị 1980, enwekwara antenna bar cryogenic nke a na-akpọ ALTAIR, nke, yana antenna okpomọkụ nke ime ụlọ nke a na-akpọ GEOGRAV, wuru na Italy dị ka ihe atụ maka antennas mmanya na-esote. Ndị na-arụ ọrụ nke GEOGRAV-nchọpụta kwuru na ha ahụla ebili mmiri ndọda na-abịa site na supernova SN1987A (yana antenna ụlọ okpomọkụ ọzọ), mana ndị obodo anabataghị nkwupụta ndị a.

N'afọ 2000, ọgbọ nke atọ nke antenna mass resonant, antennas cryogenic spherical, pụtara. Atụpụtara antennas okirikiri anọ gburugburu afọ 2000 na abụọ n'ime ha ka ewuru dị ka ụdị agbadata, kagbuo ndị ọzọ. Antenna ndị a tụrụ aro bụ GRAIL (Netherland, gbadata na MiniGRAIL), TIGA (US, obere prototypes emere), SFERA (Italy), na Graviton (Brasil, gbadara na Mario Schenberg).

Ndepụta nke ihe nchọpụta nke gravitational wave[dezie | dezie ebe o si]

Ihe na-achọpụta oke[dezie | dezie ebe o si]

Ọgbọ mbụ^[4]
- Ebe a na-ere mmanya Weber (1960s-80s)
Ọgbọ nke abụọ^[4]
- Onye Nlereanya (CERN, 1985-)
- GEOGRAV (Rome, 1980s-)
- ALTAIR (Frascati, 1990-)
- ALLEGRO (Baton Rouge, 1991-2008)
- NIOBE (Perth, 1993-)
- NAUTILUS (Rome, 1995-)
- AURIGA (Padova, 1997-)
Ọgbọ nke atọ
- Mario Schenberg (São Paulo, 2003-)
- MiniGrail (Leiden, 2003-)

Interferometers[dezie | dezie ebe o si]

^[5]^[6] na-ejikarị ndị na-achọpụta ụzarị ike ndọda na ọgbọ dabere na teknụzụ eji eme ihe. Ndị nchọpụta int^[5] e depụtara na 1990s na 2000s na-egosi ihe ndabere maka ọtụtụ n'ime teknụzụ ntọala dị mkpa maka nchọpụta mbụ ma a na-akpọkarị ha ọgbọ mbụ. ^[6] Ọgbọ nke abụọ nke ihe nchọpụta ^[5]-arụ ọrụ na afọ 2010, ọtụtụ n'ime ha n'otu ụlọ ọrụ ahụ dị ka LIGO na Virgo, meziwanyere atụmatụ ndị a na usoro dị mgbagwoju anya dị ka enyo cryogenic na ntinye nke ikuku. Nke a dugara na nchọpụta mbụ doro anya nke ebili mmiri nke ike ndọda site na Advanced LIGO na 2015. Ọgbọ nke atọ nke ndị na-achọpụta ihe dị ugbu a na atụmatụ, ma na-achọ imeziwanye n'ọgbọ nke abụọ site n'inweta nghọta nchọpụta ka ukwuu na ọnụọgụ dị ukwuu. Nnyocha ndị a niile na-agụnye ọtụtụ teknụzụ n'okpuru mmepe na-aga n'ihu n'ime ọtụtụ iri afọ, yabụ nhazi site na ọgbọ bụ ihe siri ike.

Ọgbọ mbụ
- (1995) TAMA 300Ugboro 300
- (1995) GEO600
- (2002) IHEIHE NDỊ
- (2006) Klas
- (2007) Virgo interferometer
Ọgbọ nke Abụọ
- (2010) GEO High Frequency^[7]^[5]
- (2015) Advanced LIGO^[5]
- Advanced (2016) Virgo^[5]
- (2019) KAGRA (LCGT) ^[5]
- (2023) IndIGO (LIGO-India) ^[8]
- ^[5] (nke na-adịghịzi adị) AIGO[1]
Ọgbọ nke atọ
- (2030s) Einstein Telescope
- (2030s) Cosmic ExplorerOnye Nnyocha Eluigwe
Ebe e si nweta ya
- (2035) TianQin
- (2030s?) Taiji (nchọpụta nke ebili mmiri) Taiji (ebe a na-enyocha ebili mmiri)
- (2027) Deci-hertz Interferometer Gravitational wave Observatory (DECIGO)
- (2034) Laser Interferometer Space Antenna (LISA Pathfinder, ọrụ mmepe, ka a malitere na Disemba 2015)

Oge Pulsar[dezie | dezie ebe o si]

(2005) Usoro oge pulsar nke mba ụwa

Hụkwa[dezie | dezie ebe o si]

Echiche nchọpụta
Nkà mmụta mbara igwe nke gravitational wave
Ihe nzacha kwekọrọ

Edensibia[dezie | dezie ebe o si]

