Neutron Stars - Otterbein University
... • core continues to cool and contract • Size ~ Earth • Density: a million times that of Earth – 1 cubic cm has 1000 kg of mass! ...
... • core continues to cool and contract • Size ~ Earth • Density: a million times that of Earth – 1 cubic cm has 1000 kg of mass! ...
Objects Beyond our Solar System
... This dying star actually burns hotter than the sun but will slowly get cooler and cooler until it becomes a black dwarf…this has yet to happen as it is estimated to take longer than the known age of the universe, 13.8 billion years. ...
... This dying star actually burns hotter than the sun but will slowly get cooler and cooler until it becomes a black dwarf…this has yet to happen as it is estimated to take longer than the known age of the universe, 13.8 billion years. ...
Slide 1
... they run out of nuclear fuel.. Typically 1,000 times the size of our solar system These Ten have names like Owl, the Cat's Eye, the Ghost of Jupiter, Ring. This glorious final phase in the life of a star lasts only about 10,000 ...
... they run out of nuclear fuel.. Typically 1,000 times the size of our solar system These Ten have names like Owl, the Cat's Eye, the Ghost of Jupiter, Ring. This glorious final phase in the life of a star lasts only about 10,000 ...
Homework problems for Quiz 2: AY5 Spring 2013
... lifetime of the Sun is 10 billion years). Lifetime = 4/5000 ×1010 = 8 × 106 years 5. Label the following True (T) or False (F) F More massive stars have lower temperatures in their cores T The reason main-sequence stars do not collapse due to gravity is the thermal pressure of the gases they are com ...
... lifetime of the Sun is 10 billion years). Lifetime = 4/5000 ×1010 = 8 × 106 years 5. Label the following True (T) or False (F) F More massive stars have lower temperatures in their cores T The reason main-sequence stars do not collapse due to gravity is the thermal pressure of the gases they are com ...
Chapter 27 Stars and Galaxies
... The second and longest stage in the life of a star is the main-sequence stage Main-sequence stars do not expand because the force of gravity pulls the matter inward. Some white dwarfs will just cool and die, they are then called black dwarfs ...
... The second and longest stage in the life of a star is the main-sequence stage Main-sequence stars do not expand because the force of gravity pulls the matter inward. Some white dwarfs will just cool and die, they are then called black dwarfs ...
How the univ works
... 21. ____________ always produce the same amount of light and are used to measure distance to galaxies. ...
... 21. ____________ always produce the same amount of light and are used to measure distance to galaxies. ...
The Death of Stars - Mounds Park Academy Blogs
... • They slowly fizzle out over billions of years. ...
... • They slowly fizzle out over billions of years. ...
Integrative Studies 410 Our Place in the Universe
... • Cloud contracts/warms, begins radiating; almost all radiated energy escapes • Cloud becomes dense opaque to radiation radiated energy trapped core heats up ...
... • Cloud contracts/warms, begins radiating; almost all radiated energy escapes • Cloud becomes dense opaque to radiation radiated energy trapped core heats up ...
ORIGIN OF THE UNIVERSE
... has been used. The outer layers explode off into space just leaving the white hot core (very small nearing the end of life) ...
... has been used. The outer layers explode off into space just leaving the white hot core (very small nearing the end of life) ...
Universe 8e Lecture Chapter 17 Nature of Stars
... (about 0.4 M to about 4 M) becomes a red giant when shell hydrogen fusion begins, a horizontal-branch star when core helium fusion begins, and an asymptotic giant branch (AGB) star when the helium in the core is exhausted and shell helium fusion begins. Planetary Nebulae and White Dwarfs: Helium s ...
... (about 0.4 M to about 4 M) becomes a red giant when shell hydrogen fusion begins, a horizontal-branch star when core helium fusion begins, and an asymptotic giant branch (AGB) star when the helium in the core is exhausted and shell helium fusion begins. Planetary Nebulae and White Dwarfs: Helium s ...
Universe 8e Lecture Chapter 17 Nature of Stars
... (about 0.4 M to about 4 M) becomes a red giant when shell hydrogen fusion begins, a horizontal-branch star when core helium fusion begins, and an asymptotic giant branch (AGB) star when the helium in the core is exhausted and shell helium fusion begins. Planetary Nebulae and White Dwarfs: Helium s ...
... (about 0.4 M to about 4 M) becomes a red giant when shell hydrogen fusion begins, a horizontal-branch star when core helium fusion begins, and an asymptotic giant branch (AGB) star when the helium in the core is exhausted and shell helium fusion begins. Planetary Nebulae and White Dwarfs: Helium s ...
File
... Massive stars have much _______ gravitational pressure on the core... they consume hydrogen much __________ (7-10 million years) the core temperatures are very ________ the outer surface is very large...a ______________ ________ when fuel runs out the star collapses and explodes...__________ ...
... Massive stars have much _______ gravitational pressure on the core... they consume hydrogen much __________ (7-10 million years) the core temperatures are very ________ the outer surface is very large...a ______________ ________ when fuel runs out the star collapses and explodes...__________ ...
Hertzsprung - Russel Diagram
... 10. What color are the coolest stars? _____________ 11. What category of stars is hot but not very luminous? ______________________________ 12. If you know a stars color, you can determine it’s ______________________________________. 13. The H-R Diagram is based on what two criteria? A. ____________ ...
... 10. What color are the coolest stars? _____________ 11. What category of stars is hot but not very luminous? ______________________________ 12. If you know a stars color, you can determine it’s ______________________________________. 13. The H-R Diagram is based on what two criteria? A. ____________ ...
Stars after the Main Sequence. Example: Betelgeuse (Alpha Orionis
... PV=nRT. Pressure depends on both density and temperature • Extremely dense, “degenerate” gas PV=Kn. Pressure depends only on density • Demo ...
... PV=nRT. Pressure depends on both density and temperature • Extremely dense, “degenerate” gas PV=Kn. Pressure depends only on density • Demo ...
Stellar Notes
... On our test we will be diagraming the life cycle of a star, explaining the EM spectrum and how astronomers ID stars. ...
... On our test we will be diagraming the life cycle of a star, explaining the EM spectrum and how astronomers ID stars. ...
Stellar Evolution Reading Questions Integrated Science 2 Name
... shock wave from an ___________________ of a nearby star may trigger the contraction. Once the process begins, _________________ squeezes particles in the nebula, pulling every particle toward the _____________. As the nebula shrinks, gravitational energy is converted to _______________ energy. 3. Mo ...
... shock wave from an ___________________ of a nearby star may trigger the contraction. Once the process begins, _________________ squeezes particles in the nebula, pulling every particle toward the _____________. As the nebula shrinks, gravitational energy is converted to _______________ energy. 3. Mo ...
Stars - Images
... Ways of tracking where the constellations are located during the different seasons of the year. Remember as the earth revolves around the sun, it also rotates causing the stars to “shift” in the ...
... Ways of tracking where the constellations are located during the different seasons of the year. Remember as the earth revolves around the sun, it also rotates causing the stars to “shift” in the ...
Stellar evolution, II
... Consider a cloud of cold (50 deg K) atomic hydrogen gas. If an electron of one atom flips its spin state and the electron then has a slightly lower energy state, the photon that is emitted is a. An ultraviolet photon of wavelength 1216 Angstroms b. An optical photon of wavelength 6563 Angstroms c. ...
... Consider a cloud of cold (50 deg K) atomic hydrogen gas. If an electron of one atom flips its spin state and the electron then has a slightly lower energy state, the photon that is emitted is a. An ultraviolet photon of wavelength 1216 Angstroms b. An optical photon of wavelength 6563 Angstroms c. ...
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.