Slide 1
... would be locked up inside white dwarfs if it wasn't for supernovae. Supernovae enrich the gas between the stars with all kinds of chemical elements that are necessary for the production of planets and life. The pressure of a supernova blast may trigger the formation of stars and planets in an inters ...
... would be locked up inside white dwarfs if it wasn't for supernovae. Supernovae enrich the gas between the stars with all kinds of chemical elements that are necessary for the production of planets and life. The pressure of a supernova blast may trigger the formation of stars and planets in an inters ...
Linking Asteroids and Meteorites through Reflectance Spectroscopy
... • The white area is the core of a Galaxy • Inside the core there is a brown spiralshaped disk. • It weighs a hundred thousand times as much as our Sun. ...
... • The white area is the core of a Galaxy • Inside the core there is a brown spiralshaped disk. • It weighs a hundred thousand times as much as our Sun. ...
Death of Stars
... Birth Place of Stars: Dark and cold inter-stellar clouds These clouds are made of more hydrogen than helium. These clouds have very small amount of heavier elements. ...
... Birth Place of Stars: Dark and cold inter-stellar clouds These clouds are made of more hydrogen than helium. These clouds have very small amount of heavier elements. ...
ANTARES - National Optical Astronomy Observatory
... Astronomy continues to have a strong discovery-based element. Despite theoretical consideration of Einstein’s cosmological constant (Carroll et al., 1992), no one predicted the revolution that occurred in 1998 when observations of supernovae revealed that the Universe was not just expanding, but acc ...
... Astronomy continues to have a strong discovery-based element. Despite theoretical consideration of Einstein’s cosmological constant (Carroll et al., 1992), no one predicted the revolution that occurred in 1998 when observations of supernovae revealed that the Universe was not just expanding, but acc ...
Stellar Evolution
... carbon core. • How they get from main sequence to the carbon core stage is a little different. • Now however, there is enough mass that it becomes hot enough to fuse carbon? • Hot enough to eventually fuse lots of elements. ...
... carbon core. • How they get from main sequence to the carbon core stage is a little different. • Now however, there is enough mass that it becomes hot enough to fuse carbon? • Hot enough to eventually fuse lots of elements. ...
Solutions
... Therefore, a B0 star has a lifetime of 1010 yr / 173 = 2 Million years b (2 points) What do you expect to be the end-state of this star? ...
... Therefore, a B0 star has a lifetime of 1010 yr / 173 = 2 Million years b (2 points) What do you expect to be the end-state of this star? ...
The Hidden Lives of Galaxies NSTA 2001
... • Under collapse, protons and electrons combine to form neutrons. • 10 Km across Black Hole (If mass of core > 5 x Solar) • Not even compacted neutrons can support weight of very massive stars. ...
... • Under collapse, protons and electrons combine to form neutrons. • 10 Km across Black Hole (If mass of core > 5 x Solar) • Not even compacted neutrons can support weight of very massive stars. ...
life cycle of stars
... • Under collapse, protons and electrons combine to form neutrons. • 10 Km across Black Hole (If mass of core > 5 x Solar) • Not even compacted neutrons can support weight of very massive stars. ...
... • Under collapse, protons and electrons combine to form neutrons. • 10 Km across Black Hole (If mass of core > 5 x Solar) • Not even compacted neutrons can support weight of very massive stars. ...
Stars and Light
... out) gravity will force the sun to collapse, which will increase the temperature so He can fuse (to form carbon). • When it does this, the outer layers “explode” and it becomes a Red Giant star. ...
... out) gravity will force the sun to collapse, which will increase the temperature so He can fuse (to form carbon). • When it does this, the outer layers “explode” and it becomes a Red Giant star. ...
Low-Mass Stars
... • Now however, there is enough mass that it becomes hot enough to fuse carbon? • Hot enough to eventually fuse lots of elements. ...
... • Now however, there is enough mass that it becomes hot enough to fuse carbon? • Hot enough to eventually fuse lots of elements. ...
Stellar Evolution
... • Now however, there is enough mass that it becomes hot enough to fuse carbon? • Hot enough to eventually fuse lots of elements. ...
... • Now however, there is enough mass that it becomes hot enough to fuse carbon? • Hot enough to eventually fuse lots of elements. ...
