Science Centre Talk
... Stellar evolution is the struggle of pressure against gravity. Gravity always defeats gas pressure, eventually For solar-type stars, the last defence is electron degeneracy pressure (the sun will end its life as a white dwarf). For more massive stars, the final fate is a neutron star, or a black hol ...
... Stellar evolution is the struggle of pressure against gravity. Gravity always defeats gas pressure, eventually For solar-type stars, the last defence is electron degeneracy pressure (the sun will end its life as a white dwarf). For more massive stars, the final fate is a neutron star, or a black hol ...
astronomy final exam - Physics and Astronomy
... Why is carbon is so important to living organisms? What is the necessary medium for the transport of materials needed for the life process? Describe the possibility of planets with stable orbits in binary star systems compared to single star systems. ...
... Why is carbon is so important to living organisms? What is the necessary medium for the transport of materials needed for the life process? Describe the possibility of planets with stable orbits in binary star systems compared to single star systems. ...
Quantum Well Electron Gain Structures and Infrared
... ~5-6 variation in EW in 1 year) implies that one star is dominant source of ionizing radiation • Thus, even if it is a binary, probable q>1 and mass limit >> 75 M0 • (And … something BIGGER made a neutron star ...
... ~5-6 variation in EW in 1 year) implies that one star is dominant source of ionizing radiation • Thus, even if it is a binary, probable q>1 and mass limit >> 75 M0 • (And … something BIGGER made a neutron star ...
Hertzsprung-Russell Diagram Astronomy Project Purpose: To
... sun. Example: Betelgeuse is 38000 LSUN, and emits 1.4 x 1031 watts 3.) With the provided formula, determine the star’s radius, and find some way of comparing it to other objects in the solar system. Example: The radius of Betelgeuse is 380,000,000 km, which could fit the entire orbit of the inner pl ...
... sun. Example: Betelgeuse is 38000 LSUN, and emits 1.4 x 1031 watts 3.) With the provided formula, determine the star’s radius, and find some way of comparing it to other objects in the solar system. Example: The radius of Betelgeuse is 380,000,000 km, which could fit the entire orbit of the inner pl ...
Stellar Evolution – Test Review Answers
... Nearly in the middle of both the temperature and luminosity scales relative to other stars. This puts it around the middle of the main sequence. 17. Where are giant stars, supergiant stars and white dwarfs found on the H-R diagram, relative to the main sequence? Giant and supergiant stars lie above ...
... Nearly in the middle of both the temperature and luminosity scales relative to other stars. This puts it around the middle of the main sequence. 17. Where are giant stars, supergiant stars and white dwarfs found on the H-R diagram, relative to the main sequence? Giant and supergiant stars lie above ...
Starlight and What it Tells Us
... Radiation is Reflected from Some Other Source • The Sun Emits Black-Body Radiation, the Moon Does Not ...
... Radiation is Reflected from Some Other Source • The Sun Emits Black-Body Radiation, the Moon Does Not ...
chapter 18
... helium nuclei to form carbon nuclei. c) hydrogen nuclei to form helium nuclei. d) carbon nuclei to form magnesium nuclei. ...
... helium nuclei to form carbon nuclei. c) hydrogen nuclei to form helium nuclei. d) carbon nuclei to form magnesium nuclei. ...
Stellar Brightness Apparent magnitude
... 4. Gas pressure increases as atomic collisions and density (atoms/space) increase. 5. The protostar’s gas pressure RESISTS the collapse of the nebula. 6. When gas pressure = gravity, the protostar has reached equilibrium and accretion stops ...
... 4. Gas pressure increases as atomic collisions and density (atoms/space) increase. 5. The protostar’s gas pressure RESISTS the collapse of the nebula. 6. When gas pressure = gravity, the protostar has reached equilibrium and accretion stops ...
Integrative Studies 410 Our Place in the Universe
... a interstellar gas cloud at the same time •Evidence: We see “associations” of stars of same age ...
... a interstellar gas cloud at the same time •Evidence: We see “associations” of stars of same age ...
ASTR 101 Deming EXAM II November 18 OFFICE HRS in CSS
... Stellar properties—how do astronomers determine motion, distance, brightness, luminosity, temperature, size, mass? (handouts) What did you do in labs 6, 7 and 8? What stellar properties were used/determined? How are studies of binary stars useful? How does the HR diagram help astronomers understand ...
