Observations of Supernova 1987a R. D. Gehrz University of MInnesota.

Slides:



Advertisements
Similar presentations
Evolution of Stars.
Advertisements

Life Cycle of Stars. Omega / Swan Nebula (M17) Stars are born from great clouds of gas and dust called Stars are born from great clouds of gas and dust.
Lives of Stars for Website. Life of Stars Nebula- a large cloud of gas and dust spread out in an immense volume. A star on the other hand is made of a.
The Life Cycle of a Star.
LECTURE 19, NOVEMBER 4, 2010 ASTR 101, SECTION 3 INSTRUCTOR, JACK BRANDT 1ASTR 101-3, FALL 2010.
Objectives Determine the effect of mass on a star’s evolution.
The Evolution of Stars - stars evolve in stages over billions of years 1.Nebula -interstellar clouds of gas and dust undergo gravitational collapse and.
Supernova and Neutron Stars
Astronomy 100 Tuesday, Thursday 2:30 - 3:45 pm Tom Burbine
Giant clouds of gas and dust The birthplace of stars! Nebula.
What is the Lifecycle of a Star? Chapter Stars form when a nebula contracts due to gravity and heats up (see notes on formation of the solar system).
NOT THOSE TYPES OF STARS! LIFE CYCLE OF STARS WHAT IS A STAR? Star = ball of plasma undergoing nuclear fusion. Stars give off large amounts of energy.
THE LIFE CYCLES OF STARS. In a group, create a theory that explains: (a)The origin of stars Where do they come from? (b)The death of stars Why do stars.
Key Ideas How are stars formed?
Life Cycle of Stars. Stars are born in Nebulae Vast clouds of gas and dust Composed mostly of hydrogen and helium Some cosmic event triggers the collapse.
Birth and Life of a Star What is a star? A star is a really hot ball of gas, with hydrogen fusing into helium at its core. Stars spend the majority of.
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 Life Cycles of Stars
Charles Hakes Fort Lewis College1. Charles Hakes Fort Lewis College2.
High Mass Stellar Evolution Astrophysics Lesson 13.
Sun, Moon, Earth, What kind of life cycle does a star have?
A cloud of gas and dust collapses due to gravity.
Bret Betz, Nick Jones, Calvin Schildknecht
Ch Stellar Evolution. Nebula—a cloud of dust and gas. 70% Hydrogen, 28% Helium, 2% heavier elements. Gravity pulls the nebula together; it spins.
Stars By: Mary Aragon Theory of Relativity. What are stars?  Enormous balls of gas  Made mostly of hydrogen and helium  Constant nuclear process (fusion)
Astronomy 1020-H Stellar Astronomy Spring_2015 Day-36.
Life Cycle of Stars Nebula hundreds of light years in size contract under gravity
The "Fingerprints" of Stars The best tool we have for studying a star's light is the star's spectrum. A spectrum (the plural is "spectra") of a star is.
Life Cycle of Stars Birth Place of Stars:
Star Formation. 1) Nebula  Cloud of interstellar gas and dust  Collapses due to its own gravity  Begins Star Formation.
Unit 1 Lesson 3 The Life Cycle of Stars
Unit 1: Space The Study of the Universe.  Mass governs a star’s temperature, luminosity, and diameter.  Mass Effects:  The more massive the star, the.
The life cycle of stars from birth to death
Life Cycle of Stars Mr. Weaver.
The Sun-Earth-Moon System. What is the moon? The moon is a natural satellite of Earth This means that the moon orbits Earth.
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.
The Star Cycle. Birth Stars begin in a DARK NEBULA (cloud of gas and dust)… aka the STELLAR NURSERY The nebula begins to contract due to gravity in.
Announcements Exam 3 is scheduled for Wednesday April 8. Will be pushed back to Monday April 13 Tentatively will cover the rest of Chapter 4, all of Chapters.
E5 stellar processes and stellar evolution (HL only)
Chapter 13 Post Main Sequence Stellar Evolution. The Sun.
Topic: The Life Cycle of Stars PSSA: D/S8.D.3.1.
By: Chelsea Incognito Astronomy Research Project Stars and How They Form.
THE LIFE CYCLE OF A STAR Objective: I will compare and contrast the life cycle of stars based on their mass.
Stellar Evolution From Nebula to Neutron Star. Basic Structure The more massive the star the hotter it is, the hotter it is the brighter it burns Mass.
Stellar Evolution Continued…. White Dwarfs Most of the fuel for fusion is used up Giant collapses because core can’t support weight of outer layers any.
Stellar Evolution. Structure Mass governs a star’s temperature, luminosity, and diameter Hydrostatic Equilibrium – the balance between gravity squeezing.
Unit 1 Lesson 3 The Life Cycle of Stars
12-2 Notes How Stars Shine Chapter 12, Lesson 2.
Stellar Evolution Chapters 16, 17 & 18.
Section 3: Stellar Evolution
Stars: Old Age, Death, and New Life
The Life Cycle of a Star.
The Life Cycle of a Star.
Main Sequence Stars Once the star has ignited, it becomes a main sequence star. Main Sequence stars fuse hydrogen to form helium, releasing enormous.
Evolution of Stars Lesson 3 page 816.
Middleweight Stars 4-12 solar masses.
The lifecycles of stars
The Life Cycle of a Star.
Lifecycle of a star - formation
The Life Cycle of a Star.
The Life Cycle of a Star.
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.
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.
Death of Stars (for high mass stars)
STELLAR EVOLUTION. STELLAR EVOLUTION What is a star? A star is a huge ball of hot gas, held together by its own gravity. Most of the gas is hydrogen.
Stellar Evolution for high mass stars
The lifecycles of stars
The Life Cycle of a Star.
Presentation transcript:

