Unit 1
... – Radiation carries away energy in regions where the photons are not readily absorbed by stellar gas – Close to the cores of massive stars, there is enough material to impede the flow of energy through radiation ...
... – Radiation carries away energy in regions where the photons are not readily absorbed by stellar gas – Close to the cores of massive stars, there is enough material to impede the flow of energy through radiation ...
Chapter 5 Lesson 1: The Sun
... • What is the largest object in our solar system? • An object in the solar system that produces heat and light is a _______________. • What causes energy to be released inside the sun? • How would earth be affected if the sun stopped producing energy? • Why are the planets not stars? • Why do you th ...
... • What is the largest object in our solar system? • An object in the solar system that produces heat and light is a _______________. • What causes energy to be released inside the sun? • How would earth be affected if the sun stopped producing energy? • Why are the planets not stars? • Why do you th ...
The Hertzsprung-Russell Diagram
... 9. Label the following steps on your H-R diagram to show the series of changes that our sun has undergone since its formation 4.6 billion years ago. a. Originally, a big cloud of gas and dust called a nebula condensed to form a young, cool star called a red dwarf. In this first stage of life, our s ...
... 9. Label the following steps on your H-R diagram to show the series of changes that our sun has undergone since its formation 4.6 billion years ago. a. Originally, a big cloud of gas and dust called a nebula condensed to form a young, cool star called a red dwarf. In this first stage of life, our s ...
Volcanoes and Igneous Activity Earth
... • Hydrogen burning migrates outward. The star’s outer envelope expands. • Its surface cools and becomes red. • The core collapses as helium is converted to carbon. Eventually all nuclear fuel is used and gravity squeezes the star. ...
... • Hydrogen burning migrates outward. The star’s outer envelope expands. • Its surface cools and becomes red. • The core collapses as helium is converted to carbon. Eventually all nuclear fuel is used and gravity squeezes the star. ...
Stars 3
... pressure but by the pressure that comes from heat energy. The carbon core ultimately reaches the 600 million degrees K needed for fusion of carbon, and the star keeps burning, developing a whole series of nuclear burning shells around an iron core. The final catastrophe for a massive star comes when ...
... pressure but by the pressure that comes from heat energy. The carbon core ultimately reaches the 600 million degrees K needed for fusion of carbon, and the star keeps burning, developing a whole series of nuclear burning shells around an iron core. The final catastrophe for a massive star comes when ...
StarCharacteristics
... If person A (pen light) stood in the classroom and person B (mega light) stood at the baseball fields across the street, which light would appear brighter? You cannot tell by looking in the sky how bright a star truly is. The farther away the star is, the less bright it ...
... If person A (pen light) stood in the classroom and person B (mega light) stood at the baseball fields across the street, which light would appear brighter? You cannot tell by looking in the sky how bright a star truly is. The farther away the star is, the less bright it ...
Teacher Subject Title Concept Context Tek/SE Verb
... Objects in the sky can be described and illustrated. We can observe objects in the sky, such as the Moon, Sun, and stars. — When is the best time to observe stars? — When is the best time to observe the Sun? The Sun is our nearest star. — What is the Sun? Objects in the sky can be described and illu ...
... Objects in the sky can be described and illustrated. We can observe objects in the sky, such as the Moon, Sun, and stars. — When is the best time to observe stars? — When is the best time to observe the Sun? The Sun is our nearest star. — What is the Sun? Objects in the sky can be described and illu ...
Astronomy 122 mid Term Exam
... Use the blackbody simulator to get a better feel for this inverse relation and review the material in Module 1 Lecture F. Also, as I said in class, if this inverse relation did not hold then cooler objects would be emitting short wavelength high energy photons which doesn’t make any physical sense b ...
... Use the blackbody simulator to get a better feel for this inverse relation and review the material in Module 1 Lecture F. Also, as I said in class, if this inverse relation did not hold then cooler objects would be emitting short wavelength high energy photons which doesn’t make any physical sense b ...
Test 2, November 14, 2016 - Physics@Brock
... 12. Which of the following features determines the resolving power of a telescope? (a) the focal length of the objective. (b) the focal length of the eyepiece. (c) the diameter of the objective. (d) the diameter of the eyepiece. 13. If the focal length of the objective of a telescope is 120 cm and t ...
