Big Bang, 429
... 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 ...
Supernovae
... Neutrinos (Cont.) • Neutrinos detected consistent with number expected from supernova in LMC in Feb 1987. • Probably type II SN because originator was massive B star (20 M) • Neutrinos are rarely absorbed so energy changed little over many x 10 9 years (except for loss due to expansion of Universe ...
... Neutrinos (Cont.) • Neutrinos detected consistent with number expected from supernova in LMC in Feb 1987. • Probably type II SN because originator was massive B star (20 M) • Neutrinos are rarely absorbed so energy changed little over many x 10 9 years (except for loss due to expansion of Universe ...
lecture22
... Iron cores do not immediately collapse due to electron degeneracy pressure. If the density continues to rise, eventually the electrons are forced to combine with the protons – resulting in neutrons. What comes next … is core collapse. ...
... Iron cores do not immediately collapse due to electron degeneracy pressure. If the density continues to rise, eventually the electrons are forced to combine with the protons – resulting in neutrons. What comes next … is core collapse. ...
Lecture 9/10 Stellar evolution Ulf Torkelsson 1 Main sequence stars
... the star, but in the extreme conditions that are now present in the core, the stellar material becomes opaque even to neutrinos, and these may give a push to the shock wave such that it gains momentum and continues outward. The shock wave eventually reaches the stellar surface after a few hours, at ...
... the star, but in the extreme conditions that are now present in the core, the stellar material becomes opaque even to neutrinos, and these may give a push to the shock wave such that it gains momentum and continues outward. The shock wave eventually reaches the stellar surface after a few hours, at ...
Circumstellar interaction in supernovae
... • Implosion turns into explosion • Neutron star remnant at the centre. • Explosion with 1053 ergs energy • 99% in neutrinos and 1 % in ElectroMagnetic • Scatter all heavy material required for life ...
... • Implosion turns into explosion • Neutron star remnant at the centre. • Explosion with 1053 ergs energy • 99% in neutrinos and 1 % in ElectroMagnetic • Scatter all heavy material required for life ...
The Life Cycle of a Star
... the star has ignited, it becomes a main sequence star. Main Sequence stars fuse hydrogen to form helium, releasing enormous amounts of energy. It takes about 10 billion years to consume all the hydrogen in a Main Sequence star. ...
... the star has ignited, it becomes a main sequence star. Main Sequence stars fuse hydrogen to form helium, releasing enormous amounts of energy. It takes about 10 billion years to consume all the hydrogen in a Main Sequence star. ...
File
... *99 percent of that energy is in the form of neutrinos. *This flood of neutrinos carries large amounts of energy out of the core—allowing it to collapse further. ...
... *99 percent of that energy is in the form of neutrinos. *This flood of neutrinos carries large amounts of energy out of the core—allowing it to collapse further. ...
Due: January 15, 2014 Name
... b. a rapidly rotating shell of gas, dust, and radiation, but no central object. c. a rapidly expanding shell of gas and a compact white dwarf star at its center. d. nothing, the explosion changes all the matter completely into energy, which then radiates into space at the speed of light. ...
... b. a rapidly rotating shell of gas, dust, and radiation, but no central object. c. a rapidly expanding shell of gas and a compact white dwarf star at its center. d. nothing, the explosion changes all the matter completely into energy, which then radiates into space at the speed of light. ...
Document
... 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 supernova! ...
... 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 supernova! ...
Stars and Space - science
... • As it swells, it cools and turns red – a red giant. • When all the light elements in the core have fused, fusion stops. The star collapses on itself and heats up to become a white dwarf. • Smaller stars (like our Sun) then fade out and go cold. AQA Science © Nelson Thornes Ltd 2006 ...
... • As it swells, it cools and turns red – a red giant. • When all the light elements in the core have fused, fusion stops. The star collapses on itself and heats up to become a white dwarf. • Smaller stars (like our Sun) then fade out and go cold. AQA Science © Nelson Thornes Ltd 2006 ...
Parallax
... use Light Years when calculating Distances Light travels at 3.00 x 10^8 m/s • How far does it travel in one year? ...
... use Light Years when calculating Distances Light travels at 3.00 x 10^8 m/s • How far does it travel in one year? ...
What stars do Summary: Nuclear burning in stars •
... • For M > 7-8 M , stars end up with iron cores No further nuclear burning possible • Core eventually becomes too massive to be held up by degenerate electron pressure: • e- + p n • Sudden core collapse: 104 km 20 km • Then core rebounds • Outer layers fall in, then get hit by rebounding core. ...
