Muon Lifetime Alden Deran.

Slides:



Advertisements
Similar presentations
QUARKNET 2011 SESSION 1 1. Abstract Week One Hardware Performance Plateauing Flux Shower Lifetime Purpose, Research Question, Hypothesis Experimental.
Advertisements

Lecture items Neutron log * Definition. * Types
Particle interactions and detectors
Measurement of lifetime for muons captured inside nuclei Advisors: Tsung-Lung Li Wen-Chen Chang Student: Shiuan-Hal Shiu 2007/06/27.
Cosmic Ray Lifetime Study A measurement of Special Relativity Richard Lasky – Summer 2010.
Conducted by: Adrian Lorenzana David Harris Muon Speed/Lifetime Study.
Cosmic Rays Basic particle discovery. Cosmic Rays at Earth – Primaries (protons, nuclei) – Secondaries (pions) – Decay products (muons, photons, electrons)
Presented by Steve Kliewer Muon Lifetime Experiment: A Model.
Counting Cosmic Rays through the passage of matter By Edwin Antillon.
Particle RANGE Through Material and Particle Lifetimes Dan Claes CROP Fall 2006 Workshop Saturday, October 14, 2006.
SCIPP Summer Outreach Project July Cosmic Ray Detectors Cosmic Ray Detectors Detector Testing Detector Testing Muon Lifetime Experiment Muon Lifetime.
Particle Interactions
Cosmic Ray Detection Experimental Report Alisa Bredensteiner Endeavour Institute Santa Cruz Institute of Particle Physics Quarknet August 2010.
How to draw a (Bohr) model of an atom
Cosmic Ray Muon Detection Department of Physics and Space Sciences Florida Institute of Technology Georgia Karagiorgi Julie Slanker Advisor: Dr. M. Hohlmann.
Radiation therapy is based on the exposure of malign tumor cells to significant but well localized doses of radiation to destroy the tumor cells. The.
Stopping Power The linear stopping power S for charged particles in a given absorber is simply defined as the differential energy loss for that particle.
Lecture 1.3: Interaction of Radiation with Matter
Tools for Nuclear & Particle Physics Experimental Background.
Energy Distribution of Cosmic Ray Muons Paul Hinrichs With David Lee Advised by Phil Dudero.
1 Nuclear Stability The larger the atom, the greater the proportion of the nucleus that must be neutrons. –The A/Z ratio is greater than 2 (or the N to.
Masses of Atoms. Atomic Mass  Remember that Protons and Neutrons are much bigger than an Electron.  Because of this, the nucleus contains the majority.
Measurement of lifetime for muons captured inside nuclei
Alpha and Beta Interactions
1 dE/dx  Let’s next turn our attention to how charged particles lose energy in matter  To start with we’ll consider only heavy charged particles like.
Cosmic rays at sea level. There is in nearby interstellar space a flux of particles—mostly protons and atomic nuclei— travelling at almost the speed of.
Cosmic Rays Cosmic Rays at Sea-Level - Extensive Air Showers and the detection of cosmic rays.
Cosmic Ray Workshop May 15, Cosmic Ray Detector Kit.
QuarkNet and Cosmic Ray Muon Flux Experiments Florida Academy of Sciences Spring Conference 2009 Alfred Menendez and Michael Abercrombie with Dr. Marcus.
Resolution and radiative corrections A first order estimate for pbar p  e + e - T. H. IPN Orsay 05/10/2011 GDR PH-QCD meeting on « The nucleon structure.
Calibration instructions for Quarknet Cosmic-Ray Detector How to Plateau the Counters A friendly guide for students and teachers Edited by Jeremy Paschke,
Victor Hess in his balloon (1912). Cosmic Rays Produce Muons in the Atmosphere.
INTERACTIONS OF RADIATION WITH MATTER. twCshttp:// twCs
Learning Objectives Calorimetry and Showers
Introduction Cosmic rays, originating from distant solar flares and supernova, bombard our planet constantly and collide with atomic nuclei at an altitude.
Radiation Protection and Safety 3/12/ Interactions with Electrons   Energy-loss Mechanisms Electrons and positrons have similar stopping powers.
Track Reconstruction in MUCH and TRD Andrey Lebedev 1,2 Gennady Ososkov 2 1 Gesellschaft für Schwerionenforschung, Darmstadt, Germany 2 Laboratory of Information.
Nuclear Chemistry. Reactions All the reactions you have see have involved transfer or share of electrons. The atoms on the left are the same as the atoms.
Some nuclei – usually large ones – are unstable They cannot fit their neutrons and protons into a space small enough that that strong nuclear force can.
Steve Chao & Maha Hamid. Day 1 After reviewing the syllabus for the two weeks, we moved to laboratory to take apart and rebuild two cosmic ray detector.
Calibration Instructions for Quarknet Cosmic Ray Detector
Rolling radioactive dice
QuarkNet Student Investigations
Muon Lab Theory Muons (standard model) Cosmic rays Life time
INTERACTION OF PARTICLES WITH MATTER
QuarkNet and Cosmic Ray Muon Flux Experiments
X-rays Physics 102: Lecture 26
Methods of Experimental Particle Physics
Interactions of Radiation With Matter
Dr Andrew French P5/6 Winchester College
Radioactivity.
DO NOW Pick up notes sheet and Subatomic particle table.
Nuclear Medicine Physics & Instrumentation I
The Life and Times of Cosmic-ray Muons
Spectrometry of high energy gamma ray
NanoBPM Status and Multibunch Mark Slater, Cambridge University
Dr. Izyan Hazwani + JPARC (Prof. Ejiri)
Devil physics The baddest class on campus IB Physics
Summary of alpha etc.
Monoenergetic Neutrino Beam for Long Baseline Experiments
Measuring High Energy Electromagnetic Cascades in the Laboratory
Nuclear Chemistry Chapter 21A
Nuclear Chemistry Chapter 21A
Muonic Atoms I’d like to talk to you about muonic atoms.
PHYS 3446 – Lecture #14 Wednesday,March 7, 2012 Dr. Brandt
PHYS 3446, Spring 2012 Andrew Brandt
Austin Park and Willie Dong
Experiments from the Dark Side of the Muon
Radioactivity GEOG/PHYS 182.
Radioactivity – inverse square law, absorption, and rates
Presentation transcript:

