The Life Cycle of a Star
... dwarf forms from the core. • If it is of high mass, death occurs in a massive explosion known as a supernova, the remaining core then transforms into a neutron star or a black hole. ...
... dwarf forms from the core. • If it is of high mass, death occurs in a massive explosion known as a supernova, the remaining core then transforms into a neutron star or a black hole. ...
Physics@Brock - Brock University
... 42. In order to detect a black hole the astronomers look for (a) a spot into which stars and their planets fall. (b) a very intense source of infrared radiation. (c) a binary system where a companion star is not visible but it has a mass greater than 3 solar mass and is an intense X-ray source. (d) ...
... 42. In order to detect a black hole the astronomers look for (a) a spot into which stars and their planets fall. (b) a very intense source of infrared radiation. (c) a binary system where a companion star is not visible but it has a mass greater than 3 solar mass and is an intense X-ray source. (d) ...
Astronomy ANSWER KEY KEEP SECURE
... shown in the image above? Mira, Omicron-ceti 8. Which letter in the picture best approximates the location of material that was ejected from the surface of this star 20,000 years ago? (Local time frame of reference.) B, according to Dr. Robert Hurt, Hidden Universe Showcase, the entire tail represen ...
... shown in the image above? Mira, Omicron-ceti 8. Which letter in the picture best approximates the location of material that was ejected from the surface of this star 20,000 years ago? (Local time frame of reference.) B, according to Dr. Robert Hurt, Hidden Universe Showcase, the entire tail represen ...
Lecture Nine (Powerpoint format) - FLASH Center for Computational
... times mass sun) is similar to that of lower-mass stars through the beginning stages, except far more rapid due to its greater mass burning rate. Where a 1 solar mass star spends 10 billion years reaching the red giant stage, a 10 solar mass star may reach the same evolutionary point in just 10 mil ...
... times mass sun) is similar to that of lower-mass stars through the beginning stages, except far more rapid due to its greater mass burning rate. Where a 1 solar mass star spends 10 billion years reaching the red giant stage, a 10 solar mass star may reach the same evolutionary point in just 10 mil ...
The origin, life, and death of stars
... actually has nothing to do with planets, but we didn’t know that in the 18th century when Herschel coined the term) The core collapses to form a White Dwarf ...
... actually has nothing to do with planets, but we didn’t know that in the 18th century when Herschel coined the term) The core collapses to form a White Dwarf ...
The Lives of Stars
... M > 8 Msun à Supernova + neutron star or a black hole n 0.08 Msun < M < 8 Msun à White dwarf n M < 0.08 Msun à Brown dwarf (fusion never ...
... M > 8 Msun à Supernova + neutron star or a black hole n 0.08 Msun < M < 8 Msun à White dwarf n M < 0.08 Msun à Brown dwarf (fusion never ...
More detailed notes - Particle Physics and Particle Astrophysics
... need to heat the hydrogen just outside the core by a small amount to initiate fusion, whereas you’d have to heat the helium by at least a factor of 5.) When this happens, the resulting increase in internal pressure is more than enough to stop the star shrinking: instead the outer layers expand and c ...
... need to heat the hydrogen just outside the core by a small amount to initiate fusion, whereas you’d have to heat the helium by at least a factor of 5.) When this happens, the resulting increase in internal pressure is more than enough to stop the star shrinking: instead the outer layers expand and c ...
Lives of Stars - Madison County Schools
... outshine the entire galaxy (300,000,000,000 stars) it was in. Supernovae can be seen from Earth. There are historic records of some stars that were so bright that they could be seen during the day for weeks at a time. ...
... outshine the entire galaxy (300,000,000,000 stars) it was in. Supernovae can be seen from Earth. There are historic records of some stars that were so bright that they could be seen during the day for weeks at a time. ...
January 2006
... enough to sustain nuclear fusion • Stage 7: Main-sequence star; pressure from nuclear fusion and gravity are in balance – Duration ~ 10 billion years (much longer than all other stages combined) – Temperature ~ 15 million K at core, 6000 K at surface – Size ~ Sun ...
... enough to sustain nuclear fusion • Stage 7: Main-sequence star; pressure from nuclear fusion and gravity are in balance – Duration ~ 10 billion years (much longer than all other stages combined) – Temperature ~ 15 million K at core, 6000 K at surface – Size ~ Sun ...
Stellar Classification and Evolution What is a star? A cloud of gas
... from helium fusion _____________ much of their mass The ejected material expands and cools, becoming a planetary ________________ (which actually has nothing to do with planets, but we didn’t know that in the 18th century when Herschel coined the term) The core _____________________ to form a Wh ...
... from helium fusion _____________ much of their mass The ejected material expands and cools, becoming a planetary ________________ (which actually has nothing to do with planets, but we didn’t know that in the 18th century when Herschel coined the term) The core _____________________ to form a Wh ...
Lesson 3 Power Notes Outline
... When nearly all the hydrogen in a star’s core has fused into helium, the core contracts under its own gravity and its temperature rises. ...
... When nearly all the hydrogen in a star’s core has fused into helium, the core contracts under its own gravity and its temperature rises. ...
Stellar Evolution - Hays High School
... Star has settled into the most stable part of its life Converts hydrogen to helium (H => He) Next step depends on the mass of the star Three different examples of stars: 1. Stars similar to our Sun 2. Stars several times more massive than the Sun 3. HUGE HUMONGOUS stars, VERY massive ...
