Cosmic Rays. Sayfa 3

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1 Cosmic Rays Sayfa 3

2 Early Attempts Sayfa 4

3 Cosmic Rays Cosmic rays are energetic particles which do not originate from Earth. Primary Cosmic Rays originate from energetic processes on the Stars and travel interstellar medium. The cosmic radiation comes from Sun and outside the solar system (such as rotating neutron stars, supernovae) High energy primary cosmic rays collide with particles high in the atmosphere and cause jets of secondary particles known as air shower. Sayfa 5

4 The primary cosmic radiation includes all stable charged particles and nuclei with lifetimes of order 10 6 years or longer. Electrons / Positrons Protons / Antiprotons Helium Lithium Beryllium Boron Carbon Oxygen Iron... Sayfa 6

5 Sayfa 7

6 Major components of the primary cosmic radiation. * Protons ~ 90% * He ~ 9 % * e s and other nuclei ~ 1% Note that some cosmic rays can have energies of over 10 6 GeV = 1000 TeV = 1 PeV. far higher than LHC protons (7 TeV) Sayfa 8

7 Cosmic Rays in Atmosphere When primary cosmic rays hit Earth's atmosphere at around 30,000 m above the surface, the impacts cause nuclear reactions which produce pions, kaons and other unstable mesons called air shower. This is important for radio carbon dating Sayfa 12

8 Cosmic Muons The newly produced (many) charged pions, quickly decay into muons. and neutral pions decay mostly to two photons: Many of these muons are able to reach the surface of the Earth. Since > muons do not interact strongly with the atmosphere and > the relativistic effect of time dilation. Sayfa 13

9 Sayfa 15

10 Sayfa 16

11 Muon charge ratio Sayfa 17

12 Muon vertical intensity Sayfa 18

13 Big-Bang Cosmological model to explain the universe today Exapanding Universe Hubble Red shift (1924) Cosmic Background (1964) Temperature of the universe in Kelvin: T / t is the time in secons. t Age of the universe is: billion years. T = 3 K Sayfa 19

14 Cosmic Background Radiation (CBR) Expanding universe cools down. CBR is the thermal radiation assumed to be left over from the "Big Bang" of cosmology. With a traditional optical telescope, the space between stars and galaxies (the background) is completely dark. However, a sufficiently sensitive radio telescope shows a faint background glow, almost exactly the same in all directions. Sayfa 20

15 CBR & GZK cutoff GZK cutoff is a theoretical upper limit on the energy of cosmic rays coming from "distant" sources. Consider an ultra-relativistic proton ejected from a star. This proton may collide with a microwave from CBR photon and the following reactions can occur: p n 0 p p Here, energy of the microwave photon is about: E kt 2.63x10 10 MeV Sayfa 22

16 CBR & GZK cutoff Question: What is the threshold energy of proton starting the reaction? p n Answer: E p ( mnc m c ) ( mpc ) 20 3 x 10 4E ev Above this energy no primary cosmic ray can be found. Sayfa 23

17 CBR & GZK cutoff Sayfa 24

18 Kıvılcım Odası (Spark Chamber) Haziran 2016 Sayfa 1

19 Kıvılcım Odası Parçacıkların izinin gözlenmesi için kullanılan Gaz Algıcı. Sayfa 2

20 Kıvılcım Odası (KO) 1970 lerin ortasına kadar seçici iz sürücüler olarak kullanıldı. Günümüzde Fizik Bölümlerinde, Sergilerde, Müzelerde Kıvılcım Odası (KO): soygaz veya gaz karışımları içerir Saçılma deneyleri - Λ 0 magnetic moment - Neutrino etkileşme deneyleri Sayfa 3

21 Kıvılcım Odası (KO) Kıvılcım Odası (KO): soygaz veya gaz karışımları içerir. Gaziantep te: 20cm x 20cm ebatlarındaki Alüminyum düzlemlerden oluşan bir KO tasarlanıp üretilmesi amaçlanladı. Sonuç... Sayfa 4

22 Nisan 2014 (BAP Projesi) Sayfa 5

23 Nisan 2015 (parçalar geldi) 2 parıldak (BC408, 2x500 Dolar) 2 PMT module (H , 2x500 Avro) 1 DRS4 (Evaluation Board, 900 Avro) Toplam: ~ TL Sayfa 6

