Ihe gbara ọchịchịrị

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  Na ihe mbara igwe, ihe gbara bụ ụdị ihe a na-eche n'echiche nke na-egosi na ọ naghị eme ihe na ìhè ma ọ bụ oghere electromagnetic .  Ihe gbara ụmụaka site na mgbochi ndòda nke Park ike ya site na mmekọ izugbe ọ ọgwụgwọla ma ihe dị ugbu a akụkụ ka ike ịhụ.  hụrụ dị otú ahụ na-eme na nhazi na evolushọn nke ike ike, [1] gravitational lensing, [2] ejide na ala na-ahụ anya njikọ a, oke ọnọdụ na galactic collisions.  ime nsogbu nsogbu, na mbara igwe microwave.  anisotropies ndabere .

[1] [2] [3]N' ọkọlọtọ Lambda-CDM nke cosmology, oke-ike mgbochi nke ọnụnọ na ala bụ 5% akpọ okwu, 26.8% gbara mgbochi, na 68.2% ụdị ume nke a mara dị ka mgbochi ike .  [1] [2] [3] [4] Ya mere, ihe gbara bụ 85% [lower-alpha 1] nke mkpokọta mkpokọta, ebe ike ịgba na ihe mgbochi bụ 95% nke mkpokọta ume-ike

[4] [5]A maghị ihe gbara ka ya na ihe baryonic n'ebe na radieshon na-emekọ ihe ma e nso site na ike ndoda, [lower-alpha 2] na-eme ka o sie ike na ụlọ ụlọ.  Nkọwa na-eduga bụ na ihe gbara mgbochi bụ ụfọdụ subatomic a na-ahụ, [lower-alpha 1] dị ka ihe ndị na-adịghị ike na-eme egwuregwu ihe (WIMPs) ma ọ bụ axions .  [1] Isi ihe ọzọ nwere ike ime bụ na ihe m na-agba gbara bụ oghere ojii primordial

. A na-ekewa ihe mgbochi dị ka "oyi", "ọkụ", ma ọ bụ "ọkụ" dị ka ọsọ ya siri dị (kpọmkwem, ogologo mgbasa ozi efu ya).  Modelsdị ndị na-adịbeghị anya akwadowo akụkụ gbara dị iche, nke ihe owuwu na- site na iji jawaabta na-achịkọta ụmụ irighiri ihe, mana ka ọkara apụta nke , 5okwu gbara na- Caraba, nnukwu ike ndọda  na nso nso a na James Webb Space Telescope mere emeela ka okwu ahụ sie ike nke ukwuu maka primordial.  na oghere daa[4] [6] [7]

. [8]Ọ bụ ebe ahụ na obodo astrophysics n'ozuzu na-anabata ụmụaka ndị nke iwu, [1] ole na ole nke ndị ọkà daban mbara igwe, ndị nleba anya anya nke ọma na-adịghị nke ọma site n'okwu gbara, na-  arụ ụka maka ịdị iche iche nke ọkọlọtọ nke izugbe.  Ma ọ bụ ike ndoda .  Ka ọ dị ugbu a, ọ dịghị nke ọ na-eche echiche ike ndọda a na-atụ aro nwere ike kọwapụta nke ọma mpempe ihe ọ elva n'otu oge, na-atụ aro na ọkọta na a ga-agbanwe ike.  ndọda, a ka ga-achọkwa ụdị ụfọdụ nri nke.

[9]Echiche nke ihe gbara nwere nnukwu nnukwu ihe mere eme.  [1] N'ihe odide nke akwụkwọ Baltimore na-ekwu ihe ndị na-eme ka ihe ndị dị ndụ na ihe ndị na-efe efe nke ìhè bụ ebe isi ihe odide gbadoro ụkwụ na nkuzi e nyere na 1884, [  2] Lord Kelvin tụlere ọnụ ọgụgụ ndị nwere ike gburugburu ebe na ọsọ nke ib.  Prọfesọ nke ndị nkuzi, na-eche na ọmụmụ dị 20 ruo 100 nde afọ.  Ọ tụpụtara ihe ga-eme ma ọ bụrụ na ndị ọrụ otu puku nde mmadụ n'ime 1 kilo-parsec nke Sun (n'ebe dị anya parallax ha ga-abụ 1 milli-arcsec ).  Lord Kelvin kwubiri "Ọtụtụ n'ime anyị chere puku kwuru nde, nna ukwu n'ime ha nwere ike ịbụ ahụ gbara afa".  [3] [4] Na 1906, Henri Poincaré na "The Milky Way and Theory of Gases" ji okwu French matière obscure mee ihe.</link> ("okwu gbara mgbochi") n'ịtụle ọrụ Kelvin.  [5] [4] Ọ na ọnụ ọgụgụ nke ihe gbara mgba ga-adị mkpa ka ọ dị obere obere nke ihe a na-ahụ anya.

