Prep Homework Solutions for HW due 10/04/10
... Sequence before its companion, but then it lost significant mass through mass transfer to the companion, so the more massive star is the less massive star now. Note: a couple of you suggested that the paradox could be resolved by supposing that stars in binaries change each other rate of aging or “l ...
... Sequence before its companion, but then it lost significant mass through mass transfer to the companion, so the more massive star is the less massive star now. Note: a couple of you suggested that the paradox could be resolved by supposing that stars in binaries change each other rate of aging or “l ...
ASTRONOMY: WHAT DO YOU NEED TO KNOW
... What is the CNO cycle and what is formed through this cycle? How massive are stars that follow this cycle? This cycle is found in stars more massive than our Sun. The cores of such stars are hotter than the Sun and use the CNO cycle to produce helium instead of the hydrogen to helium formation of th ...
... What is the CNO cycle and what is formed through this cycle? How massive are stars that follow this cycle? This cycle is found in stars more massive than our Sun. The cores of such stars are hotter than the Sun and use the CNO cycle to produce helium instead of the hydrogen to helium formation of th ...
Assessment 1 - Stars - Teacher Key
... In the list below, you will find the steps in the birth of a star. The steps are not in order. Carefully cut each step out with scissors. Place the strips in the order which they occur in a star’s birth. 1. Friction causes temperature to rise to 10-15,000,000°C. 3 2. Nuclei fuse together. 4 3. Star ...
... In the list below, you will find the steps in the birth of a star. The steps are not in order. Carefully cut each step out with scissors. Place the strips in the order which they occur in a star’s birth. 1. Friction causes temperature to rise to 10-15,000,000°C. 3 2. Nuclei fuse together. 4 3. Star ...
High Mass Stellar Evolution
... High mass stars (> 8 Msolar) have more fuel but they use it up much more quickly than low mass stars (higher luminosity). ...
... High mass stars (> 8 Msolar) have more fuel but they use it up much more quickly than low mass stars (higher luminosity). ...
Stellar Evolution
... neutron stars. The mass of the star is so great that the core of the star simply continues to collapse, compacting matter into a smaller and smaller volume. The small, but extremely dense, object that remains is called a black hole because its gravity is so immense that nothing, not even light, can ...
... neutron stars. The mass of the star is so great that the core of the star simply continues to collapse, compacting matter into a smaller and smaller volume. The small, but extremely dense, object that remains is called a black hole because its gravity is so immense that nothing, not even light, can ...
The Electromagnetic Spectrum: Astronomy 1
... Microwave: The Cosmic Microwave Background (CMB). Shortly after the Big Bang, the Universe cooled enough to allow atoms to form. After this point in time, radiation was able to travel freely through the Universe. Initially, the radiation (known as the CMB) from this epoch had a short wavelength, how ...
... Microwave: The Cosmic Microwave Background (CMB). Shortly after the Big Bang, the Universe cooled enough to allow atoms to form. After this point in time, radiation was able to travel freely through the Universe. Initially, the radiation (known as the CMB) from this epoch had a short wavelength, how ...
Document
... Microwave: The Cosmic Microwave Background (CMB). Shortly after the Big Bang, the Universe cooled enough to allow atoms to form. After this point in time, radiation was able to travel freely through the Universe. Initially, the radiation (known as the CMB) from this epoch had a short wavelength, how ...
... Microwave: The Cosmic Microwave Background (CMB). Shortly after the Big Bang, the Universe cooled enough to allow atoms to form. After this point in time, radiation was able to travel freely through the Universe. Initially, the radiation (known as the CMB) from this epoch had a short wavelength, how ...
Slide 1
... The Lives of Stars Gestation, Birth, and Youth: 1. The womb: Stars are born in dense molecular clouds. --The interstellar medium must be dense enough so H atoms can collide and form H2 molecules. This also is facilitated on dust--for other molecules as well. It increases gravitation enough for stars ...
... The Lives of Stars Gestation, Birth, and Youth: 1. The womb: Stars are born in dense molecular clouds. --The interstellar medium must be dense enough so H atoms can collide and form H2 molecules. This also is facilitated on dust--for other molecules as well. It increases gravitation enough for stars ...
Russell County Schools Non-Traditional Instructional Expectations
... process stops here, and we have a neutron star. But if the original star was more massive than a few solar masses, even the strong nuclear forces cannot resist the gravitational orunch. The neutrons are forced into one another to form heavier hadrons and these in turn coalesce to form heavier entiti ...
