Stars
... Stars have different colors ranging from reds, oranges, and yellows, to blues and whites. ...
... Stars have different colors ranging from reds, oranges, and yellows, to blues and whites. ...
Powerpoint
... We start by drawing the axes: •Luminosity up the vertical axis (measured relative to the Sun) •Temperature along the horizontal axis (measured in Kelvin) The stars Vega and Sirius are brighter than the Sun, and also hotter. Where would you put them? Where would you mark the Sun on the plot? ...
... We start by drawing the axes: •Luminosity up the vertical axis (measured relative to the Sun) •Temperature along the horizontal axis (measured in Kelvin) The stars Vega and Sirius are brighter than the Sun, and also hotter. Where would you put them? Where would you mark the Sun on the plot? ...
Star in a Box - Las Cumbres Observatory Global Telescope
... We start by drawing the axes: •Luminosity up the vertical axis (measured relative to the Sun) •Temperature along the horizontal axis (measured in Kelvin) The stars Vega and Sirius are brighter than the Sun, and also hotter. Where would you put them? Where would you mark the Sun on the plot? ...
... We start by drawing the axes: •Luminosity up the vertical axis (measured relative to the Sun) •Temperature along the horizontal axis (measured in Kelvin) The stars Vega and Sirius are brighter than the Sun, and also hotter. Where would you put them? Where would you mark the Sun on the plot? ...
Word doc - UC-HiPACC - University of California, Santa Cruz
... Some stars end their lives in cataclysmic explosions: spectacular supernovae, which briefly become the most brilliant objects in their home galaxies, visible from millions or even billions of light-years away. Supernovae are of several distinct types, as is evident from their spectra—the graphs astr ...
... Some stars end their lives in cataclysmic explosions: spectacular supernovae, which briefly become the most brilliant objects in their home galaxies, visible from millions or even billions of light-years away. Supernovae are of several distinct types, as is evident from their spectra—the graphs astr ...
Hertzsprung-Russell Diagram
... A star has a high luminosity (100 solar luminosities) and a surface temperature of 3500 K. What type of star is it? ...
... A star has a high luminosity (100 solar luminosities) and a surface temperature of 3500 K. What type of star is it? ...
Document
... find the exam with your name on it bring ID, calculator, and pencil there will be about 80 questions on the final exam ...
... find the exam with your name on it bring ID, calculator, and pencil there will be about 80 questions on the final exam ...
The Life And Times Of A Star
... The hydrogen fusion is happening very, very fast now, so a LOT of waste helium is getting produced and dumped onto the dead helium core. The dead helium core is now very big and massive, but still isn’t producing energy using nuclear fusion, so it continues to collapse under its own weight. ...
... The hydrogen fusion is happening very, very fast now, so a LOT of waste helium is getting produced and dumped onto the dead helium core. The dead helium core is now very big and massive, but still isn’t producing energy using nuclear fusion, so it continues to collapse under its own weight. ...
Chapter 21 power point - Laconia School District
... • A large amount of gas and dust in space spreaded out in an immense volume ...
... • A large amount of gas and dust in space spreaded out in an immense volume ...
Section 1 Notes on Stars
... of term – this is about the birth, life and death of stars and that is NOT evolution)? 2. What kind of matter exists in the spaces between the stars? 3. In what kind of nebulae do new stars form? 4. What steps are involved in forming a star like the Sun? 5. When a star forms, why does it end up with ...
... of term – this is about the birth, life and death of stars and that is NOT evolution)? 2. What kind of matter exists in the spaces between the stars? 3. In what kind of nebulae do new stars form? 4. What steps are involved in forming a star like the Sun? 5. When a star forms, why does it end up with ...
Document
... of term – this is about the birth, life and death of stars and that is NOT evolution)? 2. What kind of matter exists in the spaces between the stars? 3. In what kind of nebulae do new stars form? 4. What steps are involved in forming a star like the Sun? 5. When a star forms, why does it end up with ...
... of term – this is about the birth, life and death of stars and that is NOT evolution)? 2. What kind of matter exists in the spaces between the stars? 3. In what kind of nebulae do new stars form? 4. What steps are involved in forming a star like the Sun? 5. When a star forms, why does it end up with ...
Ch 29 Sun and Solar Activity
... atmosphere, disrupt longrange radios, satell. & radar • solar flame animation ...
... atmosphere, disrupt longrange radios, satell. & radar • solar flame animation ...
Other Facets of Giant Branch Evolution • As the envelope cools due
... Other Facets of Giant Branch Evolution • As the envelope cools due to expansion, the opacity in the envelope increases (due to Kramers law), so by the time the star reaches the base of the giant branch (point 5), convection dominates energy transport. The thermal energy trapped by this opacity cause ...
