Supernovae and Neutron Stars

Slides:



Advertisements
Similar presentations
What is the fate of the sun and other stars??
Advertisements

Notes 30.2 Stellar Evolution
Stellar Death Astronomy 315 Professor Lee Carkner Lecture 14 “I am glad we do not have to try to kill the stars. … Imagine if a man each day should have.
1 Stellar Remnants White Dwarfs, Neutron Stars & Black Holes These objects normally emit light only due to their very high temperatures. Normally nuclear.
Stellar Evolution Describe how a protostar becomes a star.
End States Read Your Textbook: Foundations of Astronomy
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.
KEY differences Type 1: The explosion results from sudden fusion on its surface. Type 2: The explosion results from collapse of the core. Type 1: The.
Objectives Determine the effect of mass on a star’s evolution.
Neutron Stars and Black Holes
Chapter 23 Neutron Stars. Neutron stars Inspired by the discovery of the Neutron in 1932, two Astronomers Fritz Zwicky (Clatech) and Walter Baade (Mount.
ASTR 113 – 003 Spring 2006 Lecture 07 March 8, 2006 Review (Ch4-5): the Foundation Galaxy (Ch 25-27) Cosmology (Ch28-39) Introduction To Modern Astronomy.
Copyright © The McGraw-Hill Companies, Inc. Permission required for reproduction or display 1 Announcements Homework #10: Chp.14: Prob 1, 3 Chp. 15: Thought.
The Evolution of Stars - stars evolve in stages over billions of years 1.Nebula -interstellar clouds of gas and dust undergo gravitational collapse and.
Dead Stars.
White Dwarfs and Neutron Stars White dwarfs –Degenerate gases –Mass versus radius relation Neutron stars –Mass versus radius relation –Pulsars, magnetars,
Earth Science 25.2B : Stellar Evolution
10 Black Holes and Neutron Stars Dead Stars Copyright – A. Hobart.
Chapter 12: Stellar Evolution Stars more massive than the Sun The evolution of all stars is basically the same in the beginning. Hydrogen burning leads.
Announcements Pick up graded homework (projects, tests still in progress) Transit of Mercury (crossing in front of Sun), this afternoon, roughly noon-5:00.
Stellar End-States… J. B. S. Haldane (1892 – 1964) from Possible Worlds, 1927 Now, my suspicion is that the Universe is not only queerer than we suppose,
1 Stellar Remnants White Dwarfs, Neutron Stars & Black Holes These objects normally emit light only due to their very high temperatures. Normally nuclear.
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 Lives and Deaths of Stars A presentation of the Universe in the Parks program The University of Wisconsin-Madison Department of Astronomy.
LIFE CYCLE OF A STAR.
The Evolution of Stars.
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
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.
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.
Lower Limit to Stellar Masses >/= 0.08 Msun Substellar objects – Brown Dwarfs.
Chapter 13 Post Main Sequence Stellar Evolution. The Sun.
Chapter 10 The Bizarre Stellar Graveyard. The Products of Star Death White Dwarfs Neutron Stars Black Holes.
Topic: The Life Cycle of Stars PSSA: D/S8.D.3.1.
Chapter 11 The Death of High Mass Stars
Stellar Evolution. Structure Mass governs a star’s temperature, luminosity, and diameter Hydrostatic Equilibrium – the balance between gravity squeezing.
Stars, Galaxies, and the Universe Section 2 Section 2: Stellar Evolution Preview Objectives Classifying Stars Star Formation The Main-Sequence Stage Leaving.
Lives of Stars.
Announcements Quiz 7 due tonight, practice problems in Problem Sets 7A, 7B Approximate schedule for this week: Today: Finish Chapter 12, Chapter 13 Remainder.
Ch 12--Life Death of Stars
Star Formation - 6 (Chapter 5 – Universe).
1 Death of a Large Mass Star
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.
Our Cosmos.
Option D2: Life Cycle of Stars
The Fate of High-Mass Stars
Incredible Shrinking Stars The End States of Stars.
Nicholas Kellogg & Annessa strickland
Neutron Stars and Pulsars
Radio Objects.
25.2 – Stellar Evolution – Part II
Earth Science 25.2B : Stellar Evolution
Middleweight Stars 4-12 solar masses.
The Bizarre Stellar Graveyard
The lifecycles of stars
White Dwarfs and Neutron Stars
Death of stars Final evolution of the Sun
Supernova.
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.
The burnt-out cores of low mass, post-main sequence stars
The Evolution of Massive Stars
Evolution of the Solar System
You can often predict how a baby will look as an adult by looking at other family members. Astronomers observe stars of different ages to infer how stars.
The Death of a Star.
Final states of a star: 1. White Dwarf
Lives of Stars.
The lifecycles of stars
The Death of a Star.
Presentation transcript:

Supernovae and Neutron Stars

Specific textbook sections Evolution after the main sequence: Section 19.4 White dwarf stars: Section 20.1 Supernovae and neutron stars: Section 20.2

Core collapse of a massive star has two consequences Massive explosion (1044 Joules) Production of a neutron star

Formation of a neutron star from stellar core As core collapses, matter becomes compressed Electrons and protons forced together e+p > n + nu (neutronization) Core of the becomes a neutron fluid Neutronization produces a burst of neutrinos Neutron fluid in core becomes degenerate and rigid

The physics of a self-gravitating neutron blob (neutron star) Radius versus mass relation for neutron star Notice size of neutron star Masses extend above Chandrasekhar limit

Theoretical prediction of the existence of a neutron star The remnant after the explosion of a massive star An object having the mass of the Sun (or more) but in an object with the diameter of Iowa City! An equivalent to the Chandrasekhar mass (largest possible mass of a neutron star) Do they exist?

The problem of the Crab Nebula…the remnant of the supernova of 1054 AD Even today,something is powering the Crab Nebula, causing it to shine at x-rays

1968: The Discovery of Pulsars: Rotating Neutron Stars http://www.jb.man.ac.uk/~pulsar/Education/Sounds/sounds.html

Highly regular pulse properties PSR0329+54, P=0.714519699726 sec Pulsar properties Highly regular pulse properties PSR0329+54, P=0.714519699726 sec PSR1633+24, P=0.4905065128003 sec What in nature could provide such a perfect clock? Demo

Pulsars as rotating neutron stars demo

The Crab Nebula Pulsar http://chandra.harvard.edu/photo/2002/0052/movies.html

How many pulsars (neutron stars) are there in the sky? http://www.atnf.csiro.au/research/pulsar/psrcat

Neutron stars: from exotica to numerous astronomical objects

A final mystery…pulsar masses are nearly all AT the Chandrasekhar Limit

Periods and Period Derivatives for Pulsars

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

© 2024 SlidePlayer.com. Inc. All rights reserved.