Life of stars, formation of elements
... • Many more similar starformation regions buried deep inside cloud. ...
... • Many more similar starformation regions buried deep inside cloud. ...
The Sun is a mass of Incandescent Gas
... The Sun and other stars are really only roughly in equilibrium. The Sun is extremely dynamic, and has storms larger than the Earth. ...
... The Sun and other stars are really only roughly in equilibrium. The Sun is extremely dynamic, and has storms larger than the Earth. ...
The Lives and Deaths of Stars
... Universe in the Parks program The University of Wisconsin-Madison Department of Astronomy ...
... Universe in the Parks program The University of Wisconsin-Madison Department of Astronomy ...
Micro_lect20a
... • Supernova produce all of the heavier elements – Elements up to Iron can be produced by fusion – Elements heavier than Iron are produced by the neutrons and neutrinos interacting with nuclei during the supernova explosion ...
... • Supernova produce all of the heavier elements – Elements up to Iron can be produced by fusion – Elements heavier than Iron are produced by the neutrons and neutrinos interacting with nuclei during the supernova explosion ...
The Main Sequence
... • How dense can something get? • How strong can the force of gravity be? • What if the escape velocity is faster than light? ...
... • How dense can something get? • How strong can the force of gravity be? • What if the escape velocity is faster than light? ...
Stars: Their Life and Afterlife
... not only tend to form close together in space, but also in time – and so, for massive stars, they will also die relatively close together in space and time. Superbubbles form from OB associations. OB associations are clusters of massive stars of spectral types – you guessed it – O and B. • O stars a ...
... not only tend to form close together in space, but also in time – and so, for massive stars, they will also die relatively close together in space and time. Superbubbles form from OB associations. OB associations are clusters of massive stars of spectral types – you guessed it – O and B. • O stars a ...
South Pasadena • Chemistry Name 8 • Nuclear Chemistry Period
... 1. What chemical element is the primary constituent of a young star? 2. Name the astrophysicist who first advanced the idea that the chemical elements originated from hydrogen in stars. 3. Name the stellar process in which the fusion of hydrogen produces other elements. 4. Why is iron the heaviest e ...
... 1. What chemical element is the primary constituent of a young star? 2. Name the astrophysicist who first advanced the idea that the chemical elements originated from hydrogen in stars. 3. Name the stellar process in which the fusion of hydrogen produces other elements. 4. Why is iron the heaviest e ...
Birth and Life of a Star
... them very dense. The heavier the white dwarf is, then the smaller its size will be. A star like our Sun will become a white dwarf when it has run out of fuel. Near the end of its life, it will go through a red giant stage, and then lose most of its gas, until what is left settles down and becomes a ...
... them very dense. The heavier the white dwarf is, then the smaller its size will be. A star like our Sun will become a white dwarf when it has run out of fuel. Near the end of its life, it will go through a red giant stage, and then lose most of its gas, until what is left settles down and becomes a ...
Birth and Life of a Star
... them very dense. The heavier the white dwarf is, then the smaller its size will be. A star like our Sun will become a white dwarf when it has run out of fuel. Near the end of its life, it will go through a red giant stage, and then lose most of its gas, until what is left settles down and becomes a ...
... them very dense. The heavier the white dwarf is, then the smaller its size will be. A star like our Sun will become a white dwarf when it has run out of fuel. Near the end of its life, it will go through a red giant stage, and then lose most of its gas, until what is left settles down and becomes a ...
Stellar Evolution
... A supernova may explode so violently that the remaining core is compressed into an infinitely small, infinitely dense black hole. Black hole’s have such a strong gravitational pull that even light can not escape if it gets any closer than the event horizon. The radius, R, at which a body of ma ...
... A supernova may explode so violently that the remaining core is compressed into an infinitely small, infinitely dense black hole. Black hole’s have such a strong gravitational pull that even light can not escape if it gets any closer than the event horizon. The radius, R, at which a body of ma ...
Part B
... • Extremely rare (a few per galaxy per million years). They are the most luminous electromagnetic events known to occur in the Universe. • First detected in 1967 by the Vela satellites, • Redshifts clarified their distance and combined with their luminosity connected them to the deaths of massive st ...
... • Extremely rare (a few per galaxy per million years). They are the most luminous electromagnetic events known to occur in the Universe. • First detected in 1967 by the Vela satellites, • Redshifts clarified their distance and combined with their luminosity connected them to the deaths of massive st ...
File - Physical Science
... hydrogen becomes depleted, high mass stars convert helium atoms into carbon and oxygen, followed by the fusion of carbon and oxygen into neon, sodium, magnesium, sulfur and silicon. Later reactions transform these elements into calcium, iron, nickel, chromium, copper and others. When these old, larg ...
... hydrogen becomes depleted, high mass stars convert helium atoms into carbon and oxygen, followed by the fusion of carbon and oxygen into neon, sodium, magnesium, sulfur and silicon. Later reactions transform these elements into calcium, iron, nickel, chromium, copper and others. When these old, larg ...