24 BC408 Sayfa 7

25 Hamamatsu H10721 photosensor module Sayfa 8

26 Haziran 2015, Veri Toplama Sayfa 9

27 Muon Akısı [E.Şahin] Deniz seviyesi : Φ ~ 1.0 cm 2 dk 1 ~ 167 m 2 s 1 [PDG] Gaziantep (850 m) : Φ ~ 1.1 cm 2 dk 1 ~ 185 m 2 s 1 Sayfa 10

28 Muonların Açısal Dağılımı [E.Şahin] f(θ) ~ cos 2 (θ) [PDG] Sayfa 11

29 Muonların Ortalama Hızı [M.C.Karaman] x = {20, 30, 40, 50, 60, 70} cm x = 40 cm x = 70 cm Sayfa 12

30 Muonların Ortalama Hızı [M.C.Karaman] Sayfa 13

31 Muonların Ömrü [M.Masri, M.C.Karaman] Sayfa 14

32 Muonların Ömrü Sayfa 15

33 Muonların Ömrü Sayfa 16

34 Muonların Ömrü Dünya Ortalaması (PDG): ± us Bizim sonuç 1 (Nisan 2016): ± us Bizim sonuç 2 (Mayıs 2016): ± us Sayfa 17

35 Muon Lifetime Measurement (ADC circuit and DAQ system) Hızlandırıcı ve Algıç Fiziği Çalıştayı Gaziantep University Assoc.Prof.Dr. Ahmet Bingul Mehmet Can Karaman Mahmoud Masri

36 2

37 PMT Photomultiplier tube 3

38 Inside The Photosensor Module (Hamamatsu h10721) photo source : h10721 datasheet 4

39 PMT Connections 0.95V to 1.05V 10 kω 5

40 The ADC Circuit 6

41 What do we want the circuit to do DIY (do it yourself) Simple Inexpensive Easy to replicate Fast 7

42 Comparator 8 photo source : Encyclopedia of Electronic Components. Volume 2 - Charles Platt

43 A Simple Solution 9

44 The Comparator Response Time 10

45 The Uncertainty Problem 200mV overdrive => 40ns 10mV overdrive => 300ns 11

46 The Solution for the Uncertainty 12

47 The Final Circuit Uncertainty : ±5ns 13

48 The Final Circuit Uncertainty : ±5ns 14

49 The Shape of The Event We re Looking For 15

50 The Total Price Component Price Quantity Total Price LM TL 4 12 TL Resistors 1/4w Potentiomet er 0.1 TL 10 1 TL 0.5 TL 6 3 TL Total TL 16

51 Data Acquisition System 17

52 Arduino Due Price : $ Clock speed : 84MHz 18

53 Sampling Rate Using std arduino libraries : 1MHz (1000 ns) 19

54 Sampling Rate Using std arduino libraries : 1MHz (1000 ns) Using port register (ateml datasheet) : 6.25MHz (160 ns) 6.25X faster 20

55 Sampling Rate Using std arduino libraries : 1MHz (1000 ns) Using port register (ateml datasheet) : 6.25MHz (160 ns) 6.25X faster After editing the assembly output : 14MHz (71 ns) 14X faster 21

56 The Algorithm 22

57 23

58 Muon Lifetime Distribution 24

59 Muon Lifetime Distribution 25

60 Next Step Publish step-by-step Tutorial explaining how to replicate the experiment Try to reduce the cost of the PMT and the Scintillators Use more than one PMT on the Scintillator => triangulate the hit position and calculate the angular distribution 26

61 Questions?

62 Thanks Hızlandırıcı ve Algıç Fiziği Çalıştayı Gaziantep University Assoc.Prof.Dr. Ahmet Bingul Mehmet Can Karaman Mahmoud Masri

63 Kıvılcım Odası Sayfa 18

64 Optik Elektronik Mekanik Grupen, Particle Detector Sayfa 19

65 Optik Elektronik Mekanik Sayfa 20

66 Bizim Elektronik Sayfa 21

67 Kıvılcım Odası Paralel plakaların arası gaz dolu (He, Ne) Plakalar yüksek voltaj kaynağına bağlı Gaz kazancı: M = (daha küçük olunca gaz yükseltme gerçekleşmez) Sayfa 22

68 Kıvılcım Odası Çığ oluşumu Sayfa 23

69 Kıvılcım Odası (Videolar) Sayfa 24

70 Kıvılcım Odası (Videolar) Sayfa 25

71 Teşekkürler... Sayfa 26

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