... Stellar properties—how do astronomers determine motion, distance, brightness, luminosity, temperature, size, mass? (handouts) What did you do in labs 6, 7 and 8? What stellar properties were used/determined? How are studies of binary stars useful? How does the HR diagram help astronomers understand ...
Place the stars in the proper sequence, following the
... 13. What is the color of the hottest stars? Blue and White 14. Which classification of star has the most energy? Blue and White (also, hottest) a. How is a star’s temperature related to its energy? The hotter the star, the more energy it has b. How is a star’s magnitude related to its energy? Along ...
... 13. What is the color of the hottest stars? Blue and White 14. Which classification of star has the most energy? Blue and White (also, hottest) a. How is a star’s temperature related to its energy? The hotter the star, the more energy it has b. How is a star’s magnitude related to its energy? Along ...
2009 Assessment Schedule (90764)
... When the mass of the protostar is sufficiently high it enables the nuclear fusion of hydrogen into helium and becomes a main sequence star. AND Gravitational collapse explained using one or more causes stated below. Gravitational collapse can be caused by: • giant molecular clouds colliding, • passi ...
... When the mass of the protostar is sufficiently high it enables the nuclear fusion of hydrogen into helium and becomes a main sequence star. AND Gravitational collapse explained using one or more causes stated below. Gravitational collapse can be caused by: • giant molecular clouds colliding, • passi ...
1_Introduction
... The Sun is not transparent. Photons travel only an inch before being scattered in a random direction. ...
... The Sun is not transparent. Photons travel only an inch before being scattered in a random direction. ...
Star Jeopardy Review #2
... Star formation may be triggered by __________ which help gravity through compression of interstellar clouds to greater densities. ...
... Star formation may be triggered by __________ which help gravity through compression of interstellar clouds to greater densities. ...
Main Sequence Stars
... • Spheres of water have several properties: mass, volume, radius, surface area … • We can make a “Vogt-Russell” theorem for balls of water that says that all of the other properties of a ball of water are determined by just the mass and even write down equations, i.e. volume = mass/(density of water ...
... • Spheres of water have several properties: mass, volume, radius, surface area … • We can make a “Vogt-Russell” theorem for balls of water that says that all of the other properties of a ball of water are determined by just the mass and even write down equations, i.e. volume = mass/(density of water ...
knowledge quiz - Discovery Education
... in the middle where it has many stars. Where is the Milky Way brightest? A. in its middle B. on its edges C. It has the same brightness throughout. D. It’s not bright at all. 10. Galaxies are made up of billions of stars, all giving off light, but many galaxies can only be seen with powerful telesco ...
... in the middle where it has many stars. Where is the Milky Way brightest? A. in its middle B. on its edges C. It has the same brightness throughout. D. It’s not bright at all. 10. Galaxies are made up of billions of stars, all giving off light, but many galaxies can only be seen with powerful telesco ...
Characteristics of Stars
... • Absolute Magnitude: the “Real” brightness of the star. How much light it really gives off.(Need to know the distance to the Star) • Apparent Magnitude: How bright the star appears to be. ...
... • Absolute Magnitude: the “Real” brightness of the star. How much light it really gives off.(Need to know the distance to the Star) • Apparent Magnitude: How bright the star appears to be. ...
Chapter 12
... will be ready to study the rest of the universe, from galaxies that contain billions of stars to the planets that form around individual stars. ...
... will be ready to study the rest of the universe, from galaxies that contain billions of stars to the planets that form around individual stars. ...
What is a T Tauri star?
... Found in dusty regions- proper motions correlated Off main sequence Sometimes associated with disks and/or outflows ...
... Found in dusty regions- proper motions correlated Off main sequence Sometimes associated with disks and/or outflows ...
Star Life Cycle
... A Red Giant Star is a main sequence star that is not longer in equilibrium. There is a ...
... A Red Giant Star is a main sequence star that is not longer in equilibrium. There is a ...
Characteristics of Stars
... Stars that glow blue-white are the hottest (15,000 degrees Celsius) Rigel ...
... Stars that glow blue-white are the hottest (15,000 degrees Celsius) Rigel ...
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.