Observations of Supernova 1987a R. D. Gehrz University of MInnesota

Theories Confirmed by Observations of Supernova 1987a Neutrino pulse: right size and duration Infrared line emission and visual light curve decay rate: reveal formation of heavyelements Spectrum of precursor star: blue supergiant Thermal IR emission: formation of dust grains Light echoes: illuminated shells ejected by the precursor star and also illuminated a “phantom” nebula caused by reflections of the explosion off interstellar clouds Central remnant: Is a pulsar or black hole left over in the center of the system?

The Supernova Explosion The core collapses until the neutrons touch: The collapse stops because of neutron degeneracy pressure A shock wave rebounds through the outer layers of the star: some of the neutrons fly out through the ejecta and make heavy elements by 56 Fe + Nn  56+N X The core continues to collapse: it either halts as a stable neutron star or becomes a black hole depending upon the mass remaining in the core after the rebound

Core Collapse of a Massive Star Formation of the iron core: nuclei lighter than iron give off energy when they are formed by fusion, nuclei heavier than iron absorb energy when they are formed by fusion. Iron is on the dividing line between these processes. Photo-disintegration of iron and helium:  + 56 Fe  13 4 He + 4n and  + 4 He  4n Neutronization: p + + e -  n + Formation of a neutron star or a black hole: A neutron star forms if M c < 1.44 Solar Masses (the Chandrasekhar mass limit) A black hole forms if M exceeds M c R Black Hole = 2GM/c 2

The Escape Velocity Derivation When an object is thrown up into the air there is a battle between the object's kinetic energy and the gravitational pull on the object (its gravitational potential energy). If our object is to escape the gravitational pull of the Earth, its kinetic energy must balance the gravitational force acting upon it. The kinetic energy = ½ mv 2, where m is the mass of the object and v is its velocity. The gravitational potential energy of an object = GmM/r, where G is the gravitational constant, m is the mass of the object, M is the mass of the Earth and r is the Earth's radius. For a balance between kinetic energy and gravitational potential energy we must have: ½ mv 2 = GmM/r _______ Doing simple algebra, we obtain our escape velocity formula: V esc = √ 2MG/r

The Black Hole Equation Recall the escape velocity formula: ________ V esc = √ 2MG/r To trap light, we must have V esc = c Therefore: R Black Hole = 2GM/c 2

Black Hole’s of Various Masses R Black Hole = 2GM/c 2 : For M = 1M sun, R Black Hole = 3 km For M = 10M sun, R Black Hole = 30 km For M = 10M earth, R Black Hole = 1 cm For M = 10 6 M sun, R Black Hole = 3x10 6 km For M = 10 8 M sun, R Black Hole = 3x10 8 km

Neutron Stars For a star spinning at the limit of rotational stability: