A pulsar is a supernova remnant which is a super dense, rapidly spinning neutron star which emits dipole electromagnetic radiation and features a strong.

Slides:



Advertisements
Similar presentations
White Dwarf Stars Low mass stars are unable to reach high enough temperatures to ignite elements heavier than carbon in their core become white dwarfs.
Advertisements

1 Stellar Remnants White Dwarfs, Neutron Stars & Black Holes These objects normally emit light only due to their very high temperatures. Normally nuclear.
Lecture 26: The Bizarre Stellar Graveyard: White Dwarfs and Neutron Stars.
Copyright © 2010 Pearson Education, Inc. Chapter 13 Neutron Stars.
Stellar Deaths II Neutron Stars and Black Holes 17.
Neutron Stars and Black Holes Please press “1” to test your transmitter.
Chapter 13 The Bizarre Stellar Graveyard White Dwarfs... n...are stellar remnants for low-mass stars. n...are found in the centers of planetary nebula.
Boom! Within 0.25s core is neutrons with radius 20 km and super-nuclear density Very little light can escape, energy carried off by neutrinos. Power emitted.
The Discovery of the Neutron Star The Neutron Predicted by Ernest Rutherford in 1920 Experimentally discovered by James Chadwick in 1932.
Neutron Stars and Black Holes
Neutron Stars Chandrasekhar limit on white dwarf mass Supernova explosions –Formation of elements (R, S process) –Neutron stars –Pulsars Formation of X-Ray.
 When found in stars between 8 and 25x M sun, what happens to the core?  Cores are stopped by the outer layers of the star  Cores recontract and remain.
Copyright © The McGraw-Hill Companies, Inc. Permission required for reproduction or display 1 Announcements Homework #10: Chp.14: Prob 1, 3 Chp. 15: Thought.
Neutron Stars and Pulsars Marcus Shinbo Melissa Onishi Astronomy Pd. 3 18, April, 2011.
White Dwarfs and Neutron Stars White dwarfs –Degenerate gases –Mass versus radius relation Neutron stars –Mass versus radius relation –Pulsars, magnetars,
Supernova and Neutron Stars
Compact Objects Astronomy 315 Professor Lee Carkner Lecture 15.
10 Black Holes and Neutron Stars Dead Stars Copyright – A. Hobart.
This set of slides This set of slides covers the supernova of white dwarf stars and the late-in-life evolution and death of massive stars, stars > 8 solar.
Question The pressure that prevents the gravitational collapse of white dwarfs is a result of ______.  A) Conservation of energy  B) Conservation of.
Compact Objects Astronomy 315 Professor Lee Carkner Lecture 15.
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.
 Pulsars are just a kind of neutron stars so it’s essential to get a grip of these first.  The stars that come into being at the end of a massive.
High mass endings. Answers from you folks on yesterday’s quiz. Differences between a dying low mass vs. a dying high mass star: No He flash in a high.
O n t h e T r a c k o f M o d e r n P h y s i c s Crab Nebula testifies the Supernova explosion in 1054AD, noted in Europe, China and by Indians in New.
PSR J1400 – 1410 Jessica Pal Rowan County Senior High School Introduction Data Analysis Summary Acknowledgements Results A pulsar is a rapidly rotating.
1 Stellar Remnants White Dwarfs, Neutron Stars & Black Holes These objects normally emit light only due to their very high temperatures. Normally nuclear.
Copyright © 2010 Pearson Education, Inc. Neutron Stars and Black Holes Unit 9.
Planetary Environment Around a Pulsar David Dunkum, Jacob Houdyschell, Caleb Houdyschell, and Abigail Chaffins Spring Valley High School Huntington, WV.
Neutron Stars Pulsars. Neutron Stars In 1967, it was believed (by some) that the first intelligent signal from outer space had been discovered. A graduate.
JP ©1 2 3 Stars are born, grow up, mature, and die. A star’s mass determines its lifepath. Let M S = mass of the Sun = ONE SOLAR MASS Stellar Evolution.
The “Crab Nebula”: the most famous supernova remnant. distance  2000 pc diameter  3 pc.
High Mass Stellar Evolution Astrophysics Lesson 13.
Who discovered the first pulsar? Jocelyn Bell Pulsars spin fast due to what physics concept?
After the Supernova: Pulsars Melissa Anholm University of Wisconsin-Milwaukee 29 September, 2008.
Chapter 12 Space Exploration. Section 12.1 page 428 Explaining the Early Universe GALAXY – collection of stars, planets, gas and dust held together by.
Neutron Star. Gravitational Crush The balance point to maintain degenerate matter is 1.4 M . When the mass of the core is greater than 1.4 M , electrons.
Death of Stars II Physics 113 Goderya Chapter(s): 14
Stellar Corpses and Other Space Oddities
Copyright © 2010 Pearson Education, Inc. Chapter 13 Neutron Stars and Black Holes Lecture Outline.
带强磁场奇异星的 中微子发射率 刘学文 指导老师：郑小平 华中师范大学物理科学与技术学院. Pulsar In 1967 at Cambridge University, Jocelyn Bell observed a strange radio pulse that had a regular period.
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.
Neutron Stars & Black Holes. Neutron Stars and Black Holes I. Neutron Stars A. Remnant from the collapse of a _________. B. During the core collapse of.
4.3 Energy and Conservation Laws. Kinetic energy is the energy associated with motion. KE = ½ mv 2 m = mass, v = velocity Types of Energy – Kinetic Energy.
Supernovas Neutron Stars and Black Holes
28-1 A Closer Look at Light A. What is Light?
Announcements Grades for the third exam should be available on WebCT by noon Tuesday. Observing this week and next week counts on the third exam. Please.
Black holes, neutron stars and binary star systems
Neutron Stars and Black Holes
The Fate of High-Mass Stars
Incredible Shrinking Stars The End States of Stars.
Ch Exploding Stars & Black Holes
Will the PowerPoint presentations ever end? No.
The Legacy of Supernovae
The Sun The sun is made up of no solids or liquids
Stars.
Pulsar Search Collaboratory
Life Cycle of Stars Lesson 4, Unit 2.
Middleweight Stars 4-12 solar masses.
The Bizarre Stellar Graveyard
White Dwarfs and Neutron Stars
Neutron Stars In a type II supernova the shock wave does not start at the very center of the collapsing core. After the explosion, the inner ball of neutrons.
White Dwarf Stars Low mass stars are unable to reach high enough temperatures to ignite elements heavier than carbon in their core become white dwarfs.
Evolution of the Solar System
Chapter 13 Neutron Stars and Black Holes
The Death of a Star.
Final states of a star: 1. White Dwarf
Section 3 – pg 608 Lives of Stars
The Death of a Star.
Presentation transcript:

