22_SN1987a
... • The core collapses until the neutrons touch: The collapse stops because of neutron degeneracy pressure • A shock wave rebounds through the outer layers of the star: some of the neutrons fly out through the ejecta and make heavy elements by 56Fe + Nn 56+NX • The core continues to collapse: it eit ...
... • The core collapses until the neutrons touch: The collapse stops because of neutron degeneracy pressure • A shock wave rebounds through the outer layers of the star: some of the neutrons fly out through the ejecta and make heavy elements by 56Fe + Nn 56+NX • The core continues to collapse: it eit ...
ppt
... Because we should. The physics of galaxy formation are complex but observations suggest they must obey simple relations. Still, we do not have a good understanding and cannot work from first principles, so models must be observationally based. Fast method to compute the evolution of the galaxy popul ...
... Because we should. The physics of galaxy formation are complex but observations suggest they must obey simple relations. Still, we do not have a good understanding and cannot work from first principles, so models must be observationally based. Fast method to compute the evolution of the galaxy popul ...
Birth - Wayne State University Physics and Astronomy
... Each second in the Sun, about 600 million tons of hydrogen undergo fusion into helium, with about 4 million tons turning to energy in the process This rate of hydrogen use means that eventually the Sun (and all other stars) will run out of central fuel ...
... Each second in the Sun, about 600 million tons of hydrogen undergo fusion into helium, with about 4 million tons turning to energy in the process This rate of hydrogen use means that eventually the Sun (and all other stars) will run out of central fuel ...
Comet Pan-Starrs 12 March 2013
... High Mass Stars • Spectral types O and B • Masses up to ~ 120 M • Luminosities up to ~106 L • Radii up to ~100 R • What sets the upper mass limit? Radiation Pressure (L) exceeds gravity (M/R2) for massive stars Because L ~ M3, g ~ 1/M ...
... High Mass Stars • Spectral types O and B • Masses up to ~ 120 M • Luminosities up to ~106 L • Radii up to ~100 R • What sets the upper mass limit? Radiation Pressure (L) exceeds gravity (M/R2) for massive stars Because L ~ M3, g ~ 1/M ...
Astronomy Unit Test – Chapter 21
... 23. What category of star is Sirius B? 24. Which giant is the brightest? 25. Predict what will happen when the sun runs out of fuel. 26. What is used to classify stars? 27. At which phase of the moon could a solar eclipse occur? 28. A star is twice as massive as the sun. How will its lifespan compa ...
... 23. What category of star is Sirius B? 24. Which giant is the brightest? 25. Predict what will happen when the sun runs out of fuel. 26. What is used to classify stars? 27. At which phase of the moon could a solar eclipse occur? 28. A star is twice as massive as the sun. How will its lifespan compa ...
Formation of the Solar System
... it gets bigger, it gets hotter and denser. 6. When it becomes big enough, it ignites (nuclear fusion). ...
... it gets bigger, it gets hotter and denser. 6. When it becomes big enough, it ignites (nuclear fusion). ...
Astronomy 15 - Problem Set Number 7
... density, no matter what pressure you subject it to. This is completely unphysical, but helps illustrate the point, which is that even if this were the case, black holes would be inevitable if Einstein’s theory of gravity is correct. Let’s take the density of a neutron star to be 1014 gm cm−3 and com ...
... density, no matter what pressure you subject it to. This is completely unphysical, but helps illustrate the point, which is that even if this were the case, black holes would be inevitable if Einstein’s theory of gravity is correct. Let’s take the density of a neutron star to be 1014 gm cm−3 and com ...
The Family of Stars
... Binary Stars More than 50 % of all stars in our Milky Way are not single stars, but belong to binaries: Pairs or multiple systems of stars which orbit their common center of mass. If we can measure and understand their orbital motion, we can estimate the stellar ...
... Binary Stars More than 50 % of all stars in our Milky Way are not single stars, but belong to binaries: Pairs or multiple systems of stars which orbit their common center of mass. If we can measure and understand their orbital motion, we can estimate the stellar ...
PowerPoint Presentation - Super Massive Black Holes
... Later, it was found these sources could not be stars in our galaxy, but must be very far away --- as far as any of the distant galaxies seen. We now think these objects are the very bright centers of some distant galaxies, where some sort of energetic action is occurring. ...
... Later, it was found these sources could not be stars in our galaxy, but must be very far away --- as far as any of the distant galaxies seen. We now think these objects are the very bright centers of some distant galaxies, where some sort of energetic action is occurring. ...
star
... Life Cycle of a Star (cont.) • When a star’s hydrogen supply is nearly gone, the star leaves the main sequence and begins the next stage of its life cycle. • All stars form in the same way, but stars die in different ways, depending on their masses. • Massive stars eventually become red ...
... Life Cycle of a Star (cont.) • When a star’s hydrogen supply is nearly gone, the star leaves the main sequence and begins the next stage of its life cycle. • All stars form in the same way, but stars die in different ways, depending on their masses. • Massive stars eventually become red ...
Astronomy Assignment #1
... through the core hydrogen faster; thus shortening the high mass star’s lifetime. Low-mass stars last a long time in the main sequence stage because their lower central pressures, temperatures and densities establish a lower fusion rate in their cores. The lower fusion rates (i.e. luminosities) burn ...
... through the core hydrogen faster; thus shortening the high mass star’s lifetime. Low-mass stars last a long time in the main sequence stage because their lower central pressures, temperatures and densities establish a lower fusion rate in their cores. The lower fusion rates (i.e. luminosities) burn ...
Stars - Red, Blue, Old, New pt.4
... radio waves 33 times a second. • Pulsations occur at all wavelengths--optical, X-ray, etc. • What could it be? ...
... radio waves 33 times a second. • Pulsations occur at all wavelengths--optical, X-ray, etc. • What could it be? ...
Sources of Gravitational Waves Peter Shawhan
... 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 & Taylor, ApJ 722, 1030 (201 ...
... 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 & Taylor, ApJ 722, 1030 (201 ...
Death of sun
... Low mass red dwarf stars cannot achieve any advanced fusion because they cannot get hot enough (Temp < 100 million K) to begin the next reaction (helium to carbon) Hydrogen => Helium fusion ends at core Star shrinks to form a white dwarf ...
... Low mass red dwarf stars cannot achieve any advanced fusion because they cannot get hot enough (Temp < 100 million K) to begin the next reaction (helium to carbon) Hydrogen => Helium fusion ends at core Star shrinks to form a white dwarf ...
Vital Chapter 7 Information
... atom because we have ___________ energy in moving its electron. If that electron falls back to the lower energy level, the energy is ________________. 10. What are the two ways that atoms can become excited? ...
... atom because we have ___________ energy in moving its electron. If that electron falls back to the lower energy level, the energy is ________________. 10. What are the two ways that atoms can become excited? ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.