Celestial Bodies (Mike Stroppa) - Powerpoint
... • Stars come in a variety of colours • Scientists can tell the surface temperature by the colour of the star • Red stars are cooler (Surface T 3000 C) • Blue stars are hotter (Surface T 20000 C) • The Sun is a yellow star (6000 C) ...
... • Stars come in a variety of colours • Scientists can tell the surface temperature by the colour of the star • Red stars are cooler (Surface T 3000 C) • Blue stars are hotter (Surface T 20000 C) • The Sun is a yellow star (6000 C) ...
ppt
... How can we test theories of star evolution? • Binaries help, because one can get mass so that theories can be tested • But stars change so slowly, it is impossible to test theories by watching just one star move through phases • Fortunately, there are 1011 stars in our Galaxy, all with a range of ma ...
... How can we test theories of star evolution? • Binaries help, because one can get mass so that theories can be tested • But stars change so slowly, it is impossible to test theories by watching just one star move through phases • Fortunately, there are 1011 stars in our Galaxy, all with a range of ma ...
The H-R Diagram
... The Herzsprung Russel Diagram (HRD) is a systematic way of arranging stellar data. It plots the Absolute Magnitude (MV) or Luminosity (L/L¤) versus the Spectral Type, Surface Temperature or Color. The brightest stars are at the top and the hottest stars at the left. The radius increases diagonally t ...
... The Herzsprung Russel Diagram (HRD) is a systematic way of arranging stellar data. It plots the Absolute Magnitude (MV) or Luminosity (L/L¤) versus the Spectral Type, Surface Temperature or Color. The brightest stars are at the top and the hottest stars at the left. The radius increases diagonally t ...
Jan. 14 – Jan. 21
... other mass. The strength of the force is directly proportional to the product of the masses divided by the square of their separation F = Gm1m2/r2 F is force of gravity (N) m’s are masses (Kg) r is the distance between the masses (m) and G is the universal gravitational constant G = 6.67E-11 m3/kgs2 ...
... other mass. The strength of the force is directly proportional to the product of the masses divided by the square of their separation F = Gm1m2/r2 F is force of gravity (N) m’s are masses (Kg) r is the distance between the masses (m) and G is the universal gravitational constant G = 6.67E-11 m3/kgs2 ...
Document
... bright it looks from Earth, you can determine how far away it must be to look that faint. • For any star in the sky, we KNOW: – Apparent Magnitude (m) – Spectral Type (O, B, A, F, G, K, M) – Luminosity Class (Main Sequence, Giant, etc…). These are denoted by a roman numeral (V, III, I,…). ...
... bright it looks from Earth, you can determine how far away it must be to look that faint. • For any star in the sky, we KNOW: – Apparent Magnitude (m) – Spectral Type (O, B, A, F, G, K, M) – Luminosity Class (Main Sequence, Giant, etc…). These are denoted by a roman numeral (V, III, I,…). ...
Chapter 16 Lesson 2: What is a Star
... Lesson 2: What is a star? How the Sun Stacks Up as a Star a. The Sun is a star because all stars are very large balls of hot gases that give off electromagnetic radiation. b. The Sun gives off huge amounts of heat and light energy, due to very high heat and pressure that push hydrogen atoms together ...
... Lesson 2: What is a star? How the Sun Stacks Up as a Star a. The Sun is a star because all stars are very large balls of hot gases that give off electromagnetic radiation. b. The Sun gives off huge amounts of heat and light energy, due to very high heat and pressure that push hydrogen atoms together ...
A105 Stars and Galaxies
... orbits like? What are the eccentricities of our sun’s planets? Planets within 0.1 AU are probably tidally circularized Beyond 0.1 AU, the distribution of eccentricities appears essentially uniform between 0 and 0.8 Very different from our solar system! ...
... orbits like? What are the eccentricities of our sun’s planets? Planets within 0.1 AU are probably tidally circularized Beyond 0.1 AU, the distribution of eccentricities appears essentially uniform between 0 and 0.8 Very different from our solar system! ...
Lecture 13 (pdf from the powerpoint)
... through giant stages before becoming white dwarfs Higher mass stars move rapidly off the main sequence and into the giant stages, eventually exploding in a supernova ...
... through giant stages before becoming white dwarfs Higher mass stars move rapidly off the main sequence and into the giant stages, eventually exploding in a supernova ...
The Life CyCLe of STarS - Origins
... 33 Star Death. Eventually the core of the star runs out of fuel entirely, upsetting the balance between pressure and gravity; then the star dies. It may die gently, with the outer layers of the star drifting away from the core, or it may die dramatically in a supernova explosion in which most of the ...
... 33 Star Death. Eventually the core of the star runs out of fuel entirely, upsetting the balance between pressure and gravity; then the star dies. It may die gently, with the outer layers of the star drifting away from the core, or it may die dramatically in a supernova explosion in which most of the ...
16. Properties of Stars
... Deneb about 40000 x the area of the sun, so its radius and diameter are about 200x the diameter of the sun.l ...
... Deneb about 40000 x the area of the sun, so its radius and diameter are about 200x the diameter of the sun.l ...
