25 ii 2011NASM1 Exploring the Crab Nebula with the Hubble, Chandra and Fermi Space Telescopes Roger Blandford KIPAC Stanford.

Slides:

Advertisements

Similar presentations

YSS - Intro. to Observational Astrophysics (ASTR 205). Class #10 The Bizarre Stellar Graveyard (Chapter 13) Professor: José Maza June 20, 2011 Professor:

Advertisements

How Do Astronomers Learn About the Universe?

2009 July 8 Supernova Remants and Pulsar Wind Nebulae in the Chandra Era 1 Modeling the Dynamical and Radiative Evolution of a Pulsar Wind Nebula inside.

Neutron Stars and Black Holes

X-Ray UltravioletVisibleInfraredRadio The Electromagnetic Spectrum and the Universe.

Supernova and Neutron Stars

Fundamental Issues in High Energy Astrophysics Roger Blandford KIPAC Stanford.

What is High-Energy Astrophysics? What is studied by high-energy astrophysicists: Supernovae Supernovae remnants Pulsars/magnetars Gamma-ray bursts Accreting.

Diffuse Gamma-Ray Emission Su Yang Telescopes Examples Our work.

High Energy  -rays Roger Blandford KIPAC Stanford.

Light and Telescopes Chapter 5. Radio Interferometry The Very Large Array (VLA): 27 dishes are combined to simulate a large dish of 36 km in diameter.

A Walk Through the Electromagnetic Spectrum Ken Morgan ENGR302 May 7, 2002.

Gamma-Ray Astronomy Dana Boltuch Ph. D

Microwave: The Cosmic Microwave Background (CMB). Shortly after the Big Bang, the Universe cooled enough to allow atoms to form. After this point in time,

Light as a wave in an abstract electromagnetic field, or as a stream of massless particles called photons.

A Visit to Ghost Ranch Jim Linnemann Michigan State University & Los Alamos National Laboratory June 18, 2003.

1 Gamma-Ray Astronomy with GLAST May 24, 2008 Toby Burnett WALTA meeting.

Chapter 10 – part 3 - Neutron stars and Black Holes Neutron stars.

Nebulas are made up of gas left behind by stars forming or exploding There are different classes of Nebulas The classes are: Reflection Nebulae, Emission.

Gamma-ray Astrophysics Pulsar GRB AGN SNR Radio Galaxy The very high energy  -ray sky NEPPSR 25 Aug Guy Blaylock U. of Massachusetts Many thanks.

The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

Electromagnetic Spectrum. Different forms of radiation arranged in order according to their wavelength. – Travels through space at 300,000 km/s or 186,000.

 Celestial Sphere  Imagine a sphere that surrounds our planet in which all the stars are attached. This sphere is allowed to rotate freely around the.

Nebular Astrophysics.

CHAPTER 3 (p ) Light. Only a very small range of wavelengths, 400nm to 700nm, are visible to humans. Wavelengths are very small so astronomers use.

50 announcement: next week only : office hours Tuesday 2-4.

High-Energy Astrophysics

Problems associated with Earth based observation Optical band = stars and planets and nebulae. Infrared band = low energy heat sources. Radio band = dust.

Fermi: Highlights of GeV Gamma-ray Astronomy Dave Thompson NASA GSFC On behalf of the Fermi Gamma-ray Space Telescope Large Area Telescope Collaboration.

The “Crab Nebula”: the most famous supernova remnant. distance  2000 pc diameter  3 pc.

Jacques Paul Soft Gamma-Ray Astronomy 23 January 2001 Rencontres de Moriond Les Arcs Expected Impact on VHE Phenomena Panorama in the Coming Years INTEGRAL.

Project Gamma By Wylie Ballinger and Sam Russell Visit For 100’s of free powerpoints.

ELECTROMAGENTIC RADIATION. ELECTROMAGNETIC RADIATION IS A FORM OF ENERGY. IT CAN BEHAVE AS PARTICLES OR WAVES. SOMETIMES, WE USE THE TERM “LIGHT” WHEN.

A105 Stars and Galaxies  Homework #4 due today  Telescopes  Read unit 30 for next week  News Quiz Tuesday  First Exam on Sept. 28 Today’s APODAPOD.

SOLAR FLARE A sudden, rapid, and intense variation in brightness. They occurs when magnetic energy that has built up in the solar atmosphere and is.

Discovery of  rays from Star-Forming Galaxies New class of nonthermal sources/gamma-ray galaxies (concept of temperature breaks down at high energies)

Who discovered the first pulsar? Jocelyn Bell Pulsars spin fast due to what physics concept?

Introduction to the High Energy Astrophysics Introductory lecture.

260404Astroparticle Physics1 Astroparticle Physics Key Issues Jan Kuijpers Dep. of Astrophysics/ HEFIN University of Nijmegen.

121 vii 2009LTD-13 The Low Temperature Universe Roger Blandford Stanford SLAC KIPAC.

What Channel is That?.  Visible light is a form of electromagnetic radiation.  Others include:  Radio waves  Infrared waves (heat)  Ultraviolet waves.

Death of Stars II Physics 113 Goderya Chapter(s): 14

What is Astronomy? An overview..

Diffuse Emission and Unidentified Sources

A Pulsar Wind Nebula Origin for Luminous TeV Source HESS J Joseph Gelfand (NYUAD / CCPP) Eric Gotthelf, Jules Halpern (Columbia University), Dean.

