Lockyer’s sketch of his “evolutionary” stellar classification system Lockyer’s laboratory spectra from electric arcs and (higher temperature) sparks, showing.

Slides:



Advertisements
Similar presentations
Black Body Radiation Physics 105 Goderya. Need for Quantum Physics Classical mechanics and relativity cannot explain Blackbody Radiation –The electromagnetic.
Advertisements

Susan CartwrightOur Evolving Universe1 The Deaths of Stars n What happens to stars when the helium runs out? l l do they simply fade into oblivion? l l.
By Danny, Tiffany, and Connor.  A “star” is a massive, luminous ball of plasma held together by gravity.  A star forms as a collapsing cloud of material.
Good Afternoon! Please get your eInstruction remote and notebook.
Stephen C.-Y. Ng McGill University. Outline Why study supernova? What is a supernova? Why does it explode? The aftermaths --- Supernova remnants Will.
Review for Quiz 2. Outline of Part 2 Properties of Stars  Distances, luminosities, spectral types, temperatures, sizes  Binary stars, methods of estimating.
Supernovae Supernova Remnants Gamma-Ray Bursts. Summary of Post-Main-Sequence Evolution of Stars M > 8 M sun M < 4 M sun Subsequent ignition of nuclear.
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.
The Fate of Massive Stars Post Main-Sequence Evolution of Massive Stars The Classification of Supernovae Core-Collapse Supernovae Gamma Ray Bursts Cosmic.
Chapter A. Star Size Mass – the mass of a star determines the size, temperature, and brightness of the star. - The greater the mass, the greater.
A Star is Born Photo in 1995 of the Orion Nebula..
Supernova. Explosions Stars may explode cataclysmically. –Large energy release (10 3 – 10 6 L  ) –Short time period (few days) These explosions used.
Stars and the HR Diagram Dr. Matt Penn National Solar Observatory
Announcements Exam 3 is Monday May 5 at the usual class time,. Will cover Chapters 8 & 9. Sample questions are posted. Observing nights this week Tuesday,
The Lives of Stars Chapter 12. Life on Main-Sequence Zero-Age Main Sequence (ZAMS) –main sequence location where stars are born Bottom/left edge of main.

