Cosmic Rays and Air Showers

Slides:



Advertisements
Similar presentations
Tyler Thiele.  Cosmic rays are high energy charged particles, in outer space, that travel at nearly the speed of light and strike the Earth from all.
Advertisements

Spectroscopy. Spectroscopy is complex - but it can be very useful in helping understand how an object like a Star or active galaxy is producing light,
Stellar Nucleosynthesis
Cosmic rays in solar system By: Tiva Sharifi. Cosmic ray The earth atmosphere is bombarded with the energetic particles originating from the outer space.
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.
Gravitational waves LIGO (Laser Interferometer Gravitational-Wave Observatory ) in Louisiana. A laser beam is.
Victor Hess Before making balloon ascents himself, he determined the height at which ground radiation would stop producing ionization (about 500 meters)
The Sun The Sun in X-rays over several years The Sun is a star: a shining ball of gas powered by nuclear fusion. Luminosity of Sun = 4 x erg/s =
Cosmic Rays Discovery of cosmic rays Local measurements Gamma-ray sky (and radio sky) Origin of cosmic rays.
NUCLEAR PHYSICS & RADIOACTIVITY PHYSICS - UNIT ONE.
THE SUN AND STARS And anything I want to put in here.
The Sun Our Nearest Star. The Source of the Sun’s Energy The Source of the Sun’s Energy Fusion of light elements into heavier elements. Hydrogen converts.
Sayfa 1 EP228 Particle Physics Department of Engineering Physics University of Gaziantep Dec 2014 Topic 5 Cosmic Connection Course web page
NASA/NSTA Web Seminar: Radiation – Can’t Live With It, Can’t Live Without It LIVE INTERACTIVE YOUR.
The SUN.
EARTH SCIENCE Prentice Hall EARTH SCIENCE Tarbuck Lutgens 
Cosmic Rays The discovery of cosmic rays Discoveries made with cosmic rays Cosmic rays in modern physics education Let’s count cosmic rays around us.
The Sun Unit 6: Astronomy.
24.1 The Study of Light Electromagnetic Radiation
Cosmic Rays Discovery and its nature. .1 Discovery As long ago as 1900, C. T. R. Wilson and others found that the charge on an electroscope always 'leaked'
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.
Galactic Cosmic Rays (GCRS) Galactic cosmic rays (GCRs) come from outside the solar system but generally from within our Milky Way galaxy. GCRs are atomic.
Cosmic Rays2 The Origin of Cosmic Rays and Geomagnetic Effects.
Marcus Hohlmann with help from Ashraf Farahat Cosmic Rays and Air Showers.
The Sun By: JGilliam The Sun’s CompositionIdentifying Stars Composition ▪ Hydrogen and Helium together make up 99% of the sun’s mass. ▪ 75% of the sun’s.
Unit 8 Chapter 29 The Sun. We used to think that our sun was a ball of fire in the sky. Looking at our sun unaided will cause blindness. The Sun’s Energy.
COSMIC RAYS. At the Earth’ Surface We see cascades from CR primaries interacting with the atmosphere. Need to correct for that to understand their astronomical.
Chapter 29. Sec 1 Structure of the sun People believed the sun’s energy came from fire They believed the sun burned some type of fuel to produce energy.
What is radiation  A form of energy that can move through empty space.  Transfer of energy by electromagnetic waves.
Unit 2- Stars.
12-2 Notes How Stars Shine Chapter 12, Lesson 2.
The Sun.
Chapter 19 Radioactivity
Topic 6 : Atomic and Nuclear Physics.
The Sun Unit 1B : Astronomy.
Particle Physics Lesson 6
Unit 2 Lesson 3 The Sun Copyright © Houghton Mifflin Harcourt Publishing Company.
Physical Science Honors
QuarkNet and Cosmic Ray Muon Flux Experiments
The Atomic Nucleus.
Introduction (Atomic and Nuclear Structure-Radioactivity)
PROPERTIES OF THE SUN Essential Questions
Studying the Sun Who is Stan Hatfield and Ken Pinzke.
25.2 – Stellar Evolution – Part II
24.1 The Study of Light Electromagnetic Radiation
Neutron Detection with MoNA LISA
The Sun Unit 6: Astronomy.
Astronomy-Part 8 Notes Here Comes The Sun
Outside the nucleus, the beta decay {image} will not occur because the neutron and electron have more total mass than the proton. This process can occur.
Search for Order Ancient Greeks: Aristotle Earth Air Fire Water
24.3 – The Sun.
Detecting Particles: The Spark Chamber
Nuclear Binding, Radioactivity
Earth Science Ch. 24 The Sun.
Scintillation Counter
Section 1: Structure of the Sun
Unit 3 Lesson 3 The Sun Copyright © Houghton Mifflin Harcourt Publishing Company 1.
1. People have studied the stars for centuries
RADIOACTIVITY B.Sc. 5th sem.
Astronomy 04 Astronomy 04 The Solar System Chapter 15:
Interaction of Radiation with Matter
1.1.3 Explain how the sun produces energy which is transferred to the Earth by radiation. Sun’s Energy.
The Life Cycle of a Star.
Certain elements radiate particles and turn into other elements.
The Centre of the Solar System Earth Science 11
Certain elements radiate particles and turn into other elements.
Copy week schedule into your agenda and answer the Question of the Day
The sun gives off tremendous amounts of energy
Particle Physics Lesson 6
Presentation transcript:

Cosmic Rays and Air Showers Marcus Hohlmann Dept. of Physics & Space Sciences, Fl. Tech Irish Science Challenge 2006

A: The elements that make up your body and the Earth are star dust… 1 - Have you ever wondered what you are made off? 2 - Where did the elements come from that make up your body? 3 - The elements that make up your body are the same elements found on the Earth. Where did those Earth elements come from? A: The elements that make up your body and the Earth are star dust… … and they still keep coming in the form of cosmic rays

History of Cosmic Rays But not: Where are they coming from ? 1912 - Victor Hess reaches 5350 m altitude in a balloon and shows conclusively that the rate of charged particles increases significantly with height: There is an extraterrestrial source of radiation ! 1930 – Pierre Auger discovers particle showers. 1936 - Hess gets Nobel Prize for discovery of cosmic rays. History of Cosmic Rays Questions that have been answered by now: - What are these particles made of ? - What different kinds are there ? But not: Where are they coming from ? How do they get their momentum ?

Some Cosmic Ray Facts 1- High energy charged particles. 2- Travel at nearly the speed of light. 3- Strike the Earth from all directions.

Cosmic Rays continually bombard the Earth. The highest energy cosmic rays measured to date have energy of about 1020 eV, equivalent to the kinetic energy of a baseball traveling at about 100 mph! Cosmic Rays continually bombard the Earth. In fact, about 100,000 cosmic rays (muons) will pass through a person, e.g. YOU, every hour!

Q: What’s an electron-volt (eV) ? (A: An energy unit) Giga = 1 Billion or 109 +++++++++++++++++++++++ - Tera = 1 Trillion or or 1000 Billion or 1012 Energy = 1.5 eV Electron accelerates in electric field 1.5 V AA battery - - electron - - - - - - - - - - - - - - - - - - - - - 1 GeV = 1 Giga eV = 109 eV 1 TeV = 1 Tera eV = 1012 eV

Primary Cosmic Ray Composition They include essentially all of the elements in the periodic table. About 89% of Cosmic rays are hydrogen (single protons), 9% Helium (He) nuclei, and about 1% heavier nuclei - in fact, all of the elements in the periodic table . Cosmic rays for the most part are fully ionized atoms, i.e. bare nuclei.

A more detailed view: Relative Abundances of the elements in cosmic rays observed at the top of the Earth’s atmosphere compared with the Solar System abundances, both given relative to silicon (=100%) (Simpson 1983) Solid line: Cosmic ray abundances [%] Dashed line: Solar system abundances

Cosmic ray energy spectrum Fairly similar shapes Max. around a few 100 MeV/nucleon Steeply falling spectra

Where are Cosmic Rays Coming from? 1- Galactic Cosmic Rays (GCRs) These Cosmic Rays originate in sources outside the solar system but inside the Milky Way Galaxy. Most GCRs are probably accelerated in the blast waves of supernovae remnants. This doesn’t mean that a supernova explosion itself gets the particles up to these speeds, but the remnants of the explosions, i.e. expanding clouds of gas and associated magnetic fields can last for thousands of years, and can accelerate Cosmic Rays. Most GCRs have energies between 100 MeV (0.43 c) and 10 GeV (0.996 c). Bouncing back and fourth in the magnetic field of the remnant lets particles gain energy and become Cosmic Rays. Eventually they build up enough speed to escape to the Galaxy.

Cosmic Ray Particles coming from outside galaxies passing through Where are Cosmic Rays Coming from? 2 - Extra Galactic Cosmic Rays Cosmic Ray Particles coming from outside galaxies passing through the Milky Way Galaxy.

Where are Cosmic Rays Coming from? 3 - Solar Energetic Particles (SEPs, “solar wind”) The sun is one of the sources of Cosmic Rays. Nuclei and electrons are accelerated by shock waves traveling through the Corona and by magnetic energy released in Solar flares. The Solar Wind contains roughly equal numbers of electrons and protons along with heavier ions and blows continuously from the Sun at an average speed of 400 km/sec. This leads to a mass loss of 10 million tons of material from the sun every year. Typical energies are less than 10 MeV/nucleon.