↑ Conover (15 September 2023). Scientists have two ways to spot gravitational waves. Here are some other ideas. sciencenews.org. Retrieved on 17 September 2023. “Just as light comes in a spectrum, or a variety of wavelengths, so do gravitational waves. Different wavelengths point to different types of cosmic origins and require different flavors of detectors.”
↑ For a review of early experiments using Weber bars, see Levine (April 2004). "Early Gravity-Wave Detection Experiments, 1960-1975". Physics in Perspective 6 (1): 42–75. DOI:10.1007/s00016-003-0179-6.
↑ Moore, Christopher (19 July 2013). Gravitational Wave Detectors and Sources. Archived from the original on 16 April 2014. Retrieved on 17 April 2014.
↑ ^4.0 ^4.1 Aguiar (2010-12-22). "Past, present and future of the Resonant-Mass gravitational wave detectors" (in en). Research in Astronomy and Astrophysics 11 (1): 1–42. DOI:10.1088/1674-4527/11/1/001. ISSN 1674-4527.
↑ ^5.0 ^5.1 ^5.2 ^5.3 ^5.4 ^5.5 ^5.6 ^5.7 Harry (February 2012). "Second generation gravitational wave detectors", The Twelfth Marcel Grossmann Meeting (in en). UNESCO Headquarters, Paris, France: WORLD SCIENTIFIC, 628–644. DOI:10.1142/9789814374552_0032. ISBN 978-981-4374-51-4. Harry, Gregory M. (February 2012). "Second generation gravitational wave detectors". The Twelfth Marcel Grossmann Meeting. UNESCO Headquarters, Paris, France: WORLD SCIENTIFIC. pp. 628–644. doi:10.1142/9789814374552_0032. ISBN 978-981-4374-51-4.
↑ ^6.0 ^6.1 Punturo (21 April 2010). "The third generation of gravitational wave observatories and their science reach". Classical and Quantum Gravity 27 (8): 084007. DOI:10.1088/0264-9381/27/8/084007. ISSN 0264-9381.
↑ GEO High Frequency and Squeezing. www.geo600.org. Archived from the original on 15 September 2019. Retrieved on 18 September 2019.
↑ Bhattacharya (25 March 2016). India's LIGO Detector Has the Money it Needs, a Site in Sight, and a Completion Date Too (en-GB). The Wire. Retrieved on 16 June 2016.

Njikọ mpụga[dezie | dezie ebe o si]

NYT.com/2016/02/12/science/ligo-gravitational-waves-black-holes-einstein.html" id="mwA6o" rel="mw:ExtLink nofollow">Vidio (04:36) - Ịchọpụta ebili mmiri, Dennis Overbye, NYT (11 Febụwarị 2016).
Vidio (71:29) - Nzukọ ndị nta akụkọ na-ekwupụta nchọpụta: "LIGO na-achọpụta ebili mmiri", National Science Foundation (11 Febụwarị 2016).

Àtụ:Gravitational waves

[conover2023-1] Conover (15 September 2023). Scientists have two ways to spot gravitational waves. Here are some other ideas. sciencenews.org. Retrieved on 17 September 2023. “Just as light comes in a spectrum, or a variety of wavelengths, so do gravitational waves. Different wavelengths point to different types of cosmic origins and require different flavors of detectors.”

[2] For a review of early experiments using Weber bars, see Levine (April 2004). "Early Gravity-Wave Detection Experiments, 1960-1975". Physics in Perspective 6 (1): 42–75. DOI:10.1007/s00016-003-0179-6.

[3] Moore, Christopher (19 July 2013). Gravitational Wave Detectors and Sources. Archived from the original on 16 April 2014. Retrieved on 17 April 2014.

[:2-4] 4.0 ^4.1 Aguiar (2010-12-22). "Past, present and future of the Resonant-Mass gravitational wave detectors" (in en). Research in Astronomy and Astrophysics 11 (1): 1–42. DOI:10.1088/1674-4527/11/1/001. ISSN 1674-4527.

[:1-5] 5.0 ^5.1 ^5.2 ^5.3 ^5.4 ^5.5 ^5.6 ^5.7 Harry (February 2012). "Second generation gravitational wave detectors", The Twelfth Marcel Grossmann Meeting (in en). UNESCO Headquarters, Paris, France: WORLD SCIENTIFIC, 628–644. DOI:10.1142/9789814374552_0032. ISBN 978-981-4374-51-4. Harry, Gregory M. (February 2012). "Second generation gravitational wave detectors". The Twelfth Marcel Grossmann Meeting. UNESCO Headquarters, Paris, France: WORLD SCIENTIFIC. pp. 628–644. doi:10.1142/9789814374552_0032. ISBN 978-981-4374-51-4.

[:0-6] 6.0 ^6.1 Punturo (21 April 2010). "The third generation of gravitational wave observatories and their science reach". Classical and Quantum Gravity 27 (8): 084007. DOI:10.1088/0264-9381/27/8/084007. ISSN 0264-9381.

[7] GEO High Frequency and Squeezing. www.geo600.org. Archived from the original on 15 September 2019. Retrieved on 18 September 2019.

[8] Bhattacharya (25 March 2016). India's LIGO Detector Has the Money it Needs, a Site in Sight, and a Completion Date Too (en-GB). The Wire. Retrieved on 16 June 2016.

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