... Other Facets of Giant Branch Evolution • As the envelope cools due to expansion, the opacity in the envelope increases (due to Kramers law), so by the time the star reaches the base of the giant branch (point 5), convection dominates energy transport. The thermal energy trapped by this opacity cause ...
Section 14
... The number of stars in the sky that we can see on crystal clear nights with just our eyes is maybe 4000. The number of stars in the universe is estimated to be in the area of 100,000,000,000,000,000 (100 quadrillion) or more. Birth of Stars: The universe is not a perfect vacuum dotted with stars and ...
... The number of stars in the sky that we can see on crystal clear nights with just our eyes is maybe 4000. The number of stars in the universe is estimated to be in the area of 100,000,000,000,000,000 (100 quadrillion) or more. Birth of Stars: The universe is not a perfect vacuum dotted with stars and ...
Document
... of term – this is about the birth, life and death of stars and that is NOT evolution)? 2. What kind of matter exists in the spaces between the stars? 3. In what kind of nebulae do new stars form? 4. What steps are involved in forming a star like the Sun? 5. When a star forms, why does it end up with ...
... of term – this is about the birth, life and death of stars and that is NOT evolution)? 2. What kind of matter exists in the spaces between the stars? 3. In what kind of nebulae do new stars form? 4. What steps are involved in forming a star like the Sun? 5. When a star forms, why does it end up with ...
Birth of Elements
... For stars with M ˂ 8Mʘ, Helium burning is all that can happen.10 During the later part of the evolution of these stars, a significant part of the outer envelope is ejected to form a tenuous cloud called a planetary nebula. Since these stars are not heavy enough to ignite further nuclear reactions, t ...
... For stars with M ˂ 8Mʘ, Helium burning is all that can happen.10 During the later part of the evolution of these stars, a significant part of the outer envelope is ejected to form a tenuous cloud called a planetary nebula. Since these stars are not heavy enough to ignite further nuclear reactions, t ...
Unit 1
... • a. differential rotation on the Sun creates vortices, or eddies, which are cooler and darker than the rest of the solar surface • b. solar flares cause the photoshere to expand and cool in the vicinity of the flare • c. magnetic fields breaking through the photosphere inhibit heat conduction where ...
... • a. differential rotation on the Sun creates vortices, or eddies, which are cooler and darker than the rest of the solar surface • b. solar flares cause the photoshere to expand and cool in the vicinity of the flare • c. magnetic fields breaking through the photosphere inhibit heat conduction where ...
PH507 - University of Kent
... 3. Taking Deneb to have a surface temperature of 8,500K and a radius of 200 solar radii, determine the present spectral class and luminosity class of Deneb. Investigate and state the stages through which Deneb is expected to progress. State the name of the pre-main-sequence track that Deneb would ha ...
... 3. Taking Deneb to have a surface temperature of 8,500K and a radius of 200 solar radii, determine the present spectral class and luminosity class of Deneb. Investigate and state the stages through which Deneb is expected to progress. State the name of the pre-main-sequence track that Deneb would ha ...
Notes
... 4. After about ______________________years the core will run out of helium and will contract further which will cause outer layers to __________________. a. the sun will then become a __________________ i. about the size of ___________ ...
... 4. After about ______________________years the core will run out of helium and will contract further which will cause outer layers to __________________. a. the sun will then become a __________________ i. about the size of ___________ ...
Star Life
... 8) The smallest of stars will end their life as which of the following? a. Black Hole b. White Dwarf c. Super Red Giant d. Neutron Star 9) A main sequence star is mostly made of which two elements? a. Hydrogen and Carbon b. Hydrogen and Helium c. Helium and Carbon d. Helium and Iron 10) Which stage ...
... 8) The smallest of stars will end their life as which of the following? a. Black Hole b. White Dwarf c. Super Red Giant d. Neutron Star 9) A main sequence star is mostly made of which two elements? a. Hydrogen and Carbon b. Hydrogen and Helium c. Helium and Carbon d. Helium and Iron 10) Which stage ...
How do stars produce energy?
... • Helium nuclear reactions can occur for a while, but they will run out pretty fast • Sun will end its life as a hot carbon core: a white dwarf – Further collapse and heating is prevented by a different kind of pressure called electron degenerate pressure • Outer layers are shed in what is known as ...
... • Helium nuclear reactions can occur for a while, but they will run out pretty fast • Sun will end its life as a hot carbon core: a white dwarf – Further collapse and heating is prevented by a different kind of pressure called electron degenerate pressure • Outer layers are shed in what is known as ...
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.