From Supernovae to Planets - Astronomical Society of the Pacific
... Artist’s concept of a stellar system in formation, in which leftover gas and dust in the disk surrounding a newborn star clump together to form planets. Credit: NASA/JPL-Caltech. ...
... Artist’s concept of a stellar system in formation, in which leftover gas and dust in the disk surrounding a newborn star clump together to form planets. Credit: NASA/JPL-Caltech. ...
Lecture103002
... nuclei get so close together the nuclear force repels them particles falling inward sent back outward up to 30,000 km/s ...
... nuclei get so close together the nuclear force repels them particles falling inward sent back outward up to 30,000 km/s ...
astr study guide ex 3 s`16
... 38. Where are elements heavier than iron can only be created ? 39. When the mass of a star's core becomes greater than 1.4 times the mass of the Sun, degenerate electrons can no longer keep it as a white dwarf. Instead, what does it become? 40. To predict whether a star will ultimately become a blac ...
... 38. Where are elements heavier than iron can only be created ? 39. When the mass of a star's core becomes greater than 1.4 times the mass of the Sun, degenerate electrons can no longer keep it as a white dwarf. Instead, what does it become? 40. To predict whether a star will ultimately become a blac ...
Document
... outer shell Core continues to collapse, outer shell expands because of hydrogen fusion, star becomes luminous Core becomes degenerate (sustained by electron pressure), outer shell dumps helium ash onto core Helium flash! Helium fusion (into carbon) begins in core Core helium fusion ends, eventually ...
... outer shell Core continues to collapse, outer shell expands because of hydrogen fusion, star becomes luminous Core becomes degenerate (sustained by electron pressure), outer shell dumps helium ash onto core Helium flash! Helium fusion (into carbon) begins in core Core helium fusion ends, eventually ...
20.1 Notes
... own gravity and rebounds with a shock wave that violently blows the stars outer layers from the core. This huge, bright explosion is called a Type II _________________________. If the core that remains after a supernova has a mass of 1.4 – 3 solar masses it becomes a _______________ star, a very den ...
... own gravity and rebounds with a shock wave that violently blows the stars outer layers from the core. This huge, bright explosion is called a Type II _________________________. If the core that remains after a supernova has a mass of 1.4 – 3 solar masses it becomes a _______________ star, a very den ...
Document
... • The result of the catastrophic collapse is the rebound and explosion of the core. • From start of collapse to now: 1 second! • Matter thrown back into the interstellar medium. • Matter rushing outwards, fuses with matter rushing inwards. • Every element after Fe is made in the instant of a superno ...
... • The result of the catastrophic collapse is the rebound and explosion of the core. • From start of collapse to now: 1 second! • Matter thrown back into the interstellar medium. • Matter rushing outwards, fuses with matter rushing inwards. • Every element after Fe is made in the instant of a superno ...
The light curves for a nova look like the following.
... v A supernova is more than a million times brighter than a nova. v In a matter of few months it radiates away as much energy as Sun will radiate in its entire 1010 yrs of life period. v A star can become supernova only once but it may become nova many times. v According to observations supernovae ar ...
... v A supernova is more than a million times brighter than a nova. v In a matter of few months it radiates away as much energy as Sun will radiate in its entire 1010 yrs of life period. v A star can become supernova only once but it may become nova many times. v According to observations supernovae ar ...
Chapter 3: Elements and the Periodic Table
... produce elements heavier than oxygen • Eventually, shrinks and its elements blow away o Forms a nebula – cloudlike region of gases. ...
... produce elements heavier than oxygen • Eventually, shrinks and its elements blow away o Forms a nebula – cloudlike region of gases. ...
Answer Key
... justifications must be in your own words. If you are unsure about a question, make an educated guess, and justify your guess (which can include why you can rule out certain choices from the list). If you get stuck, please seek assistance from your peers, the TA, or the professor. Note: It may be hel ...
... justifications must be in your own words. If you are unsure about a question, make an educated guess, and justify your guess (which can include why you can rule out certain choices from the list). If you get stuck, please seek assistance from your peers, the TA, or the professor. Note: It may be hel ...