[10]Na 1933, onye Switzerland astrophysicist Fritz Zwicky, bụ onye ike ike iwe mgbe ọ na-arụ ọrụ na California Institute of Technology, mere ihe yiri ya.  [1] [2] Zwicky ebe virial theorem na Coma Cluster wee nwe ihe nkiri nke oke a na-ahụ ahụ anya ọkpara dunkle Materie ('ihe gbara').  Zwicky mere na oke ya dabere na Lincoln nke mkpà dị nso na nsstụ ya wee jiri nke ahụ gosiri dabere na nchapụta ya na nọmba mpịaji.  O mere akara na ahụ nwere ihe dị ka okpukpu 400 akụkụ ka a na-ahụ anya.  mmetụta ike ndoda nke ndị ọrịa ndị a na-ahụ anya dị obere maka ịgba ịgba ọsọ ọsọ dị ahụ, ya mere a ike izochi oke n'anya.  Dabere na nkwubi okwu ndị a, Zwicky chepụtara ụfọdụ ihe a na-ahụ ahụ anya nyere oke na ihe ndị na-achọ data ya iji jide ahụ ọnụ.  [3] Atụmatụ Zwicky site na ihe usoro nke fim ukwuu, tumadi n'ihi uru na-adịchaghị nke Hubble mgbe niile ;  [4] Otu ngụkọ taa na-egosi ntakiri, na-eji ebu ka ukwuu maka oke ọkụ.  Ka o sina dị, Zwicky kwubiri n'ụzọ ziri ezi site na ngụkọ ya na ihe ka ukwuu n'okwu ahụ gbara.

. [11]Ngosipụta ndị ọzọ nke nhụsianya oke na ọkụ sitere na nha usoro ngagharị iwe.  N'afọ 1939, Horace W. Babcock kọkwara na ntụgharị maka Andromeda nebula (nke a maara ugbu a dị ka Andromeda Galaxy), nke ebu aro na oke-na-luminosity ruru na- arọ radially.  [1] O kwuru na ọ bụ n'ihi mmịnye ọkụ dị n'ime ikike ma ọ bụ ike n'amaka mpụta nke gburugburu ahụ ọ bụghị n'ihe na-efu efu ọ a.  N'ịgbaso ndị Babcock nke 1939 mgbanwe ngbanwe ngwa na-Ịgba anya ya na-amaama ihe Andromeda na oke nha na ìhè nke 50;  na 1940 Jan Oort chọta wee dee nnukwu ihe halo na-ahụ anya nke NGC 3115

N'otu oge ahụ Rubin na Ford nọ na-enyocha akụkụ ntụgharị anya anya, ndị na-enyocha mbara igwe redio na-eji teliskop redio ọhụrụ mee eserese 21. ahịrị cm nke atomic hydrogen na ụyọkọ kpakpando dị nso. Nkesa radial nke interstellar atomic hydrogen ( H Ⅰ ) na-agbasakarị n'ebe dị anya nke galactic karịa ka a na-ahụ anya dị ka ìhè kpakpando mkpokọta, na-agbasapụ anya nke anya maka ntụgharị ntụgharị - ma si otú a na-ekesa mkpokọta - na ọchịchị ọhụrụ na-agbanwe agbanwe. Maapụ mbụ nke Andromeda nwere ndị 300 Igwefoto ụkwụ na Green Bank [12] na 250 efere ụkwụ na Jodrell Bank [13] egosilarị ụzọ ntụgharị H Ⅰ achọpụtaghị ọdịda Keplerian tụrụ anya ya. Ka ndị nnata nwere mmetụta siri ike dị, Roberts & Whitehurst (1975) [14] nwere ike ịchọpụta ọsọ ọsọ Andromeda na 30. kpc, karịrị ihe nlele anya. Na-egosipụta uru nke ịchọta diski gas na nnukwu radii; Ọgụgụ akwụkwọ ahụ 16 [14] na-ejikọta data anya [15] (ụyọkọ nke isi ihe na radii na-erughị 15). kpc nwere otu ihe n'ihu) na data H Ⅰ n'etiti 20 na 30 kpc, na-egosipụta ịdị larịị nke mgbanaka mgbanaka ụyọkọ kpakpando dị n'èzí; akụkụ ahụ siri ike na-arị elu n'etiti bụ njupụta anya elu, ebe akụkụ nke ọzọ na-egosi mkpokọta mkpokọta, ka na-ebili n'ahịrị n'ogo kachasị elu. N'otu aka ahụ, a na-emepụta ojiji nke interferometric arrays maka extragalactic H Ⅰ spectroscopy. Rogstad & Shostak (1972) [16] bipụtara H Ⅰ ntụgharị ntụgharị nke spirals ise nke ejiri interferometer Owens Valley mapụta; ntụgharị ntụgharị nke ise ahụ niile dị larịị, na-atụ aro nnukwu ụkpụrụ nke oke-na-ọkụ n'akụkụ mpụta nke H Ⅰ ha gbatịrị. diski. [16]

