DABAS VĒSTURE I daļa (5 lekcijas) Kosmiskā evolūcija DABAS VĒSTURE
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1 DABAS VĒSTURE I daļa (5 lekcijas) Kosmiskā evolūcija Kārlis Bērziņš kberzins@latnet.lv lekcija. Reliktais mikroviļņu fona starojums. DABAS VĒSTURE I daļa (5 lekcijas) Kosmiskā evolūcija Kārlis Bērziņš kberzins@latnet.lv Kursa I daļas temati: 1. Ievads kosmoloģijā. 2. Visuma evolūcijas pamati. 3. Reliktais mikroviļņu fona starojums. 4. Visuma struktūras veidošanās un attīstība. Alternatīvās kosmoloģiskās teorijas. 5. Zvaigžņu fizikas pamati. Saules sistēmas kosmogonija. Kosmiskā evolūcija 3 1
2 DABAS VĒSTURE 3. lekcija Reliktais mikroviļņu fona starojums. Lekcijas temati: Reliktā starojuma rašanās fizikālais mehānisms. Reliktā starojuma atklāšana. Absolūti melns ķermenis. Mikroskopiskas anizotropijas. Mikroviļņu fona novērojumu eksperimenti uz Zemes virsmas, atmosfērā un kosmosā. Reliktā starojuma informācijas nozīmīgums kosmoloģijā gadi CMBR, CMB cosmic microwave background radiation. Kosmiskā evolūcija 3 2
3 Visuma evolūcija (atkārtojums) T = 3000 K Rekombinācija Starojums atdalās no vielas = reliktais starojums T 0 = ± K (T = 6000 K) Apmēram tajā pašā laikā iestājas matērijas ēra: COBE Visums ir ļoti homogens 1: No šīm nehomogenitātēm izaug Visuma struktūra! Horizonta rādiusa leņķiskie izmēri: Rekombinacijas virsma Pēdējās izkliedes virsma z~1000 karstāks θ Horizonts ~2º aukstāks Kosmiskā evolūcija 3 3
4 Mikroviļņu fona jeb reliktais starojums G.Gamow un R.Dicke paredzēja ~5K relikto starojumu jau gados. Saīsinājumi: CMB vai CMBR Cosmic Microwave Background Radiation Reliktā starojuma atklāšana Adams (1941) konstatēja ierosinātas starpzvaigžņu CN molekulas, McKellar (1941) novērtēja starojuma lauka λ=2.64mm g. sākumā Robert H. Dicke, P.J.E. Peebles, P.G.Roll, D.T.Wilkinson grupa uz Princtonas universitātes jumta iesāka būvēt pirmo CBR eksperimentu. Well boys, we ve been scooped! Interesanti, ka dažus % no TV trokšņa veido reliktais starojums! Kosmiskā evolūcija 3 4
5 Reliktā starojuma atklāšana 7.35 cm radio viļņa sakaru eksperimentos Penzias un Wilson konstatēja lieku 3.5K troksni, no kuriem 0.5K dēļ baložiem 3K? Nobela prēmija fizikā gadā. T = ± K gada Nobela prēmija fizikā ±30μK rms John C. Mather George F. Smoot Mather et al θ = 7º par kosmiskā mikroviļņu fona starojuma absolūti melna ķermeņa formas un anizotropiju atklāšanu DMR: 90, 53, 31.5 GHz (3.3, 5.7, 9.5 mm) Kosmiskā evolūcija 3 5
6 COsmic Background Explorer COBE Darbs pie projekta iesākās jau g g. 18. novembrī Delta nesējraķete veiksmīgi ievadīja COBE vajadzīgajā orbītā ap Zemi. +10 gadi, risinot datu apstrādes problēmas. COBE orbīta Kosmiskā evolūcija 3 6
7 Datu apstrādes problēmas Liels datu apjoms Nepieciešami jauni algoritmi Hu & Dodelson 2002 COsmic Background Explorer COBE DIRBE FIRAS DMR 3 instrumenti: DIRBE DMR FIRAS Observatorijas izmēri ar Saules paneļiem: 8.5 m; augstums: 5.5 m; svars: kg Kosmiskā evolūcija 3 7
8 DIRBE Diffuse InfraRed Background Explorer Projekta vadītājs: Mike Hauser Uzdevums: mērīt IS fona intensitāti. DIRBE Kosmiskā evolūcija 3 8
9 FIRAS Far InfraRed Background Explorer Projekta vadītājs: John Mather Uzdevums: mērīt CMB spektrālo sadalījumu mm Perfekts absolūti melns ķermenis Mather et al.1990 T = ± K Kosmiskā evolūcija 3 9
10 Perfekts absolūti melns ķermenis F = σ T eff 4 df 2hc λ 2 / dλ = 5 exp 1 ( hc / λkt ) 1 Perfekts absolūti melns ķermenis Kļūda ir 400σ!!! FIRAS 0,1-10 mm Kosmiskā evolūcija 3 10