Neutron Stars When stars about five times the mass of the sun run out of fuel, their own weight compresses the material unbelievably. The protons and.

Sources emitting gamma-rays observed in the MAGIC field of view Jelena-Kristina Željeznjak , Zagreb.

1 The Stars Great Idea: The Sun and other stars use nuclear fusion reactions to convert mass into energy. Eventually, when a star’s nuclear fuel is depleted,

Satellites, Telescopes, Probes and Rovers

Telescopes and The Sky Katherine Rawlins University of Wisconsin- Madison Presented by Jim Madsen UW-RF.

Gamma-Ray Emission from Pulsars

White dwarfs cool off and grow dimmer with time. The White Dwarf Limit A white dwarf cannot be more massive than 1.4M Sun, the white dwarf limit (or Chandrasekhar.

**If you’ve missed part of your test, you need to come in before or after school to make it up. Grab your clickers!

Extreme Astrophysics the the > 10 GeV photon energy < cm wavelength > 10 8 TeV particles exist > 10 8 TeV particles exist they should.

A black hole: The ultimate space-time warp Ch. 5.4 A black hole is an accumulation of mass so dense that nothing can escape its gravitational force, not.

A fast online and trigger-less signal reconstruction Arno Gadola Physik-Institut Universität Zürich Doktorandenseminar 2009.

The Electromagnetic Spectrum and Telescopes Rose Emanuel Journey into Space Journey Museum, July 18-20, 2012.

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.

5 vii 2012Frascati1 The Crab Impact Roger Blandford Yajie Yuan KIPAC Stanford.

High Energy Observational Astrophysics. 1 Processes that emit X-rays and Gamma rays.

MAGIC Max Planck Institut fürPhzsik The MAGIC Telescope ShangYu Sun A. Boller, L. Fortson, N. Galante, D. Paneque and B. Steinke On behalf of the Fermi,

Gamma-Ray Bursts Please press “1” to test your transmitter.

Telescope Technology Types of Telescopes Hubble Telescope and NASA’s Great Observatories.

3.2 The Electromagnetic Spectrum: Beyond Visible Light

3.2 The Electromagnetic Spectrum: Beyond Visible Light

Using Telescopes to Observe Electromagnetic Radiation in Space

Types of Telescopes Dr. Charles Ophardt EDU 370.

Discussion slide- info from hq. nasa

3.2 The Electromagnetic Spectrum: Beyond Visible Light

Presentation transcript:

25 ii 2011NASM1 Exploring the Crab Nebula with the Hubble, Chandra and Fermi Space Telescopes Roger Blandford KIPAC Stanford

Anasazi Indians 25 ii 2011NASM2

Charles Messier 25 ii 2011NASM3

Sam Okoye discovers compact radio source 25 ii 2011NASM4

Franco Pacini predicts Crab Nebula Powered by Neutron Star 25 ii 2011NASM5

Jocelyn Bell Discovers Pulsars 25 ii 2011NASM6

John Bahcall ( ) 25 ii 2011NASM Astrophysicist Astronomical Leader Mentor to Young Scientists Champion of Hubble Space Telescope 7

Hubble Space Telescope 25 ii 2011NASM8

Chandra X-ray Telescope 25 ii 2011NASM9

25 ii 2011NASM10 High Energy Astronomy! VERITAS/H.E.S.S. LIGO Ice Cube eV keV MeV GeV TeV PeV EeV ZeV Cosmic Rays Gamma-Rays X X Electromagnetic waves comprise particles called Photons Cosmic rays comprise mainly Protons and Electrons Radi o

25 ii 2011NASM11 Fermi (the scientist and the telescope)

The Pulsing  -ray Sky Pulses at 1/10 th true rate 25 ii NASM

25 ii 2011NASM H.E.S.S. 13

Supernova Explosion 25 ii 2011NASM14 Supernova 1987a in Magellanic Cloud

Crab Nebula at Different Wavelengths 25 ii 2011NASM15

Optical and X-rays Combined 25 ii 2011NASM16

The Entire Spectrum 25 ii 2011NASM17 Radio Gamma Rays TeV Synchrotron Radiation Compton Scattering

Synchrotron Radiation Maximum Synchrotron Photon Energy ~ 100 MeV 25 ii NASM ~0.01 Gauss 10 keV 10 TeV

Compton Scattering 25 ii 2011NASM eV Infrared Photon 10 TeV Electron 5 TeV Electron 5 TeV Gamma-rayPhoton

Neutron Star 25 ii 2011NASM20 Wilson Mass: 1.5 suns Radius: 10 km Density: million, billion x water Rotation Rate: 30 per second Magnetic Field: 1 trillion Gauss

Crab Pulsar 25 ii 2011NASM21

25 ii 2011NASM22 Faraday’s Disk Magnet Conducting Disk Crank Voltage: 50 PetaVolts Current: 300 TeraAmps Power: 100,000 Suns

The Restless Crab Hester 25 ii NASM

Fermi Flares 25 ii NASM

Spectral Changes September Flare 4 day variation Synchrotron Radiation Compton Scattering 25 ii NASM Synchrotron Radiation Limit

Where is the Flare? 25 ii 2011NASM26 Jet Torus Pulsar

Let’s Keep Exploring the Crab Nebula 25 ii 2011NASM27 Thank You