... • For M > 7-8 M , stars end up with iron cores No further nuclear burning possible • Core eventually becomes too massive to be held up by degenerate electron pressure: • e- + p n • Sudden core collapse: 104 km 20 km • Then core rebounds • Outer layers fall in, then get hit by rebounding core. ...
07-01TheColsmologicalDistanceLadder
... • A sub-Chandrasekhar white dwarf • A less dense companion star 2. Gravity strips material off companion star 3. Dwarf gets more and more massive 4. Mass exceeds Chandrasekhar limit (1.4 Msun) 5. Kablooey 6. Kablooey has a certain absolute magnitude 7. Kablooey is very very bright. 8. Use apparent/a ...
... • A sub-Chandrasekhar white dwarf • A less dense companion star 2. Gravity strips material off companion star 3. Dwarf gets more and more massive 4. Mass exceeds Chandrasekhar limit (1.4 Msun) 5. Kablooey 6. Kablooey has a certain absolute magnitude 7. Kablooey is very very bright. 8. Use apparent/a ...
powerpoints - Georgia Southern University Astrophysics
... Concepts • Astronomers make 3 color diagrams to represent 3 pieces of information visually. For example, 3 different emission line features. • Spectral lines are like fingerprints, they are unique to the element or molecule that emitted (or absorbed) them due to the unique electronic energy levels ...
... Concepts • Astronomers make 3 color diagrams to represent 3 pieces of information visually. For example, 3 different emission line features. • Spectral lines are like fingerprints, they are unique to the element or molecule that emitted (or absorbed) them due to the unique electronic energy levels ...
Stars
... When a Type II supernova first becomes visible, the temperature of the expanding cloud of debris is so high that most radiation is emitted as ultraviolet light. As the cloud expands, its temperature drops. One week after the explosion, the temperature has fallen to 6000 K and the cloud radiates most ...
... When a Type II supernova first becomes visible, the temperature of the expanding cloud of debris is so high that most radiation is emitted as ultraviolet light. As the cloud expands, its temperature drops. One week after the explosion, the temperature has fallen to 6000 K and the cloud radiates most ...
22 Stellar Remnant/HR Diagram
... Assigned a letter in alphabetical order from complex looking to simple looking (A-Q) Later they figured out that these lines were absorption lines corresponding to different elements Re-ordered according to which elements were strong (usually H): OBAFGKM was born! ...
... Assigned a letter in alphabetical order from complex looking to simple looking (A-Q) Later they figured out that these lines were absorption lines corresponding to different elements Re-ordered according to which elements were strong (usually H): OBAFGKM was born! ...
Black Hole
... Black holes of a few solar masses are believed to form when massive stars undergo core collapse if the collapsed core exceeds the maximum of ~ 3 M permitted for neutron stars. The best evidence for such black holes comes from binary stars. Single-line spectroscopic binaries Some stars have spectral ...
... Black holes of a few solar masses are believed to form when massive stars undergo core collapse if the collapsed core exceeds the maximum of ~ 3 M permitted for neutron stars. The best evidence for such black holes comes from binary stars. Single-line spectroscopic binaries Some stars have spectral ...
black hole - Purdue Physics
... force according to Newton’s Law, just like any star of the same mass • Only at a distance of 3 Rs from the black hole will the gravity increase from what Newton’s Law predicts. – then one could eventually fall into the black hole, if you get rid of your ...
... force according to Newton’s Law, just like any star of the same mass • Only at a distance of 3 Rs from the black hole will the gravity increase from what Newton’s Law predicts. – then one could eventually fall into the black hole, if you get rid of your ...
What is the net result of the proton-proton chain? a. 2 protons make
... What are the two most important intrinsic properties used to classify stars: a. Mass and age b. Luminosity and surface temperature c. Distance and luminosity d. Distance and surface temperature e. Distance and color Stars that have masses similar to the Sun and sizes similar to the Earth are: a. Mai ...
... What are the two most important intrinsic properties used to classify stars: a. Mass and age b. Luminosity and surface temperature c. Distance and luminosity d. Distance and surface temperature e. Distance and color Stars that have masses similar to the Sun and sizes similar to the Earth are: a. Mai ...
Life Cycle of a Star Notes
... Stars glow because of a nuclear fusion reaction whereby hydrogen fuses together to form heavier elements such as helium and release energy. If enough matter is left behind, this may be so dense, and its gravitational field so strong that nothing can escape from it, not even light or other forms of e ...
... Stars glow because of a nuclear fusion reaction whereby hydrogen fuses together to form heavier elements such as helium and release energy. If enough matter is left behind, this may be so dense, and its gravitational field so strong that nothing can escape from it, not even light or other forms of e ...
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.