  1. ↑ Planck captures portrait of the young Universe, revealing earliest light. University of Cambridge (21 March 2013). Retrieved on 21 March 2013.
  2. ↑ Carroll (2007). Dark Matter, Dark Energy: The dark side of the universe. The Teaching Company. “... dark matter: An invisible, essentially collisionless component of matter that makes up about 25 percent of the energy density of the universe ... it's a different kind of particle... something not yet observed in the laboratory ...” 
  3. ↑ Jarosik (2011). "Seven-year Wilson microwave anisotropy probe (WMAP) observations: Sky maps, systematic errors, and basic results". Astrophysical Journal Supplement 192 (2). DOI:10.1088/0067-0049/192/2/14. 
  4. ↑ 4.0 4.1 Bird (1 August 2023). "Primordial black hole dark matter". Physics of the Dark Universe 41. DOI:10.1016/j.dark.2023.101231. ISSN 2212-6864.  Kpọpụta njehie: Invalid <ref> tag; name "Bird" defined multiple times with different content
  5. ↑ Carr (2 May 2022). "Primordial black holes as dark matter candidates". SciPost Physics Lecture Notes. DOI:10.21468/SciPostPhysLectNotes.48. Retrieved on 13 February 2023.  (See also the accompanying slide presentation.
  6. ↑ Hütsi (2 February 2023). "Did JWST observe imprints of axion miniclusters or primordial black holes?". Physical Review D 107 (4). DOI:10.1103/PhysRevD.107.043502. 
  7. ↑ Özsoy (2023). "Inflation and Primordial Black Holes". Universe 9 (5). DOI:10.3390/universe9050203. 
  8. ↑ Sean Carroll (9 May 2012). Dark matter vs. modified gravity: A trialogue. Retrieved on 14 February 2017.
  9. ↑ A history of dark matter – Ars Technica (en-US) (2017-02-03). Retrieved on 2023-10-31.
  10. ↑ "A history of dark matter", Ars Technica. Retrieved on 8 February 2017. (in en-us)
  11. ↑ Oort (April 1940). "Some problems concerning the structure and dynamics of the galactic system and the elliptical nebulae NGC 3115 and 4494". The Astrophysical Journal 91 (3): 273–306. DOI:10.1086/144167. 
  12. ↑ Roberts (May 1966). "A high-resolution 21 cm hydrogen-line survey of the Andromeda nebula". The Astrophysical Journal 159: 639–656. DOI:10.1086/148645. 
  13. ↑ Gottesman (1966). "A neutral hydrogen survey of the southern regions of the Andromeda nebula". Monthly Notices of the Royal Astronomical Society 133 (4): 359–387. DOI:10.1093/mnras/133.4.359. 
  14. ↑ 14.0 14.1 Roberts (October 1975). "The rotation curve and geometry of M 31 at large galactocentric distances". The Astrophysical Journal 201: 327–346. DOI:10.1086/153889. 
  15. ↑ Rubin (February 1970). "Rotation of the Andromeda nebula from a spectroscopic survey of emission regions". The Astrophysical Journal 159: 379–403. DOI:10.1086/150317. 
  16. ↑ 16.0 16.1 Rogstad (September 1972). "Gross properties of five Scd galaxies as determined from 21 centimeter observations". The Astrophysical Journal 176: 315–321. DOI:10.1086/151636. 
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