Astronomy 242: Review Questions #1 Distributed: February 10
... (a) Using the information in this diagram, estimate the range of surface gravities g for stars along the Main Sequence. Which end of the main sequence has the highest surface gravities? (b) Typical white dwarf stars have masses Mwd ≃ 1M⊙ . How do the surface gravities of white dwarf stars compare to ...
... (a) Using the information in this diagram, estimate the range of surface gravities g for stars along the Main Sequence. Which end of the main sequence has the highest surface gravities? (b) Typical white dwarf stars have masses Mwd ≃ 1M⊙ . How do the surface gravities of white dwarf stars compare to ...
galaxies - GEOCITIES.ws
... – How are stars born? • When a heavy body passes near or through the nebula, its gravity causes swirls and ripples. It is no different in a nebula when a star passes by. The "piles" of matter continue to group together in the nebula until they are gigantic clumps of dust and gas. • At this stage, t ...
... – How are stars born? • When a heavy body passes near or through the nebula, its gravity causes swirls and ripples. It is no different in a nebula when a star passes by. The "piles" of matter continue to group together in the nebula until they are gigantic clumps of dust and gas. • At this stage, t ...
Lecture 1
... During the AGB phase, spare neutrons react with other elements in the star to build up "heavier" elements, all the way to Pb. During the planetary nebula phase, these elements (along with the H and He) are put back into space for future generations of stars to use. ...
... During the AGB phase, spare neutrons react with other elements in the star to build up "heavier" elements, all the way to Pb. During the planetary nebula phase, these elements (along with the H and He) are put back into space for future generations of stars to use. ...
Life of a star - bahringcarthnoians
... bright and cause a burst of radiation that often briefly outshines a galaxy, before fading from view. During this short time a supernova can radiate as much energy as the Sun is expected to emit over its entire life span. The Big Bang produced hydrogen, helium, and traces of lithium, while all heavi ...
... bright and cause a burst of radiation that often briefly outshines a galaxy, before fading from view. During this short time a supernova can radiate as much energy as the Sun is expected to emit over its entire life span. The Big Bang produced hydrogen, helium, and traces of lithium, while all heavi ...
Chapter 12 Stellar Evolution
... A star of more than 8 solar masses can fuse elements far beyond carbon in its core, leading to a very different fate. Its path across the H–R diagram is essentially a straight line – it stays at just about the same luminosity as it cools off. Eventually the star dies in a violent explosion called a ...
... A star of more than 8 solar masses can fuse elements far beyond carbon in its core, leading to a very different fate. Its path across the H–R diagram is essentially a straight line – it stays at just about the same luminosity as it cools off. Eventually the star dies in a violent explosion called a ...
Structure of the Universe
... Spectroscopic Parallax -- Have to be able to resolve star and it must be bright enough to get a spectrum ...
... Spectroscopic Parallax -- Have to be able to resolve star and it must be bright enough to get a spectrum ...
The life-cycle of stars - Young Scientists Journal
... process where atoms fall into the clump and become part of the protostar is called accretion. To become a star, the protostar will need to achieve hydrostatic equilibrium by balancing the gravity, pulling atoms in, and the radiation pressure pushing heat and light out. When equilibrium is achieved, ...
... process where atoms fall into the clump and become part of the protostar is called accretion. To become a star, the protostar will need to achieve hydrostatic equilibrium by balancing the gravity, pulling atoms in, and the radiation pressure pushing heat and light out. When equilibrium is achieved, ...
Document
... b) the end result of massive star evolution c) objects that are not quite massive enough to be stars d) cooled off white dwarfs e) the objects at the centers of planetary nebulae 29. What is not the same for each star in a cluster? a) age, b) mass, c) composition, d) distance from Earth 30. Nearly a ...
... b) the end result of massive star evolution c) objects that are not quite massive enough to be stars d) cooled off white dwarfs e) the objects at the centers of planetary nebulae 29. What is not the same for each star in a cluster? a) age, b) mass, c) composition, d) distance from Earth 30. Nearly a ...
ULTRASAT in a nutshell (Feb 2017)
... - Instantaneous >50% of sky (8 times better than ground based), in <5 min for >2.5hr. - GW error box in a single image. - Sensitive out to 200 Mpc to early UV signals predicted in common models. ...
... - Instantaneous >50% of sky (8 times better than ground based), in <5 min for >2.5hr. - GW error box in a single image. - Sensitive out to 200 Mpc to early UV signals predicted in common models. ...
Stars 3
... The blue glow in the inner part of the nebula -- light emitted by energetic electrons as they spiral through the Crab’s magnetic field -- is powered by the Crab Pulsar. The picture on the right shows a Hubble Space Telescope image of the inner parts of the Crab. The pulsar itself is visible as the l ...
... The blue glow in the inner part of the nebula -- light emitted by energetic electrons as they spiral through the Crab’s magnetic field -- is powered by the Crab Pulsar. The picture on the right shows a Hubble Space Telescope image of the inner parts of the Crab. The pulsar itself is visible as the l ...
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.