Muon Lifetime Alden Deran

Muon Energy Loss in Materials Typical cosmic ray muons experience energy loss in a material almost completely due to electronic stopping power – the ionization of atoms in the material. 1The remaining (approximately 1%) of the energy loss is due to Bremsstrahlung radiation, electron/positron pair production, and photonuclear interraction. However, due to the much lower mass of electrons, they are accelerated much more by atomic nuclei and lose more energy to Bremsstrahlung radiation than muons. The amount of energy loss due to Bremsstrahlung radiation is proportional to 1/m4. This radiation is the dominant form of energy loss for electrons, so some materials will stop muons while having a much smaller effect on electrons. In this experiment, it is hypothesized that books will stop muons but allow electrons to reach the detectors.

DAQ Board Setup Gate width set to 10 microseconds, and changed to 15 microseconds for one experiment. TMC delay set to 48 nanoseconds. Different coincidence settings were tried.

Muon Lifetime Experimental Setup When a muon passes through detector A and then is trapped in the material between the detectors, it will eventually decay into an electron, which may be detected in another one of the detectors (or multiple). The time between these two events will be recorded. If a muon passes through detector a and then is not trapped, it will pass through another detector within a nanosecond, and this event will be ignored.

4

5 Hours Stacked With Books

With Books, stacked, 158 minutes

Without Books, Stacked, 158 minutes

Overnight with Partial Box

Partial Box with 2-Fold Coincidence

Results Data Set Time (minutes) Maximum decays Lifetime (microseconds) Error Comments 1 5 3 Not enough data, gate width set too small 2 Data file was lost 36 6 Still not enough data, though several decays detected 4 120 27 1.921 .307 37 3.145 .608 150 2.401 0.228 First successful overnight test 7 100 1.870 0.139 Second successful overnight test – box configuration. 8 80 2.420 .199 2 fold coincidence 9 155 1.913 .107 2 fold coincidence with partial box 10 30 11 1.853 .384 Without books stacked 13 1.254 .210 With books box configuration 12 158 1.897 .346 With books stacked 39 1.354 .172

Additional Error Calculations Chi-square test can determine how good the curve fit is. Data must be downloaded from quarknet: In the data plot, click “analysis directory.” Then, click “lifetimeOut”. Somehow move the data to an excel file or write an analysis program to parse the data file.

Sources Groom, Donald E. Muon Stopping Power and Range Tables 10 MeV to 100 TeV. http://www.sciencedirect.com/science?_ob=ArticleURL&_udi=B6WBB-45BT4PM-6&_user=4428&_coverDate=07%2F31%2F2001&_rdoc=1&_fmt=high&_orig=search&_sort=d&_docanchor=&view=c&_acct=C000059601&_version=1&_urlVersion=0&_userid=4428&md5=3d7e89088f9c3ffdbe1a22f4459f1f7e