Stars Study Guide KEY
... 3. Describe the life cycle of a high mass star. (Tell the steps in the life cycle.) The steps are: nebula, mature star, red SUPER giant, then supernova. Then it can become a nebula again or either a neutron star or a black hole. ...
... 3. Describe the life cycle of a high mass star. (Tell the steps in the life cycle.) The steps are: nebula, mature star, red SUPER giant, then supernova. Then it can become a nebula again or either a neutron star or a black hole. ...
The Milky Way Galaxy
... The reason Hershel incorrectly deduced that the sun is in the center is due to the presence of dark nebulae and dust in the Galaxy. Interstellar extinction blocks out all the star far away from the sun. ...
... The reason Hershel incorrectly deduced that the sun is in the center is due to the presence of dark nebulae and dust in the Galaxy. Interstellar extinction blocks out all the star far away from the sun. ...
Planets
... Of rocks and metal. The rocks come in many sizes. Larger rocks are Asteroids. They are found in large areas between the orbits of Mars And Jupiter. ...
... Of rocks and metal. The rocks come in many sizes. Larger rocks are Asteroids. They are found in large areas between the orbits of Mars And Jupiter. ...
Document
... • Stars begin as clouds of gas and dust, which collapse to form a stellar disk. This disk eventually becomes a star. • The star eventually runs out of nuclear fuel and dies. The manner of its death depends on its mass. ...
... • Stars begin as clouds of gas and dust, which collapse to form a stellar disk. This disk eventually becomes a star. • The star eventually runs out of nuclear fuel and dies. The manner of its death depends on its mass. ...
Galactic Address/Stars/Constellations
... • Stars can be as small as Earth or as large as the orbit of Jupiter. • https://www.youtube.com/watch?v=HEheh1BH34Q ...
... • Stars can be as small as Earth or as large as the orbit of Jupiter. • https://www.youtube.com/watch?v=HEheh1BH34Q ...
Announcements
... Visible (Balmer) lines of H formed when electron in 2nd level absorbs a photon and jumps up to a higher level, or when an electron in a higher level emits a photon and jumps down to the 2nd level. ...
... Visible (Balmer) lines of H formed when electron in 2nd level absorbs a photon and jumps up to a higher level, or when an electron in a higher level emits a photon and jumps down to the 2nd level. ...
AST 301 Introduction to Astronomy - University of Texas Astronomy
... How do we use the Hertzsprung-Russell diagram to make sense of the temperatures and luminosities of stars? Describe the life stages of a low-mass star, like the Sun. Use the HR diagram to show the evolution of a low-mass star graphically. What happens inside of a star that makes it change from a mai ...
... How do we use the Hertzsprung-Russell diagram to make sense of the temperatures and luminosities of stars? Describe the life stages of a low-mass star, like the Sun. Use the HR diagram to show the evolution of a low-mass star graphically. What happens inside of a star that makes it change from a mai ...
chapter3 - Empyrean Quest Publishers
... • Model was only a little more accurate than Ptolemaic model in predicting planetary positions, because it still used perfect circles & stars on a sphere, only a little bigger than Pythagoras claimed. ...
... • Model was only a little more accurate than Ptolemaic model in predicting planetary positions, because it still used perfect circles & stars on a sphere, only a little bigger than Pythagoras claimed. ...
Introduction to the Earth
... distance measurement called the Light- year 1 light-year is the distance light travels in one ...
... distance measurement called the Light- year 1 light-year is the distance light travels in one ...
Earth Science, 10th edition Chapter 23: Beyond Our Solar System I
... 2. Both orbit around a common center of mass b. Visual binaries are resolved telescopically c. More than 50% of the stars in the universe are binary stars d. Used to determine stellar mass 2. Stellar mass a. Determined using binary stars – the center of mass is closest to the most massive star b. Ma ...
... 2. Both orbit around a common center of mass b. Visual binaries are resolved telescopically c. More than 50% of the stars in the universe are binary stars d. Used to determine stellar mass 2. Stellar mass a. Determined using binary stars – the center of mass is closest to the most massive star b. Ma ...
Stars Notes
... 4.d – Students know that stars are the source of light for all bright objects in outer space and that the Moon and planets shine by reflected sunlight, not by their own light ...
... 4.d – Students know that stars are the source of light for all bright objects in outer space and that the Moon and planets shine by reflected sunlight, not by their own light ...
Chapter 20 The Universe
... Sun’s Atmosphere 1. Chromosphere- above photosphere - “sphere of color” bright red - 2500 km thick - 100,000 degrees C (hotter!) -only seen during solar eclipse photosphere is blocked -Solar prominences- erupting clouds of gas that fall back to sun Motions & Activities of Sun -energy at Earth now wa ...
... Sun’s Atmosphere 1. Chromosphere- above photosphere - “sphere of color” bright red - 2500 km thick - 100,000 degrees C (hotter!) -only seen during solar eclipse photosphere is blocked -Solar prominences- erupting clouds of gas that fall back to sun Motions & Activities of Sun -energy at Earth now wa ...
The Stars and the Solar System
... on a summer night. Others can only be seen on a winter night. This is because the Earth revolves around the sun. As it does, the part of the night sky that is visible from any one place changes. ...
... on a summer night. Others can only be seen on a winter night. This is because the Earth revolves around the sun. As it does, the part of the night sky that is visible from any one place changes. ...