Characteristics of Stars
... 4. In relation to the brightness of other stars how bright is the Sun? What are the three characteristics astronomers use to classify stars? 5. What size is the Sun compared to other stars? What are very large stars called? How far would the supergiant Betelgeuse reach if it were to replace our Sun? ...
... 4. In relation to the brightness of other stars how bright is the Sun? What are the three characteristics astronomers use to classify stars? 5. What size is the Sun compared to other stars? What are very large stars called? How far would the supergiant Betelgeuse reach if it were to replace our Sun? ...
Chapter 28 – Stars and Galaxies
... 5 Milky Way belongs to the Local Group of about 30 galaxies B. Types of galaxies 1 Spiral – like the Milky Way 2 Elliptical – spherical to lens shaped 3 Irregular – much smaller and fainter with no shape C. Active Galaxies 1 Galaxies that emit more energy than their combined stars are said to be act ...
... 5 Milky Way belongs to the Local Group of about 30 galaxies B. Types of galaxies 1 Spiral – like the Milky Way 2 Elliptical – spherical to lens shaped 3 Irregular – much smaller and fainter with no shape C. Active Galaxies 1 Galaxies that emit more energy than their combined stars are said to be act ...
Life Cycle of a Star - Intervention Worksheet
... After the star explodes, some of the materials from the star are left behind. This material may form a neutron star. Neutron stars are the remains of massive stars. The most massive stars become black holes when they die. After a massive star explodes, a large amount of mass may remain. The gravity ...
... After the star explodes, some of the materials from the star are left behind. This material may form a neutron star. Neutron stars are the remains of massive stars. The most massive stars become black holes when they die. After a massive star explodes, a large amount of mass may remain. The gravity ...
Section 25.2 Stellar Evolution
... 7. forms a red giant, which then collapses into a red dwarf and forms a planetary nebula 8. blows up in a supernova explosion 9. does not form a red giant; collapses directly into a white dwarf ...
... 7. forms a red giant, which then collapses into a red dwarf and forms a planetary nebula 8. blows up in a supernova explosion 9. does not form a red giant; collapses directly into a white dwarf ...
CHAPTER 2 NOTES (STARS AND GALAXIES)
... 3 types of galaxies are: 1. spiral- arms like a pinwheel ex our galaxy- Milky Way 2. elliptical- nearly spherical to flatdisks (older than other galaxies) 3. irregular- no orderly or definite shape, not very common Milky Way Galaxy- pinwheel shaped disk with bulge in center -the older stars are near ...
... 3 types of galaxies are: 1. spiral- arms like a pinwheel ex our galaxy- Milky Way 2. elliptical- nearly spherical to flatdisks (older than other galaxies) 3. irregular- no orderly or definite shape, not very common Milky Way Galaxy- pinwheel shaped disk with bulge in center -the older stars are near ...
the Study Guide
... common shape is a spiral, like our own Milky Way Galaxy. Scientists estimate that the Milky Way has 200 billion stars. Gravity: The attractive force of celestial objects. The amount of gravity is determined by the mass of the object, the greater the mass, the more powerful the gravity. Hydrogen: The ...
... common shape is a spiral, like our own Milky Way Galaxy. Scientists estimate that the Milky Way has 200 billion stars. Gravity: The attractive force of celestial objects. The amount of gravity is determined by the mass of the object, the greater the mass, the more powerful the gravity. Hydrogen: The ...
the size and structure of the universe
... are balls of gas that produce their own energy by the process of NUCLEAR FUSION; they are the major features of galaxies – diameter of the sun (an average star) = 870,000 miles (1,392,000 km.) – That’s over 100,000 times the diameter of the Earth. Over 1,000,000 Earths could fit inside of the Sun ...
... are balls of gas that produce their own energy by the process of NUCLEAR FUSION; they are the major features of galaxies – diameter of the sun (an average star) = 870,000 miles (1,392,000 km.) – That’s over 100,000 times the diameter of the Earth. Over 1,000,000 Earths could fit inside of the Sun ...
Image Credit: NASA,ESA, HEIC, Hubble
... • Only set amount of Hydrogen gas to use in nuclear fusion. – Must find some other way to counteract gravitational pressure ...
... • Only set amount of Hydrogen gas to use in nuclear fusion. – Must find some other way to counteract gravitational pressure ...
Unit E Space Exploration Section 1 Notnd Space has changed over
... Held together by gravity. The Milky Way Galaxy is ...
... Held together by gravity. The Milky Way Galaxy is ...
Stellar Structure, Polytropes, Standard Stellar Model
... For a massive stellar core just prior to collapse, T ≃ 0.7 MeV and ρ ≃ 6 × 109 g cm−3, and the Pth /P ≃ 0.12, and the effective Mch is (1.12)3/2 = 1.19 times larger. The negative Coulomb lattice pressure, which is about 4% of the total, lowers this. At densities in excess of 106 g cm−3, electron cap ...
... For a massive stellar core just prior to collapse, T ≃ 0.7 MeV and ρ ≃ 6 × 109 g cm−3, and the Pth /P ≃ 0.12, and the effective Mch is (1.12)3/2 = 1.19 times larger. The negative Coulomb lattice pressure, which is about 4% of the total, lowers this. At densities in excess of 106 g cm−3, electron cap ...
