How Stars Evolve
... • Leaves behind core of carbon and oxygen surrounded by thin shell of hydrogen – a white dwarf ...
... • Leaves behind core of carbon and oxygen surrounded by thin shell of hydrogen – a white dwarf ...
test - Scioly.org
... 7) A white dwarf, also called a degenerate dwarf, is a stellar remnant composed mostly of neutron-degenerate matter. 8) The density of a White dwarf is 1 × 109 kg/m3 . Therefore the specific gravity of White Dwarf material is 10,000 SG. 9) A blackbody refers to an opaque object that emits ultraviole ...
... 7) A white dwarf, also called a degenerate dwarf, is a stellar remnant composed mostly of neutron-degenerate matter. 8) The density of a White dwarf is 1 × 109 kg/m3 . Therefore the specific gravity of White Dwarf material is 10,000 SG. 9) A blackbody refers to an opaque object that emits ultraviole ...
Stellar Evolution Hertzsprung-Russell Diagram Hertzsprung
... when it stops emitting light end of many sun-like stars ...
... when it stops emitting light end of many sun-like stars ...
V Example: our SUN (G2V)
... Supernovae A supernova occurs when the core of the massive star collapses and a shock wave rips the star apart, usually leaving behind a neutron star. Supernovae can also be produced when enough material is deposited on a white dwarf so that is exceeds the Chandrasekhar limit and collapses to a neut ...
... Supernovae A supernova occurs when the core of the massive star collapses and a shock wave rips the star apart, usually leaving behind a neutron star. Supernovae can also be produced when enough material is deposited on a white dwarf so that is exceeds the Chandrasekhar limit and collapses to a neut ...
Outline2a
... Eventually, the proto-star will fuse hydrogen in its core. This energy will greatly increase the radiation pressure that the photons create on their surroundings. A stellar wind will begin to blow material away. ...
... Eventually, the proto-star will fuse hydrogen in its core. This energy will greatly increase the radiation pressure that the photons create on their surroundings. A stellar wind will begin to blow material away. ...
death_high_mass_2b
... days. This shows that the isotopes are created in the explosion. • It is also interesting that the half-life of ...
... days. This shows that the isotopes are created in the explosion. • It is also interesting that the half-life of ...
Irregular Galaxies
... • Supernovas can light up the sky for many weeks. • The core of the star becomes tremendously hot, fusing iron atoms into new elements. • Huge clouds of dust, gas, and the new elements explode into space. • This forms a new nebula. • Once a star supernovas, the core that remains of it will become ei ...
... • Supernovas can light up the sky for many weeks. • The core of the star becomes tremendously hot, fusing iron atoms into new elements. • Huge clouds of dust, gas, and the new elements explode into space. • This forms a new nebula. • Once a star supernovas, the core that remains of it will become ei ...
powerpoint file
... We are confident that very massive black holes exist at the centers of most galaxies. 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 hole ...
... We are confident that very massive black holes exist at the centers of most galaxies. 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 hole ...
High Mass Stars
... – From H-R diagram its luminosity is 100000 times greater than the Sun’s. – It therefore burns fuel (uses it’s mass) 100000 times faster than the Sun. – It has 25 times the mass of the Sun so its lifetime will be 25/100000 = 0.00025 times than the Sun’s lifetime = 2.5 million years. ...
... – From H-R diagram its luminosity is 100000 times greater than the Sun’s. – It therefore burns fuel (uses it’s mass) 100000 times faster than the Sun. – It has 25 times the mass of the Sun so its lifetime will be 25/100000 = 0.00025 times than the Sun’s lifetime = 2.5 million years. ...
AST101 Lecture 13 The Lives of the Stars
... • Stars generate luminosity through fusion of H into He • The lifetime of a star is proportional to the amount of fuel it has (mass) divided by the rate at which it expends the fuel (luminosity) • The lifetime τ ~ M/L ~ M-2 (because L ~ M3) • τ ranges from 4x106 years for O stars to ~1012 years ...
... • Stars generate luminosity through fusion of H into He • The lifetime of a star is proportional to the amount of fuel it has (mass) divided by the rate at which it expends the fuel (luminosity) • The lifetime τ ~ M/L ~ M-2 (because L ~ M3) • τ ranges from 4x106 years for O stars to ~1012 years ...
AST101_lect_13
... • Stars generate luminosity through fusion of H into He • The lifetime of a star is proportional to the amount of fuel it has (mass) divided by the rate at which it expends the fuel (luminosity) • The lifetime τ ~ M/L ~ M-2 (because L ~ M3) ...
... • Stars generate luminosity through fusion of H into He • The lifetime of a star is proportional to the amount of fuel it has (mass) divided by the rate at which it expends the fuel (luminosity) • The lifetime τ ~ M/L ~ M-2 (because L ~ M3) ...
