Lecture 17, PPT version
... Gamma rays are VERY high energy light, inherently rare for them to be emitted by astronomical objects Bursts discovered in early 1960’s, randomly distributed around the sky, a few per week, may have complex light curves, but they don’t repeat ...
... Gamma rays are VERY high energy light, inherently rare for them to be emitted by astronomical objects Bursts discovered in early 1960’s, randomly distributed around the sky, a few per week, may have complex light curves, but they don’t repeat ...
Death - Wayne State University Physics and Astronomy
... • An isolated white dwarf has a boring future: it simply cools off, dimming to invisibility • White dwarfs in binary systems where the companion is still a main sequence or red giant star can have more interesting futures • If the white dwarf is close enough to its red giant or main sequence compani ...
... • An isolated white dwarf has a boring future: it simply cools off, dimming to invisibility • White dwarfs in binary systems where the companion is still a main sequence or red giant star can have more interesting futures • If the white dwarf is close enough to its red giant or main sequence compani ...
AY1 Homework for Quiz 2: Spring 2017
... ___ A. It will have become slightly more massive than the Sun is now because lightweight hydrogen has been converted into heavier Helium ___ B. It will be enriched in helium compared to the Sun ___ ...
... ___ A. It will have become slightly more massive than the Sun is now because lightweight hydrogen has been converted into heavier Helium ___ B. It will be enriched in helium compared to the Sun ___ ...
Astrophysics 12 - Stellar Evolution
... remain there while it fuses hydrogen to helium. Core hydrogen “burning” ...
... remain there while it fuses hydrogen to helium. Core hydrogen “burning” ...
Introduction to Stellar Evolution
... Open / Galactic Star Cluster NGC6791 -- 8 Billion Years, 2-3 x solar metals ...
... Open / Galactic Star Cluster NGC6791 -- 8 Billion Years, 2-3 x solar metals ...
Stages of stars - University of Dayton
... >May remain on main sequence for up to 100 billion years >Never evolve to become bloated red giants >Remain as stable main sequence stars until they consume their hydrogen fuel and collapse into white dwarfs Death of Massive Stars: >Have relatively short life spans >Terminate in an explosion known a ...
... >May remain on main sequence for up to 100 billion years >Never evolve to become bloated red giants >Remain as stable main sequence stars until they consume their hydrogen fuel and collapse into white dwarfs Death of Massive Stars: >Have relatively short life spans >Terminate in an explosion known a ...
STARS
... • Core runs out of He, and is no longer able to fuse the remaining heavier elements • The star blows its outer layer away • The core remains behind and burns as a white dwarf • Eventually it cools to become a black dwarf ...
... • Core runs out of He, and is no longer able to fuse the remaining heavier elements • The star blows its outer layer away • The core remains behind and burns as a white dwarf • Eventually it cools to become a black dwarf ...
The Life of a Star
... core of the red giant. – The remaining core is called a white dwarf. Over time, the white dwarf cools off and becomes a black dwarf. Planetary Nebula: A collection of gas and dust that was formed during the dying phases of a star ...
... core of the red giant. – The remaining core is called a white dwarf. Over time, the white dwarf cools off and becomes a black dwarf. Planetary Nebula: A collection of gas and dust that was formed during the dying phases of a star ...
slides
... The distance from Earth of the red supergiant Betelgeuse is approximately 643 light-years. If it were to explode as a supernova, it would be one of the brightest stars in the sky. Right now, the brightest star other than the Sun is Sirius, with a luminosity of 26LSun and a distance of 8.6 light-year ...
... The distance from Earth of the red supergiant Betelgeuse is approximately 643 light-years. If it were to explode as a supernova, it would be one of the brightest stars in the sky. Right now, the brightest star other than the Sun is Sirius, with a luminosity of 26LSun and a distance of 8.6 light-year ...
The Life Cycles of Stars
... supernova. Neutron stars spin rapidly giving off radio waves. If the radio waves are emitted in pulses (due to the star’s spin), these neutron stars are called pulsars. The core of a massive star that has 8 or more times the mass of our Sun remains massive after the supernova. No nuclear fusion is t ...
... supernova. Neutron stars spin rapidly giving off radio waves. If the radio waves are emitted in pulses (due to the star’s spin), these neutron stars are called pulsars. The core of a massive star that has 8 or more times the mass of our Sun remains massive after the supernova. No nuclear fusion is t ...
The Life Cycles of Stars, Part II
... supernova. Neutron stars spin rapidly giving off radio waves. If the radio waves are emitted in pulses (due to the star’s spin), these neutron stars are called pulsars. The core of a massive star that has 8 or more times the mass of our Sun remains massive after the supernova. No nuclear fusion is t ...
... supernova. Neutron stars spin rapidly giving off radio waves. If the radio waves are emitted in pulses (due to the star’s spin), these neutron stars are called pulsars. The core of a massive star that has 8 or more times the mass of our Sun remains massive after the supernova. No nuclear fusion is t ...
Using Galaxy Clusters to Study Structure Evolution
... – Certain types of stars (Cepheid variables) – Spiral galaxies – Certain types of supernovae (Type Ia SNe) Exploding white dwarfs Emit as much light as an entire galaxy, so can be detected at great distances ...
... – Certain types of stars (Cepheid variables) – Spiral galaxies – Certain types of supernovae (Type Ia SNe) Exploding white dwarfs Emit as much light as an entire galaxy, so can be detected at great distances ...
presentation source
... Star Death: High Mass Stars • MS to Red Giant to Supergiant to Supernova to Neutron Star or Black Hole. • Nuclear fusion continues in shells to iron. • Protons + electrons fuse to neutrons. • Unstable, collapses in <1s. Bounce off rigid core detonates star - Supernova! • Shines as brightly as galax ...
