after the supernova: pulsars melissa anholm university of wisconsin-milwaukee 29 september, 2008

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QuickTime™ and a decompressor are needed to see this picture. After the Supernova: After the Supernova: Pulsars Pulsars Melissa Anholm Melissa Anholm University of Wisconsin- University of Wisconsin- Milwaukee Milwaukee 29 September, 2008 29 September, 2008

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Page 1: After the Supernova: Pulsars Melissa Anholm University of Wisconsin-Milwaukee 29 September, 2008

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After the Supernova:After the Supernova:PulsarsPulsarsAfter the Supernova:After the Supernova:PulsarsPulsars

Melissa AnholmMelissa Anholm

University of Wisconsin-MilwaukeeUniversity of Wisconsin-Milwaukee

29 September, 200829 September, 2008

Page 2: After the Supernova: Pulsars Melissa Anholm University of Wisconsin-Milwaukee 29 September, 2008

OutlineOutlineOutlineOutline

• Properties of Neutron Stars• Large Magnetic Field

• Rapid Rotation

• Origin of the Pulsing Effect• Motion in a Magnetic Field

• Light Emission

• The Lighthouse Effect

Page 3: After the Supernova: Pulsars Melissa Anholm University of Wisconsin-Milwaukee 29 September, 2008

A Typical A Typical Neutron StarNeutron StarA Typical A Typical Neutron StarNeutron Star

• Strong Magnetic FieldStrong Magnetic Field

• Fast RotationFast Rotation

Properties of Neutron StarsProperties of Neutron Stars

Page 4: After the Supernova: Pulsars Melissa Anholm University of Wisconsin-Milwaukee 29 September, 2008

Why does it spin so fast?Why does it spin so fast?Why does it spin so fast?Why does it spin so fast?

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A typical young pulsar completes about one rotation per second.

Properties of Neutron StarsProperties of Neutron Stars

A typical star completes about one rotation every week - month.

Page 5: After the Supernova: Pulsars Melissa Anholm University of Wisconsin-Milwaukee 29 September, 2008

Magnetic Fields - Now with Magnetic Fields - Now with Lines!Lines!Magnetic Fields - Now with Magnetic Fields - Now with Lines!Lines!

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http://www.freewebs.com/ayxl/magnet.jpeg http://www.utm.edu/staff/cerkal/magnetic_files/image004.jpg

Properties of Neutron StarsProperties of Neutron Stars

Page 6: After the Supernova: Pulsars Melissa Anholm University of Wisconsin-Milwaukee 29 September, 2008

After the Collapse: Rotation and the Magnetic Field

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• Dense magnetic field lines Strong magnetic field

• Angular momentum conserved Fast rotation

• Magnetic and rotationalaxes may not be aligned.

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Properties of Neutron Stars

Page 7: After the Supernova: Pulsars Melissa Anholm University of Wisconsin-Milwaukee 29 September, 2008

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Misalignment of Magnetic and Rotational Axes - Why We Care

http://www.atnf.csiro.au/news/press/images/binary_pulsar/

All newly formed neutron stars (and some older ones, too!) produce beams of light along their magnetic poles if the axes aren’t aligned.

Origin of the Pulsing Effect

Page 8: After the Supernova: Pulsars Melissa Anholm University of Wisconsin-Milwaukee 29 September, 2008

Properties of LightProperties of Light

Origin of the Pulsing Effect

• “photon” = a particle of light• accelerating charged particles produce photons (!)

Page 9: After the Supernova: Pulsars Melissa Anholm University of Wisconsin-Milwaukee 29 September, 2008

QuickTime™ and a decompressor

are needed to see this picture.• Moving magnets produce an electric force.

• Electric currents and moving charged particles produce a magnetic force.

A Strange Connection A Strange Connection between Electricity between Electricity and Magnetismand Magnetism

http://img105.imageshack.us/img105/5114/magfield0ct.jpg

Origin of the Pulsing Effect

• Result: a moving charged particle in a magnetic field will accelerate.

Page 10: After the Supernova: Pulsars Melissa Anholm University of Wisconsin-Milwaukee 29 September, 2008

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Motion on a Large Scale Near a Rotating Magnet

http://www.atnf.csiro.au/news/press/images/binary_pulsar/

Charged particles move upward or downward (depending on the charge) at the pulsar’s rotational poles.

Origin of the Pulsing Effect

Page 11: After the Supernova: Pulsars Melissa Anholm University of Wisconsin-Milwaukee 29 September, 2008

Motion in a Magnetic FieldMotion in a Magnetic Field

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• A charged particle placed in a magnetic field will spiral around the magnetic field lines.

Origin of the Pulsing Effect

Page 12: After the Supernova: Pulsars Melissa Anholm University of Wisconsin-Milwaukee 29 September, 2008

Accelerating Accelerating A Charged A Charged

ParticleParticle QuickTime™ and a decompressor

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Synchrotron Radiation = Light

• Light is emitted in a direction perpendicular to the magnetic field.

Origin of the Pulsing Effect

Page 13: After the Supernova: Pulsars Melissa Anholm University of Wisconsin-Milwaukee 29 September, 2008

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The The Lighthouse Lighthouse EffectEffect

The The Lighthouse Lighthouse EffectEffect

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Origin of the Pulsing Effect

Page 14: After the Supernova: Pulsars Melissa Anholm University of Wisconsin-Milwaukee 29 September, 2008

Conclusions

• Pulsars are rapidly rotating neutron stars with powerful magnetic fields.

• A misalignment in the rotational and magnetic axes leads to the emission of beams of light from a pulsar’s magnetic poles.

http://www.shatters.net/forum/viewtopic.php?t=11372