PHYS 175 (2014) Final Examination Name: ___SOLUTION_____
... d) its frequency is increased and its wavelength is blueshifted because time passes more rapidly in an ...
... d) its frequency is increased and its wavelength is blueshifted because time passes more rapidly in an ...
Supernova Neutrinos
... for astronomers. SNEWS exists to alert astronomers of a nearby supernova. ...
... for astronomers. SNEWS exists to alert astronomers of a nearby supernova. ...
Stellar Evolution Notes
... A protostar is the birth of a star. They are starting out in their life as a star. Eventually, a protostar’s center becomes so hot that a fusion reaction begins. When fusion begins, a star is born ...
... A protostar is the birth of a star. They are starting out in their life as a star. Eventually, a protostar’s center becomes so hot that a fusion reaction begins. When fusion begins, a star is born ...
Stellar Evolution Notes
... A protostar is the birth of a star. They are starting out in their life as a star. Eventually, a protostar’s center becomes so hot that a fusion reaction begins. When fusion begins, a star is born ...
... A protostar is the birth of a star. They are starting out in their life as a star. Eventually, a protostar’s center becomes so hot that a fusion reaction begins. When fusion begins, a star is born ...
![31 — Main-Sequence Stars [Revision : 1.1]](http://s1.studyres.com/store/data/015926256_1-97d746cbe97ccc13b433136b208bf071-300x300.png)
31 — Main-Sequence Stars [Revision : 1.1]
... ∗ So, luminosity Lr grows raidly in core, and F = Lr /4πr2 is large ∗ To transport all energy by radiation, temperature gradient very steep; convection sets in ∗ So, convective core ∗ Convection is very efficient, so ∇ = ∇ad to high degree of accuracy ∗ Convection mixes composition changes due to nu ...
... ∗ So, luminosity Lr grows raidly in core, and F = Lr /4πr2 is large ∗ To transport all energy by radiation, temperature gradient very steep; convection sets in ∗ So, convective core ∗ Convection is very efficient, so ∇ = ∇ad to high degree of accuracy ∗ Convection mixes composition changes due to nu ...
The dying sun/ creation of elements
... • Caught in act of exploding and intensively studied. • Intense neutrino flux detected. During ...
... • Caught in act of exploding and intensively studied. • Intense neutrino flux detected. During ...
Part 1—Stages of Human Life
... 1. Place the pictures in order from youngest to oldest. 2. Glue or tape the images to the paper. Draw in arrows showing the sequence. 3. Estimate the age of the person in the picture. 4. List some evidence of the person’s age. Be specific. 5. Do you have to see the entire life cycle of one person to ...
... 1. Place the pictures in order from youngest to oldest. 2. Glue or tape the images to the paper. Draw in arrows showing the sequence. 3. Estimate the age of the person in the picture. 4. List some evidence of the person’s age. Be specific. 5. Do you have to see the entire life cycle of one person to ...
2017 New Jersey Science Olympiad Union County College
... orbiting each other in a binary star system with the period of the orbit being 50 days and the sum of the semimajor axes being 2 AU. (A) Give the sum of the masses of the white dwarves in kg. (B) Given that the mass of White Dwarf 1 is 1 solar mass and the semimajor axis length of White Dwarf 1 is 1 ...
... orbiting each other in a binary star system with the period of the orbit being 50 days and the sum of the semimajor axes being 2 AU. (A) Give the sum of the masses of the white dwarves in kg. (B) Given that the mass of White Dwarf 1 is 1 solar mass and the semimajor axis length of White Dwarf 1 is 1 ...
Our Community`s Place Among the Stars
... consume their mass too quickly only live a few tens of million of years •very hot stars go through their fuel very quickly ...
... consume their mass too quickly only live a few tens of million of years •very hot stars go through their fuel very quickly ...
How are stars formed
... Stars of roughly sun’s mass ( < 8 solar masses) do not have necessary gravitational pull to create heat and pressure necessary to begin fusing carbon ...
... Stars of roughly sun’s mass ( < 8 solar masses) do not have necessary gravitational pull to create heat and pressure necessary to begin fusing carbon ...
PPT - McMaster Physics and Astronomy
... They therefore continuously evolve as their fuels are used up. H burns to He, He burns to C, etc… Stellar end-states: white dwarfs, neutron stars, or black holes. In all of these cases, significant fraction of stellar mass, ejected into interstellar medium Planets, and biomolecules made out of these ...
... They therefore continuously evolve as their fuels are used up. H burns to He, He burns to C, etc… Stellar end-states: white dwarfs, neutron stars, or black holes. In all of these cases, significant fraction of stellar mass, ejected into interstellar medium Planets, and biomolecules made out of these ...
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.