... Star has settled into the most stable part of its life Converts hydrogen to helium (H => He) Next step depends on the mass of the star Three different examples of stars: 1. Stars similar to our Sun 2. Stars several times more massive than the Sun 3. HUGE HUMONGOUS stars, VERY massive ...
doc - University of Texas Astronomy
... onto a white dwarf. This is in fact how we claimed white dwarfs could become supernovae, carbon detonation supernovae. Interpretation: rotating “lighthouse model.” (Fig. 22.3) Rotation slows down with time, on a timescale of about a million years. ...
... onto a white dwarf. This is in fact how we claimed white dwarfs could become supernovae, carbon detonation supernovae. Interpretation: rotating “lighthouse model.” (Fig. 22.3) Rotation slows down with time, on a timescale of about a million years. ...
THE LIFE CYCLE OF STARS
... globule increases, as the atoms are in closer proximity. Also, the globule rotates faster and faster. This spinning action causes an increase in centrifugal forces (a radial force on spinning objects) that causes the globule to have a central core and a surrounding flattened disk of dust (called a p ...
... globule increases, as the atoms are in closer proximity. Also, the globule rotates faster and faster. This spinning action causes an increase in centrifugal forces (a radial force on spinning objects) that causes the globule to have a central core and a surrounding flattened disk of dust (called a p ...
Acting Out the Life Cycle of Stars - University of Texas Astronomy
... As a class, we’re going to act out the life cycle of stars. Each of you will represent a small clump of gas, mostly made of hydrogen (since that’s by far the most abundant element in the Universe). a. We all start in random motion, wandering around aimlessly, mostly ignoring all other clumps of gas. ...
... As a class, we’re going to act out the life cycle of stars. Each of you will represent a small clump of gas, mostly made of hydrogen (since that’s by far the most abundant element in the Universe). a. We all start in random motion, wandering around aimlessly, mostly ignoring all other clumps of gas. ...
d - Haus der Astronomie
... By averaging, we find the approximate distance to the Andromeda Galaxy: (2,52 ± 0,14) 10 lyly ...
... By averaging, we find the approximate distance to the Andromeda Galaxy: (2,52 ± 0,14) 10 lyly ...
Fate of Stars
... Stellar Explosions For heavy white dwarves with a companion star • Acquire mass, if becomes > 1.4 M(Sun) SUPERNOVA (Ia). p + e ! n + neutrino • Usually leaves neutron star For high mass stars • Fusion continues beyond C,O • Core of degenerate electrons builds up - opposes gravity • If Mass(cor ...
... Stellar Explosions For heavy white dwarves with a companion star • Acquire mass, if becomes > 1.4 M(Sun) SUPERNOVA (Ia). p + e ! n + neutrino • Usually leaves neutron star For high mass stars • Fusion continues beyond C,O • Core of degenerate electrons builds up - opposes gravity • If Mass(cor ...
11. Dead Stars
... Why Do Neutron Stars Spin So Fast? Conservation of angular momentum: before collapsing, the star’s core probably rotates once every few hours. Collapse by a factor of x decreases the rotation period by a factor of x2. The core collapses by roughly a factor of 1000, so it spins about ...
... Why Do Neutron Stars Spin So Fast? Conservation of angular momentum: before collapsing, the star’s core probably rotates once every few hours. Collapse by a factor of x decreases the rotation period by a factor of x2. The core collapses by roughly a factor of 1000, so it spins about ...
NASC 1100
... Spectral Type The surface temperature also determines the line spectrum of a star. Hot stars display lines of highly ionized elements, while cool stars show molecular lines. Stars are classified by assigning a spectral type. The hottest stars are called spectral type O, followed by B, A, F, G, K, M ...
... Spectral Type The surface temperature also determines the line spectrum of a star. Hot stars display lines of highly ionized elements, while cool stars show molecular lines. Stars are classified by assigning a spectral type. The hottest stars are called spectral type O, followed by B, A, F, G, K, M ...
Test #3
... b. the Earth would jump to a smaller orbit c. the size of the Earth's orbit would increase rapidly d. the Earth's orbit would remain the same 2. A neutron star is expected to spin rapidly because a. they conserved angular momentum when they collapsed. b. they have high orbital velocities. c. they ha ...
... b. the Earth would jump to a smaller orbit c. the size of the Earth's orbit would increase rapidly d. the Earth's orbit would remain the same 2. A neutron star is expected to spin rapidly because a. they conserved angular momentum when they collapsed. b. they have high orbital velocities. c. they ha ...
The Genesis of the Elements
... It has the lowest mass per nuclear particle of any element It can not fuse into another element without creating mass ...
... It has the lowest mass per nuclear particle of any element It can not fuse into another element without creating mass ...
Stellar Explosions
... A supernova is a one-time event Once it happens, there is little or nothing left of the progenitor star There are two different types of supernovae, both equally common Type I - which is a carbon-detonation supernova, and Type II - which is the death of a high-mass star just described Astronomy 1-2 ...
... A supernova is a one-time event Once it happens, there is little or nothing left of the progenitor star There are two different types of supernovae, both equally common Type I - which is a carbon-detonation supernova, and Type II - which is the death of a high-mass star just described Astronomy 1-2 ...
Strongly Interacting Supernovae - The National Centre for Radio
... Initial spectrum shows Type Ib and later spectrum ...
... Initial spectrum shows Type Ib and later spectrum ...
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.