11 Perfekts absolūti melns ķermenis Mather et al. 1999: T = ± K Lielais Sprādziens apstiprināts Kosmiskā evolūcija 3 11
12 Lielais Sprādziens apstiprināts Reliktais starojums T = 3 K 1: fluktuācijas mm-cm viļņu diapazons 400 fotoni cm fotoni sekundē caur cm 2 DMR Diferential Microwave Radiometer Projekta vadītājs: George Smoot Uzdevums: mērīt 3, 6 un 10 mm. Kosmiskā evolūcija 3 12
13 COBE DMR CBR anizotriopija T= ~30 θ=10 ( T= ~90 θ=1/2 ) CMB anizotropija Dipola moments 0.1% 3 mk 100% 3 K 20 µk v Kosmiskā evolūcija 3 13
14 CMB anizotropija Dipola moments 0.1% 3 mk 100% 3 K v Saules sistēma kustas attiecībā pret CBR Lauvas zvaigznāja virzienā 371±0.5 km/s. Dipola T = ± 3.3 mk CMB anizotropijas Fluktuācijas 1:10 5 DMR: 90, 53, 31.5 GHz (3.3, 5.7, 9.5 mm) Kosmiskā evolūcija 3 14
15 CMB anizotropijas Ted Bunn Zeme, kāda tā tiktu novērota ar COBE izšķiršanas spēju COBE vs. WMAP Kosmiskā evolūcija 3 15
16 COBE vs. WMAP CBR spektrs pirms 2003 Teorētiski iespējams precizēt visus kosmoloģiskos parametrus. Kosmiskā evolūcija 3 16
17 ... un gadā WMAP 3 gadi CMB jaudas spektrs WMAP 2 gadi IR iespējams precizēt visus kosmoloģiskos parametrus! Anizotropijas jauda (µk 2 ) Kosmiskā evolūcija 3 17
18 Sfēriska harmonika Jaudas spektrs Sfēriskā harmonika Degree l Order m Clem Pryke Kosmiskā evolūcija 3 18
19 CMB jaudas spektrs Clem Pryke Individuāli multipoli WMAP Kumulatīvi multipoli 3 gadu attēli 23 GHz GHz Marts Kosmiskā evolūcija 3 19
20 CBR polarizācija WMAP 2006 WMAP datu apstrāde Kosmiskā evolūcija 3 20
21 Daži svarīgākie CMB novērošanas eksperimenti Zemes eksperimenti: DASI Balonu eksperimenti: BOOMERanG MAXIMA Kosmiskie eksperimenti: COBE (COsmic Background Explorer) WMAP (Wilkinson Microwave Anisotropy Probe) kopš 1991.g. Planck (COBRA/SAMBA) plānots 2008g. 31.jūlijā1 MAP foto Tenerifes eksperiments CMB eksperiments ( ) Kanāriju salās Kosmiskā evolūcija 3 21
22 Tenerifes eksperiments CMB eksperiments ( ) Kanāriju salās Bērziņš 1997 DASI The Degree Angular Scale Interferometer Antarktikas eksperiments Kosmiskā evolūcija 3 22
23 Balona Eksperiments TopHat Balona Eksperiments TopHat Kosmiskā evolūcija 3 23
24 BOOMERanG Baloon Observations of Milimetric Radiation and Geophysics WMAP Delta II raķetes starts 2001.g. 30. jūnijā Kosmiskā evolūcija 3 24
25 WMAP orbīta pie L2 Starts Cobe Planck simul etais CMB att els salidzinot ar COBE. Planck Planck WMAP 2 gadi WMAP 8 gadi Planck 1 gads Kosmiskā evolūcija 3 25
26 WMAP un Planck jūtība W.Hu Kosmoloģisko parametru precizēšana Kosmoloģiskie parametri nav neatkarīgi, bet ir saistīti savā starpā! Planck Phase A study Kosmiskā evolūcija 3 26
27 DM un CMB fluktuācijas Dodelson 2001 Kosmoloģiskie parametri Barioniskās matērijas daudzums W.Hu Kosmiskā evolūcija 3 27
28 Kosmoloģiskie parametri Matērijas daudzums W.Hu Visums sastāv no: WMAP Teorētiski iespējams precizēt visus kosmoloģiskos parametrus. No James Schombert Kosmiskā evolūcija 3 28
29 Visuma rejonizācija modelis Page et al. The line marked "x" is the ionization fraction, x=n e /n where n e is the number of electrons and n=11.2ω b (1+z) 3 m -3 is the number of protons with ω b the baryon density. Hinshaw et al. Mikroviļņu debess galvenie avoti Kosmiskā evolūcija 3 29
30 SZ efekts Sunajeva-Zeļedoviča efekts Adopted from L. Van Speybroeck WMAP CMB Tegmark Kosmiskā evolūcija 3 30
31 Bennett et al Kosmoloģisko parametru vērtības ± ± Visuma evolūcija Kosmiskā evolūcija 3 31
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