... 12. Which of the following features determines the resolving power of a telescope? (a) the focal length of the objective. (b) the focal length of the eyepiece. (c) the diameter of the objective. (d) the diameter of the eyepiece. 13. If the focal length of the objective of a telescope is 120 cm and t ...
Stars - Science
... The first star is larger than the second star. The first star is smaller than the second star. The first star is hotter than the second star. The first star is cooler than the second star. ...
... The first star is larger than the second star. The first star is smaller than the second star. The first star is hotter than the second star. The first star is cooler than the second star. ...
http://www.highpoint.edu/~afuller/PHY-1050
... ejects the H and He into space as a planetary nebula. • The core left behind becomes a white dwarf. • Despite the name, this phenomenon has nothing immediate to do with planets ...
... ejects the H and He into space as a planetary nebula. • The core left behind becomes a white dwarf. • Despite the name, this phenomenon has nothing immediate to do with planets ...
Absolute magnitude
... to jump to a higher energy level. ▪ The photon’s energy must be equal to the energy difference between the two levels. ...
... to jump to a higher energy level. ▪ The photon’s energy must be equal to the energy difference between the two levels. ...
Sources of Gravitational Waves Peter Shawhan
... Orbit will continue to decay (inspiral) over the next ~300 million years, until… ...
... Orbit will continue to decay (inspiral) over the next ~300 million years, until… ...
Astronomy Webquest Part 1: Life of Stars: Go to http://www.odec.ca
... 3. Near the end of the main sequence, when there is not enough hydrogen gas to support the star, the outer layers will ______________ in an attempt to ______________________________. 4. This forms a ____________. Click on next. 5. After the core collapses due to lack of hydrogen, the red giant will ...
... 3. Near the end of the main sequence, when there is not enough hydrogen gas to support the star, the outer layers will ______________ in an attempt to ______________________________. 4. This forms a ____________. Click on next. 5. After the core collapses due to lack of hydrogen, the red giant will ...
The Evening Sky in February 2016
... In February bright stars are nearly overhead. Sirius, the brightest star, is north of the zenith. Canopus, the second brightest star, is south of the zenith. Below and left of Sirius are Orion's bright stars: bluish Rigel and reddish Betelgeuse. Between them is the line of three stars making Orion's ...
... In February bright stars are nearly overhead. Sirius, the brightest star, is north of the zenith. Canopus, the second brightest star, is south of the zenith. Below and left of Sirius are Orion's bright stars: bluish Rigel and reddish Betelgeuse. Between them is the line of three stars making Orion's ...
Stellar evolution
Stellar evolution is the process by which a star changes during its lifetime. Depending on the mass of the star, this lifetime ranges from a few million years for the most massive to trillions of years for the least massive, which is considerably longer than the age of the universe. The table shows the lifetimes of stars as a function of their masses. All stars are born from collapsing clouds of gas and dust, often called nebulae or molecular clouds. Over the course of millions of years, these protostars settle down into a state of equilibrium, becoming what is known as a main-sequence star.Nuclear fusion powers a star for most of its life. Initially the energy is generated by the fusion of hydrogen atoms at the core of the main-sequence star. Later, as the preponderance of atoms at the core becomes helium, stars like the Sun begin to fuse hydrogen along a spherical shell surrounding the core. This process causes the star to gradually grow in size, passing through the subgiant stage until it reaches the red giant phase. Stars with at least half the mass of the Sun can also begin to generate energy through the fusion of helium at their core, whereas more-massive stars can fuse heavier elements along a series of concentric shells. Once a star like the Sun has exhausted its nuclear fuel, its core collapses into a dense white dwarf and the outer layers are expelled as a planetary nebula. Stars with around ten or more times the mass of the Sun can explode in a supernova as their inert iron cores collapse into an extremely dense neutron star or black hole. Although the universe is not old enough for any of the smallest red dwarfs to have reached the end of their lives, stellar models suggest they will slowly become brighter and hotter before running out of hydrogen fuel and becoming low-mass white dwarfs.Stellar evolution is not studied by observing the life of a single star, as most stellar changes occur too slowly to be detected, even over many centuries. Instead, astrophysicists come to understand how stars evolve by observing numerous stars at various points in their lifetime, and by simulating stellar structure using computer models.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.