Stars Notes
... • Outer layers continue to expand and form a planetary nebula • Remaining core is now a white dwarf which is dense and slowly cools and no longer produces energy ...
... • Outer layers continue to expand and form a planetary nebula • Remaining core is now a white dwarf which is dense and slowly cools and no longer produces energy ...
$doc.title
... “The aim of nuclear astrophysics is to understand those nuclear reacBons that shape much of the nature of the visible universe. Nuclear fusion is the engine of stars; it produces the energy that ...
... “The aim of nuclear astrophysics is to understand those nuclear reacBons that shape much of the nature of the visible universe. Nuclear fusion is the engine of stars; it produces the energy that ...
Document
... Type Ia Supernova White dwarf star with a massive binary companion. Accretion pushes white dwarf over the Chandrasekhar limit, causing thermonuclear disruption ...
... Type Ia Supernova White dwarf star with a massive binary companion. Accretion pushes white dwarf over the Chandrasekhar limit, causing thermonuclear disruption ...
test - Scioly.org
... 15. What is the name of the material spiraling around and into the left hand star? 16. Expressed in solar masses, a type 1a supernova will occur when the left hand star reaches what mass? 17. Expressed in kg, and in scientific notation, a type 1a supernova will occur when the left hand star reaches ...
... 15. What is the name of the material spiraling around and into the left hand star? 16. Expressed in solar masses, a type 1a supernova will occur when the left hand star reaches what mass? 17. Expressed in kg, and in scientific notation, a type 1a supernova will occur when the left hand star reaches ...
ASTRONOMY 1 ... You may use this only this study guide for reference... No electronic devises: I pads, lap tops, phones, etc.
... 38. Where are elements heavier than iron can only be created ? 39. When the mass of a star's core becomes greater than 1.4 times the mass of the Sun, degenerate electrons can no longer keep it as a white dwarf. Instead, what does it become? 40. To predict whether a star will ultimately become a blac ...
... 38. Where are elements heavier than iron can only be created ? 39. When the mass of a star's core becomes greater than 1.4 times the mass of the Sun, degenerate electrons can no longer keep it as a white dwarf. Instead, what does it become? 40. To predict whether a star will ultimately become a blac ...
Supernova
A supernova is a stellar explosion that briefly outshines an entire galaxy, radiating as much energy as the Sun or any ordinary star is expected to emit over its entire life span, before fading from view over several weeks or months. The extremely luminous burst of radiation expels much or all of a star's material at a velocity of up to 7007300000000000000♠30,000 km/s (10% of the speed of light), driving a shock wave into the surrounding interstellar medium. This shock wave sweeps up an expanding shell of gas and dust called a supernova remnant. Supernovae are potentially strong galactic sources of gravitational waves. A great proportion of primary cosmic rays comes from supernovae.Supernovae are more energetic than novae. Nova means ""new"" in Latin, referring to what appears to be a very bright new star shining in the celestial sphere; the prefix ""super-"" distinguishes supernovae from ordinary novae, which are far less luminous. The word supernova was coined by Walter Baade and Fritz Zwicky in 1931. It is pronounced /ˌsuːpərnoʊvə/ with the plural supernovae /ˌsuːpərnoʊviː/ or supernovas (abbreviated SN, plural SNe after ""supernovae"").Supernovae can be triggered in one of two ways: by the sudden re-ignition of nuclear fusion in a degenerate star; or by the gravitational collapse of the core of a massive star. In the first case, a degenerate white dwarf may accumulate sufficient material from a companion, either through accretion or via a merger, to raise its core temperature, ignite carbon fusion, and trigger runaway nuclear fusion, completely disrupting the star. In the second case, the core of a massive star may undergo sudden gravitational collapse, releasing gravitational potential energy that can create a supernova explosion.The most recent directly observed supernova in the Milky Way was Kepler's Star of 1604 (SN 1604); remnants of two more recent supernovae have been found retrospectively. Observations in other galaxies indicate that supernovae should occur on average about three times every century in the Milky Way, and that any galactic supernova would almost certainly be observable in modern astronomical equipment. Supernovae play a significant role in enriching the interstellar medium with higher mass elements. Furthermore, the expanding shock waves from supernova explosions can trigger the formation of new stars.