The Hertzsprung-Russell Diagram
... star against its spectral type. This works best for a cluster, where you know the stars are all at the same distance. Then apparent brightness vs spectral type is basically the same as luminosity vs temperature. They found that stars only appear in certain parts of the diagram. ...
... star against its spectral type. This works best for a cluster, where you know the stars are all at the same distance. Then apparent brightness vs spectral type is basically the same as luminosity vs temperature. They found that stars only appear in certain parts of the diagram. ...
Stars Unit 1-2: Stars
... in size, they vary even more in density! – Our sun has a density about 1.4 times greater than water. – Betelgeuse (don’t say it two more times!) is one-millionth the density of the sun. – Sirius is so dense, that one teaspoon of it would weigh more than a ton on earth! ...
... in size, they vary even more in density! – Our sun has a density about 1.4 times greater than water. – Betelgeuse (don’t say it two more times!) is one-millionth the density of the sun. – Sirius is so dense, that one teaspoon of it would weigh more than a ton on earth! ...
Stellar Evolution Diagram Answer Key:
... spin rapidly and flattens into a disk shape. Protostar: A protostars lifetime is only a few years. As the nebula shrinks a central mass will collect towards the center. It heats up because of the collision of particles and the increase in pressure. A protostar becomes a main sequence star when it re ...
... spin rapidly and flattens into a disk shape. Protostar: A protostars lifetime is only a few years. As the nebula shrinks a central mass will collect towards the center. It heats up because of the collision of particles and the increase in pressure. A protostar becomes a main sequence star when it re ...
Characteristics of stars powerpoint
... • A cluster of stars • Can contains hundreds of billions of stars • We live in the Milky Way galaxy • Distance across the Milky Way = 250 million billion kilometers • Even if you could travel at the speed of light it would still take you 25,000 years to cross the galaxy ...
... • A cluster of stars • Can contains hundreds of billions of stars • We live in the Milky Way galaxy • Distance across the Milky Way = 250 million billion kilometers • Even if you could travel at the speed of light it would still take you 25,000 years to cross the galaxy ...
Document
... of rotation. Thus, many young stars have a bipolar outflow, a flow of gas out the poles of the star. This is a feature which is easily seen by radio telescopes. This early phase in the life of a star is called the TTauri phase. ...
... of rotation. Thus, many young stars have a bipolar outflow, a flow of gas out the poles of the star. This is a feature which is easily seen by radio telescopes. This early phase in the life of a star is called the TTauri phase. ...
Ay 101 - The Physics of Stars – fall 2015 -... Homework 1, due Friday Oct 9 at class (2 pm)
... fractions: f1 = 0.10, f2 = 0.85, and f3 = 0.05. Their partition functions (degeneracies) are g1 = 1, g2 = 2, g3 = 8. The ionization energy from the fundamental level for ion 1 is 30 eV, and it is 55 eV for ion 2. Calculate ne and T . 2. (10 points) Calculate (approximately) for the Sun the gravitati ...
... fractions: f1 = 0.10, f2 = 0.85, and f3 = 0.05. Their partition functions (degeneracies) are g1 = 1, g2 = 2, g3 = 8. The ionization energy from the fundamental level for ion 1 is 30 eV, and it is 55 eV for ion 2. Calculate ne and T . 2. (10 points) Calculate (approximately) for the Sun the gravitati ...
Life Cycle of a Star
... star explodes, some of the materials from the star are left behind. This material may form a neutron star. Neutron stars are the remains of high-mass stars. The most massive stars become black holes when they die. After a large mass star explodes, a large amount of mass may remain. The gravity of th ...
... star explodes, some of the materials from the star are left behind. This material may form a neutron star. Neutron stars are the remains of high-mass stars. The most massive stars become black holes when they die. After a large mass star explodes, a large amount of mass may remain. The gravity of th ...
Life Cycle of a Star - Intervention Worksheet
... After the star explodes, some of the materials from the star are left behind. This material may form a neutron star. Neutron stars are the remains of high-mass stars. The most massive stars become black holes when they die. After a large mass star explodes, a large amount of mass may remain. The gra ...
... After the star explodes, some of the materials from the star are left behind. This material may form a neutron star. Neutron stars are the remains of high-mass stars. The most massive stars become black holes when they die. After a large mass star explodes, a large amount of mass may remain. The gra ...
Stars Life Cycle WS
... After the star explodes, some of the materials from the star are left behind. This material may form a neutron star. Neutron stars are the remains of high-mass stars. The most massive stars become black holes when they die. After a large mass star explodes, a large amount of mass may remain. The gra ...
... After the star explodes, some of the materials from the star are left behind. This material may form a neutron star. Neutron stars are the remains of high-mass stars. The most massive stars become black holes when they die. After a large mass star explodes, a large amount of mass may remain. The gra ...
galaxies - GEOCITIES.ws
... – If a star has between 1.4 and 9 solar masses, it will become a neutron star. – A neutron star is a star made entirely of neutrons, as the name suggests. After a star goes supernova, the remaining core collapses. Gravity shrinks and condenses it into a sphere about the size of Manhattan (fifteen mi ...
... – If a star has between 1.4 and 9 solar masses, it will become a neutron star. – A neutron star is a star made entirely of neutrons, as the name suggests. After a star goes supernova, the remaining core collapses. Gravity shrinks and condenses it into a sphere about the size of Manhattan (fifteen mi ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.