... Star Death: High Mass Stars • MS to Red Giant to Supergiant to Supernova to Neutron Star or Black Hole. • Nuclear fusion continues in shells to iron. • Protons + electrons fuse to neutrons. • Unstable, collapses in <1s. Bounce off rigid core detonates star - Supernova! • Shines as brightly as galax ...
The Hidden Lives of Galaxies NSTA 2001
... How does the sun produce energy? How is fusion different from bonding? Do small stars or large stars burn faster? Do small stars or large stars burn hotter? When does fusion stop in a red ...
... How does the sun produce energy? How is fusion different from bonding? Do small stars or large stars burn faster? Do small stars or large stars burn hotter? When does fusion stop in a red ...
Final Review Sheet
... are hot, most are currently strong ultraviolet emitters. Billions of years in the future they will grow cool and invisible, but they are permanently stable. They evolve in the HR diagram along a line of nearly constant radius below the main sequence, sliding slowly from left (hi T) to right (low T, ...
... are hot, most are currently strong ultraviolet emitters. Billions of years in the future they will grow cool and invisible, but they are permanently stable. They evolve in the HR diagram along a line of nearly constant radius below the main sequence, sliding slowly from left (hi T) to right (low T, ...
The Family of Stars
... Low luminosity; high temperature => White dwarfs are found in the lower center/left of the H-R diagram. ...
... Low luminosity; high temperature => White dwarfs are found in the lower center/left of the H-R diagram. ...
Nobel Prize in Physics for Accelerating Universe
... When hydrogen burning in the core stops, a star like the Sun begins to evolve A) To higher surface temperature and higher luminosity B) To lower surface temperature and higher luminosity C) To higher surface temperature and lower luminosity D) To lower surface temperature and lower luminosity E) Up ...
... When hydrogen burning in the core stops, a star like the Sun begins to evolve A) To higher surface temperature and higher luminosity B) To lower surface temperature and higher luminosity C) To higher surface temperature and lower luminosity D) To lower surface temperature and lower luminosity E) Up ...
Common Envelope Evolution Leading to Supernovae with Dense
... The suggested sequence of events leading to supernovae with dense environments is shown in Figure 1. The starting point is two massive stars in a binary. The more massive star evolves, transfers mass to its companion, and explodes as a supernova, leaving a neutron star (NS) or, less likely, a black ...
... The suggested sequence of events leading to supernovae with dense environments is shown in Figure 1. The starting point is two massive stars in a binary. The more massive star evolves, transfers mass to its companion, and explodes as a supernova, leaving a neutron star (NS) or, less likely, a black ...
Birth, Lives, and Death of Stars
... left over from when the star was still producing energy from nuclear reactions. There are no more nuclear reactions occurring so the white dwarf cools off from an initial temperature of about 100,000 K. The white dwarf loses heat quickly at first cooling off to 20,000 K in only about 100 million yea ...
... left over from when the star was still producing energy from nuclear reactions. There are no more nuclear reactions occurring so the white dwarf cools off from an initial temperature of about 100,000 K. The white dwarf loses heat quickly at first cooling off to 20,000 K in only about 100 million yea ...
Module G - U1_ L3 - Life Cycle of Stars
... A black hole is an invisible object with gravity so great that nothing, not even light, can escape it. Although black holes are invisible, they can be observed by the gravitational effect they have on their surroundings. Matter swirls around a black hole just before being pulled in. The matter becom ...
... A black hole is an invisible object with gravity so great that nothing, not even light, can escape it. Although black holes are invisible, they can be observed by the gravitational effect they have on their surroundings. Matter swirls around a black hole just before being pulled in. The matter becom ...
Stars III - Indiana University Astronomy
... • Sun-like stars with <2MSun have long lives, never become hot enough to fuse carbon nuclei, and end as white dwarfs • Intermediate mass stars can make elements heavier than carbon but end as white dwarfs ...
... • Sun-like stars with <2MSun have long lives, never become hot enough to fuse carbon nuclei, and end as white dwarfs • Intermediate mass stars can make elements heavier than carbon but end as white dwarfs ...
Observational properties of stars
... concentrated into a point). The object was visible in the sky for 2 years. A supernova remnant is associated with this event, and currently it is thought to have been a Type Ia. SN1054 – (July 4) in Taurus, observed by Arabic, Chinese, Japanese astronomers, peak of V = -6, again brighter than Venus. ...
... concentrated into a point). The object was visible in the sky for 2 years. A supernova remnant is associated with this event, and currently it is thought to have been a Type Ia. SN1054 – (July 4) in Taurus, observed by Arabic, Chinese, Japanese astronomers, peak of V = -6, again brighter than Venus. ...
The Sun: Example of Radiation Laws
... High-mass stars (M > 8M⊙ ) evolve into both red and blue giants and supergiants as their cores burn heavier and heavier elements. ...
... High-mass stars (M > 8M⊙ ) evolve into both red and blue giants and supergiants as their cores burn heavier and heavier elements. ...
Chapter 13 Practice Questions
... 12. During its life, a massive star creates heavier and heavier elements in its core through thermonuclear fusion, leading up to silicon and iron. What is the fate of the iron that is ...
... 12. During its life, a massive star creates heavier and heavier elements in its core through thermonuclear fusion, leading up to silicon and iron. What is the fate of the iron that is ...
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.