... process stops here, and we have a neutron star. But if the original star was more massive than a few solar masses, even the strong nuclear forces cannot resist the gravitational orunch. The neutrons are forced into one another to form heavier hadrons and these in turn coalesce to form heavier entiti ...
Time From the Perspective of a Particle Physicist
... decreasing RADIUS increases VELOCITY Angular momentum is conserved: spinning chair ice skater formation of neutron star in collapse of larger spinning star ...
... decreasing RADIUS increases VELOCITY Angular momentum is conserved: spinning chair ice skater formation of neutron star in collapse of larger spinning star ...
Chapter 10 The Bizarre Stellar Graveyard
... is so small that the escape velocity exceeds the speed of light. ...
... is so small that the escape velocity exceeds the speed of light. ...
Reminder: Assignments are due back to teachers within 2 school days.
... process stops here, and we have a neutron star. But if the original star was more massive than a few solar masses, even the strong nuclear forces cannot resist the gravitational orunch. The neutrons are forced into one another to form heavier hadrons and these in turn coalesce to form heavier entiti ...
... process stops here, and we have a neutron star. But if the original star was more massive than a few solar masses, even the strong nuclear forces cannot resist the gravitational orunch. The neutrons are forced into one another to form heavier hadrons and these in turn coalesce to form heavier entiti ...
Stars
... neutron star will rotate, as did the original star, but much faster (think about a twirling ice skater). Charged particles trapped by the magnetic field will radiate energy at radio wavelengths, but most of this radiation comes out along the poles of the pulsar. The radio emissions are like a search ...
... neutron star will rotate, as did the original star, but much faster (think about a twirling ice skater). Charged particles trapped by the magnetic field will radiate energy at radio wavelengths, but most of this radiation comes out along the poles of the pulsar. The radio emissions are like a search ...
PowerPoint Presentation - Super Massive Black Holes
... taken by the Hubble Space Telescope. Sirius B, which is a white dwarf, can be seen as a faint pinprick of light to the lower left of the much brighter Sirius A. Located in Canis Major, Sirius is the brightest star in the Earth’s night sky. The distance between A and B varies from 8 to 31 AU. ...
... taken by the Hubble Space Telescope. Sirius B, which is a white dwarf, can be seen as a faint pinprick of light to the lower left of the much brighter Sirius A. Located in Canis Major, Sirius is the brightest star in the Earth’s night sky. The distance between A and B varies from 8 to 31 AU. ...
Part B
... 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 stars. ...
... 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 stars. ...
Lecture 22 - Seattle Central
... The iron core gets crushed so that it’s no longer iron, the electrons and protons combine into neutrons, the volume of the core reduces by a factor of 1018 Outer core falls in at about 25% of the speed of light, the core temp rises to ...
... The iron core gets crushed so that it’s no longer iron, the electrons and protons combine into neutrons, the volume of the core reduces by a factor of 1018 Outer core falls in at about 25% of the speed of light, the core temp rises to ...
The Stellar Graveyard
... The important concept here is in the top right of this diagram which shoes this cone of emitted radiation emerging from the magnetic polar axis. This radiation can be in the form of radio, optical or x-rays and usually all three sources can come from a single pulsar. The Crab nebula, the core remna ...
... The important concept here is in the top right of this diagram which shoes this cone of emitted radiation emerging from the magnetic polar axis. This radiation can be in the form of radio, optical or x-rays and usually all three sources can come from a single pulsar. The Crab nebula, the core remna ...
White Dwarfs and Neutron Stars
... • Neutron stars can form powerful jets of matter and energy • Previously only thought possible with black holes • Binary system with neutron star gaining matter from white dwarf companion’s atmosphere in an accretion disk • Neutron star is tiny compared to white dwarf but is very dense and about 14 ...
... • Neutron stars can form powerful jets of matter and energy • Previously only thought possible with black holes • Binary system with neutron star gaining matter from white dwarf companion’s atmosphere in an accretion disk • Neutron star is tiny compared to white dwarf but is very dense and about 14 ...
Test#3
... a) they emit no light b) they are transparent and let us see deeper, darker layers c) they are cooler than their surroundings d) they are shadows 18. New stars are formed from a) the collision of one or more stars b) the gas in the interstellar medium c) coalescence of planets d) cosmic rays trapped ...