What happens when a cosmic rays strikes the earth ? Atmospheric nucleus Muon

“Pi Mesons” or “Pions” (Meson: from the Greek “meso”, meaning “middle”) IF the nucleus of an atom contains many charged protons they should repel each other due to their positive charges. What is the nature of the force that holds the nucleus together ? Mesons exchange between nucleons in the nucleus produces a strong force that overcome Coulomb repulsion, but its range is only about 10-15 m. Pi meson () or simply pion is an example of a Meson (bound quark-antiquark state). Pion comes in three varieties corresponding to three charged states: +, - and 0 Pions are not stable particles, but decay: Mπ = 139.6 MeV/C2 Muons decay, too:

Muons Muons are the most numerous energetic particles at sea level. The other shower particles mostly get absorbed in the atmosphere. A Muon interacts very little with matter except by ionization. Because of this, Muons can travel large distances and commonly reach the ground. BUT: The lifetime of a muon is 2.2 μs = 2,200 ns. As they travel at the speed of light (which as you all know is ~1 ft/ns), they typically would travel 2,200 ft or 700m. How do they get to the ground ? Special Relativity to the rescue !

Relativistic Effects on Muons At relativistic speeds the lifetime of the Muons is much longer, where the rest mass = 0.1 GeV

Energy Loss & Flux of Cosmic Ray Muons: Muons lose energy at a fairly constant rate of about 2 MeV per g/cm2. The vertical depth of the atmosphere ~ 1000 g/cm2 This means that Muons will lose ~ 2 GeV to ionization before reaching the ground. However, the mean energy of Muons at sea level is still 4 GeV. Muons arrive at sea level with an average flux of about 1 muon per square centimeter per minute.

Scintillation detector An Instrument for detecting cosmic ray muons in the lab Scintillation detector 1- Plastic Scintillator Material that emits visible photons when traversed by a high-energy charged particles. This Scintillator is made of organic materials (typically aromatic compounds). These low energy photons are subsequently collected by photomultiplier tubes (“PMTs”).

Light YOU’LL SEE SOON ! 2- Photomultiplier tube (PMTs) It consists of a photocathode and a series of dynodes in an evacuated glass enclosure. Photons that strikes the photo emissive cathode emits electros due to the photoelectric effect. Instead of collecting these few electrons these are accelerated towards a series of additional electrodes called dynodes Light The dynodes are each maintained at an increasingly positive potential. The cascading effect creates 105 to 107 electrons for each photon hitting the first cathode. The amplified signal is finally collected at the anode where it can be measured. YOU’LL SEE SOON !

Summary of the Trip There are many sources for Cosmic Rays. Cosmic rays are affected by many external factors during their trip from source to the Solar system. Muons are produced in air showers initiated at the top of the atmosphere and can reach the ground where we can detect them (fairly) easily. The study of Cosmic rays is extremely useful in many areas of physics and astronomy. Cosmic Ray study is a clue to understanding the composition of the Universe.

Thank you ! Questions ?!

Electromagnetic Processes in Cosmic Ray Air Showers Collisions of cosmic ray nuclei and atmospheric nuclei produces also gamma rays e+e- Pair Production: Creation of two electrons, one negative and the other positive (positron), from a pulse of electromagnetic energy (gamma ray) traveling through matter. This is one of the principal ways in which high energy gamma rays are absorbed in matter. For the pair production to occur the photon energy must be at least equivalent to the mass of two electrons, i.e. 1.02 MeV because the mass of a single electron is 0.51 MeV.

Supernova Explosions A supernova can release more energy in ten seconds than our Sun can produce in 10,000,000,000 years. One of the most energetic events known in the Galaxy. It occurs at the end of a star’s lifetime, when its nuclear fuel is exhausted and it is no longer supported by the release of nuclear energy. When the star is particularly massive, then its core will collapse and in so doing will release a huge amount of energy. This will cause a blast wave that ejects the star’s envelop into interstellar space. Many supernovae have been seen in nearby galaxies, they are relatively rare events in our own Milky Way Galaxy.

Solar Flares Tremendous explosion on the surface of the Sun It occurs when magnetic energy that has built up in the solar atmosphere is suddenly released Radiation are emitted from Radio waves at the long wavelength end through optical emission to x –rays and gamma rays at the short wavelength end. As the magnetic energy is being released, particles, including electrons, protons and heavy nuclei are heated and accelerated in the solar atmosphere. The energy released is on the order 1027 erg /sec or more. -> Joules ! This amount of energy is equivalent to 100 megaton hydrogen bombs exploding at the same time or ten million times greater than energy released from a volcanic explosion.

The maximum energy reached in such an event is 10 to 100 MeV; occasionally energies reach 1 GeV (once a year) and 10 GeV once a decade. Solar flares have a direct effect on Earth’s atmosphere, as the intense radiation can reach Earth in 8 minutes and the Earth’s upper atmosphere becomes more ionized. This can disturb long distance radio signals and Satellite electronic components. From a satellite