Spectrum of Sun. stellar spectra The Hertzsprung- Russel diagram a.k.a. HR diagram Vertical axis: L * Horiz. axis: T s * color of the star.
Lecture 15PHYS1005 – 2003/4 Lecture 16: Stellar Structure and Evolution – I Objectives: Understand energy transport in stars Examine their internal structure.
Wavelength flux Spectral energy distributions of bright stars can be used to derive effective temperatures Ay 123 Lecture I - Physical Properties.
Announcements Exam Grades Wednesday March 31 Angel Grade update Friday April 2 Star Assignment 6, due Wednesday March 31 ÜDo Angel quiz,
X-ray Observations of Solitary Neutron Stars an adventure to understand the structure and evolution of neutron stars 國立清華大學物理系與天文所 張祥光.
stellar spectra The Hertzsprung- Russel diagram a.k.a. HR diagram Vertical axis: L * Horiz. axis: T s * color of the star.
Place the following images in a sequence to represent the life cycle of a mid-sized star: 1, 2, 10, 14, 19, 21, – Hubble Optical Image.
Intro NASA's Chandra X-ray Observatory Exploring the X-ray Universe 2006.
CHARACTERISTICS OF STARS. A star is a ball of gas that gives off a tremendous amount of electromagnetic radiation. The energy comes from a process called.
Science Olympiad.  Description: Students will demonstrate an understanding of the basic concepts of mathematics and physics relating to stellar evolution.
10.7 Stellar processes and Stellar Evolution William Scaruffi.
Stars Star field taken with Hubble Space Telescope.
Ch. 11: The Deaths and Remnants of Stars (part a) The evolution of intermediate-mass stars. Planetary nebulae and the formation of white dwarf stars. Supernova.
The birth, life, and death of stars By Nigel Sangster
What is a star? A cloud of gas and plasma, mainly hydrogen and helium
Black holes: do they exist?
Fusion, Explosions, and the Search for Supernova Remnants Crystal Brogan (NRAO)
Supernovae and Gamma-Ray Bursts. Summary of Post-Main-Sequence Evolution of Stars M > 8 M sun M < 4 M sun Subsequent ignition of nuclear reactions involving.
Inferring Stellar Masses: Binary Systems More than 50 % of all stars are part of multiple systems. a) Visual Binaries: Both components observed directly.
The Life Cycle of Stars “protostar” The Life Cycle of Stars “protostar” “Main Sequence” (longest phase in a star’s cycle.
Dusty disks in evolved stars?
SUPERNOVA! SN 1994D in NGC 4526, NASA / ESA / Hubble Key Project Team / High-Z Supernova Search Team
Hertzsprung Russell (HR) Diagram Spectral Types: Proxy for T eff Or surface temperature Our Sun: 5,700 deg Kelvin Or about 10,000 F O B A F G K M L T.
10.7 Stellar processes and Stellar Evolution William Scaruffi.
YSS - Intro. to Observational Astrophysics (ASTR 205). Class #10 The Bizarre Stellar Graveyard (Chapter 13) Professor: José Maza July 3, 2012 Professor:
PWV LIGHT §Radio Waves §Microwaves §Infrared Light §Visible Light §Ultraviolet Waves §X-Ray Waves §Gamma Waves.
Stars, galaxies and planets Dept. of Physics, Bangalore University Bangalore B. A. Kagali.
7 - Stellar Evolution-II. Surface abundances vs. time and mass loss time What’s at the surface.
Nebula Images. Nebula.
Review: Which of the following element is the main constituent of a star? a.Hydrogenc. nitrogen b.neond. oxygen Answer: hydrogen.
Lower Limit to Stellar Masses >/= 0.08 Msun Substellar objects – Brown Dwarfs.
Stars Star field taken with Hubble Space Telescope.
BEYOND OUR SOLAR SYSTEM CHAPTER 25 Part II. INTERSTELLAR MATTER NEBULA BRIGHT NEBULAE EMISSION NEBULA REFLECTION NEBULA SUPERNOVA REMANTS DARK NEBULAE.
Stars and the HR Diagram Dr. Matt Penn National Solar Observatory.
CSI in SNRs You-Hua Chu Inst of Astron and Astroph
Our Cosmos.
Stellar Cycles Place the following images in a sequence to represent the life cycle of a mid-sized star: 1, 2, 10, 14, 19, 21,
NOTES: Spectral Class (Color-Temperature Class):
Chapter 12 Supernova Remnant
Made mostly of hydrogen
The Hertzsprung-Russell Diagram (a.k.a. H-R Diagram)
Earth and Space Science
From Birth to Death (Dust to Dust)
Atomic gas Molecular clouds
Middleweight Stars 4-12 solar masses.
The lifecycles of stars
Composition of Stars Classify stars by their color, size, and brightness. Other properties of stars are chemical composition and mass. Color and Temperature.
Stars Expectations: D2.3, D2.5,.
Classifying Stars Stars are classified by 3 Main Characteristics:
The Great Orion Nebula Star Formation Region
The Hertzsprung-Russell Diagram (a.k.a. H-R Diagram)
The lifecycles of stars
Unit 7 Vocabulary.
The Hertzsprung-Russell Diagram (a.k.a. H-R Diagram)
Presentation transcript:

Lockyer’s sketch of his “evolutionary” stellar classification system Lockyer’s laboratory spectra from electric arcs and (higher temperature) sparks, showing “proto-elements” Astrophysics: stars

Hertzsprung Russell

Astrophysics: stars HR diagram from binary star data, Redman, MNRAS 88 (1928) 718, and sketch of giant-and-dwarf evolution from Eddington 1926

Astrophysics: stars

Astrophysics: astrochemistry

Astrophysics: fusion

Astrophysics: nucleosynthesis

Astrophysics: stellar remnants Sirius B: faint in optical, but bright in X rays! The Crab Nebula and its pulsar (SNR 1054) HST image of Eskimo planetary nebula

Astrophysics: stellar remnants The presumed black-hole binary Cygnus X-1 seen in radio emission (Gallo et al., Nature 436 (2005) )

Astrophysics: stellar evolution Evolution of approximately solar-mass star in 1958 and today

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

© 2025 SlidePlayer.com. Inc. All rights reserved.