... a) they emit no light b) they are transparent and let us see deeper, darker layers c) they are cooler than their surroundings d) they are shadows 18. New stars are formed from a) the collision of one or more stars b) the gas in the interstellar medium c) coalescence of planets d) cosmic rays trapped ...
Section 25.2 Stellar Evolution
... collapsed to a very small size, believed to be near its final stage of evolution. The sun begins as a nebula, spends much of its life as a main-sequence star, and then becomes a red giant, a planetary nebula, a white dwarf, and, finally, a black dwarf. ...
... collapsed to a very small size, believed to be near its final stage of evolution. The sun begins as a nebula, spends much of its life as a main-sequence star, and then becomes a red giant, a planetary nebula, a white dwarf, and, finally, a black dwarf. ...
Astronomy 114 Problem Set # 6 Due: 11 Apr 2007 SOLUTIONS 1
... 1 Why is the temperature of a star’s core so important in determining which nuclear reactions can occur there? Fusion reactions occur when the strong force, the force that binds the neutrons and protons, binds two nuclei in two initially separate atoms. The strong force acts at very short distances. ...
... 1 Why is the temperature of a star’s core so important in determining which nuclear reactions can occur there? Fusion reactions occur when the strong force, the force that binds the neutrons and protons, binds two nuclei in two initially separate atoms. The strong force acts at very short distances. ...
Stars and Deep Time
... Star Matter! • The atoms that now form your body’s molecules came from substances here on Earth that were part of the nebula which formed our solar system 4.5 billion years ago! • These have been in many things before becoming part of you. • You are part of a larger process than you ever imagined! ...
... Star Matter! • The atoms that now form your body’s molecules came from substances here on Earth that were part of the nebula which formed our solar system 4.5 billion years ago! • These have been in many things before becoming part of you. • You are part of a larger process than you ever imagined! ...
PHYS 390 Lecture 29 - White dwarfs and neutron stars 29
... of the binary pair has a mass now quoted at 1.05±0.03 solar masses, and a surface temperature (determined half a century later) of a very hot 27,000 K in spite of a luminosity just 0.03 that of our Sun. These observations can be taken together to paint a picture of an altogether different type of st ...
... of the binary pair has a mass now quoted at 1.05±0.03 solar masses, and a surface temperature (determined half a century later) of a very hot 27,000 K in spite of a luminosity just 0.03 that of our Sun. These observations can be taken together to paint a picture of an altogether different type of st ...
Problem Set 04
... A2. Stars are stabilized by a balance between an inward gravitational force and outward pressure due to the intense heat generated by nuclear fusion reactions taking place in the star core. As stars age they consume their fuel and the fusion reactions slow down. This can lead to a gravitational col ...
... A2. Stars are stabilized by a balance between an inward gravitational force and outward pressure due to the intense heat generated by nuclear fusion reactions taking place in the star core. As stars age they consume their fuel and the fusion reactions slow down. This can lead to a gravitational col ...
Sources of Gravitational Waves Peter Shawhan
... Long-term radio observations of the Hulse-Taylor binary pulsar B1913+16 have yielded neutron star masses (1.44 and 1.39 M) and orbital parameters System shows very gradual orbital decay – just as general relativity predicts! Very strong indirect evidence for gravitational radiation Weisberg, Nice ...
... Long-term radio observations of the Hulse-Taylor binary pulsar B1913+16 have yielded neutron star masses (1.44 and 1.39 M) and orbital parameters System shows very gradual orbital decay – just as general relativity predicts! Very strong indirect evidence for gravitational radiation Weisberg, Nice ...
Pulsar
A pulsar (short for pulsating radio star) is a highly magnetized, rotating neutron star that emits a beam of electromagnetic radiation. This radiation can only be observed when the beam of emission is pointing toward Earth, much the way a lighthouse can only be seen when the light is pointed in the direction of an observer, and is responsible for the pulsed appearance of emission. Neutron stars are very dense, and have short, regular rotational periods. This produces a very precise interval between pulses that range roughly from milliseconds to seconds for an individual pulsar. Pulsars are believed to be one of the candidates of high and ultra-high energy astroparticles (see also Centrifugal mechanism of acceleration).The precise periods of pulsars make them useful tools. Observations of a pulsar in a binary neutron star system were used to indirectly confirm the existence of gravitational radiation. The first extrasolar planets were discovered around a pulsar, PSR B1257+12. Certain types of pulsars rival atomic clocks in their accuracy in keeping time.