A pulsar is a supernova remnant which is a super dense, rapidly spinning neutron star which emits dipole electromagnetic radiation and features a strong magnetic and gravitational field and also high space velocity.

PULSAR PROPERTIES: High Space Velocity High Space Velocity Rapid Spin Rate Rapid Spin Rate Super Dense Super Dense Strong Gravitational Field Strong Gravitational Field Strong Magnetic Field Strong Magnetic Field

Jocelyn Bell

“Little Green Men” Theory

Chandrasekhar Mass Limit 1.4 solar masses = × kilograms

Pulsar Property #1. High Space Velocity

Over 1500 km/s High Space Velocity

Terms to Know

Parallax

Watch Video: The Doppler Effect: what does motion do to waves?

Over 1500 km/s High Space Velocity

Pulsar Property #2. Rapid Spin Rate

Diameter = ~20km

L = mvrv = L/(mr) Rapid Spin Rate Conservation of Angular Momentum Largest ~700Hz

Pulsar Property #3-#4. Super Dense & Strong Gravitational Field

D= M/V, V = (4/3)πr 3 Super Dense, Strong Gravitational Field

Pulsar Property #5. Strong Magnetic Field

extremely powerful magnetic fields of Tesla

PULSAR PROPERTIES: High Space Velocity High Space Velocity Rapid Spin Rate Rapid Spin Rate Super Dense Super Dense Strong Gravitational Field Strong Gravitational Field Strong Magnetic Field Strong Magnetic Field

Watch: Atoms As Big As Mountains — Neutron Stars Explained

Feedback: Privacy Policy Feedback
Do Not Sell My Personal Information
About project: SlidePlayer Terms of Service

© 2024 SlidePlayer.com Inc. All rights reserved.