Evolution and the Big Bang, ET Life Lec. 6, Jan 18, 2002
... Protons and neutrons are each made of three quarks. By about 3 min. after Big Bang all of the neutrons are bound into 4He nuclei which have two protons (Helium has Z=2) and 2 neutrons. Remaining protons are free to form Hydrogen (Z=1). Thus Universe was about 25% He and 75% H and little heavier elem ...
... Protons and neutrons are each made of three quarks. By about 3 min. after Big Bang all of the neutrons are bound into 4He nuclei which have two protons (Helium has Z=2) and 2 neutrons. Remaining protons are free to form Hydrogen (Z=1). Thus Universe was about 25% He and 75% H and little heavier elem ...
VLA 90 cm Brogan et al. (2006)
... Main Sequence: The normal part of a star’s life when it is burning Hydrogen in its core. Our sun ...
... Main Sequence: The normal part of a star’s life when it is burning Hydrogen in its core. Our sun ...
Physics 127 Descriptive Astronomy Homework #20 Key
... Hubble was able to detect Cepheid variable stars within that “Nebula.” Then by observing their light curves and using the known period- luminosity relation for Cepheids, he obtained and compared the absolute magnitudes of these Cepheids with his observed apparent magnitudes, yielding a distance for ...
... Hubble was able to detect Cepheid variable stars within that “Nebula.” Then by observing their light curves and using the known period- luminosity relation for Cepheids, he obtained and compared the absolute magnitudes of these Cepheids with his observed apparent magnitudes, yielding a distance for ...
final review sheet
... Midterm 1 onward. I suggest using this review sheet as a way to gauging how well you understand the material. I also STRONGLY recommend going over the practice final on page 121 of the course reader and the multiple choice review questions at the back of each chapter of the book (solutions are on bs ...
... Midterm 1 onward. I suggest using this review sheet as a way to gauging how well you understand the material. I also STRONGLY recommend going over the practice final on page 121 of the course reader and the multiple choice review questions at the back of each chapter of the book (solutions are on bs ...
File
... Neutrinos • Neutrino detectors on earth recorded a significant neutrino burst 3 hours before the light rise was detected. – It takes a while for the light to work its way out. Neutrinos fly out unimpeded. ...
... Neutrinos • Neutrino detectors on earth recorded a significant neutrino burst 3 hours before the light rise was detected. – It takes a while for the light to work its way out. Neutrinos fly out unimpeded. ...
Life Cycles of Stars
... High-mass stars live for one million to tens of millions of years while low-mass stars, like our Sun, live for tens of millions to trillions of years. ...
... High-mass stars live for one million to tens of millions of years while low-mass stars, like our Sun, live for tens of millions to trillions of years. ...
Circumstellar interaction of supernovae and gamma-ray bursts
... Blast wave shock : Ejecta expansion speed is much higher than sound speed. Shocked CSM: Interaction of blast wave with CSM . CSM is accelerated, compressed, heated and shocked. ...
... Blast wave shock : Ejecta expansion speed is much higher than sound speed. Shocked CSM: Interaction of blast wave with CSM . CSM is accelerated, compressed, heated and shocked. ...
The Life Cycles of Stars
... supernova. Neutron stars spin rapidly giving off radio waves. If the radio waves are emitted in pulses (due to the star’s spin), these neutron stars are called pulsars. The core of a massive star that has 8 or more times the mass of our Sun remains massive after the supernova. No nuclear fusion is t ...
... supernova. Neutron stars spin rapidly giving off radio waves. If the radio waves are emitted in pulses (due to the star’s spin), these neutron stars are called pulsars. The core of a massive star that has 8 or more times the mass of our Sun remains massive after the supernova. No nuclear fusion is t ...
Death of High Mass Stars
... Death of a High Mass Star • After core has a mass greater than 1.4 M (Chandrasekhar limit) the electron degeneracy is not strong enough. • Electrons are forced to combine with the protons to create neutrons. • Core collapses until pressure from physical force of neutrons bouncing against each other ...
... Death of a High Mass Star • After core has a mass greater than 1.4 M (Chandrasekhar limit) the electron degeneracy is not strong enough. • Electrons are forced to combine with the protons to create neutrons. • Core collapses until pressure from physical force of neutrons bouncing against each other ...
Gone in a flash: supernovae in the survey era
... brighter than a Type Ia supernova). The first of SLSN (Gal-Yam 2012), commonly defined as CFHT, or DECam on the Cerro Tololo Interevent, SCP 06F6, was identified in 2009 and had being brighter than –21 in absolute magnitude American Observatory 4 m Blanco telescope), broad, unexplained spectral abso ...
... brighter than a Type Ia supernova). The first of SLSN (Gal-Yam 2012), commonly defined as CFHT, or DECam on the Cerro Tololo Interevent, SCP 06F6, was identified in 2009 and had being brighter than –21 in absolute magnitude American Observatory 4 m Blanco telescope), broad, unexplained spectral abso ...
April11
... predictable curve – Initial brightness increase followed by a slowly decaying “tail” ...
... predictable curve – Initial brightness increase followed by a slowly decaying “tail” ...
Constants and Equations
... a) AM CVn stars are binary systems with an orbital period of less than 65 minutes. b) AM CVn stars may produce a type II supernova after the white dwarf reaches a critical mass. c) AM CVn stars are sources of gravitational waves. d) AM CVn stars are binary systems where a white dwarf accretes mass f ...
... a) AM CVn stars are binary systems with an orbital period of less than 65 minutes. b) AM CVn stars may produce a type II supernova after the white dwarf reaches a critical mass. c) AM CVn stars are sources of gravitational waves. d) AM CVn stars are binary systems where a white dwarf accretes mass f ...
SES4U Life Cycle of a Star
... Throughout its life, a star oscillates between stable and unstable states Nuclear Fusion. Gas pressure=Gravity Fuel (H and He for small-medium stars; C-Fe in massive stars) runs out Fusion stops and temperature decreases Core contracts Increase in temperature and density due to increased particle co ...
... Throughout its life, a star oscillates between stable and unstable states Nuclear Fusion. Gas pressure=Gravity Fuel (H and He for small-medium stars; C-Fe in massive stars) runs out Fusion stops and temperature decreases Core contracts Increase in temperature and density due to increased particle co ...
sep04 neutrinos - Charles J Horowitz
... with the solar system. Abundances reflect composition of primitive solar nebula at time of formation. Heavy elements made in previous generation stars. Not made in Sun. ...
... with the solar system. Abundances reflect composition of primitive solar nebula at time of formation. Heavy elements made in previous generation stars. Not made in Sun. ...
Time From the Perspective of a Particle Physicist
... • if Mass(core) > 1.4 M(Sun) core collapses in SUPERNOVA (II) • leaves either Neutron Star or Black Hole • Most SN are this type PHYS 162 ...
... • if Mass(core) > 1.4 M(Sun) core collapses in SUPERNOVA (II) • leaves either Neutron Star or Black Hole • Most SN are this type PHYS 162 ...
1 Introduction - High Point University
... all RR Lyrae stars have absolute magnitudes very near MV = 0.5. However, since they are small, faint stars, they cannot be seen at large distances. Figure 2 shows the variation in the apparent magnitude of the RR Lyrae star VX Her. Note that the average apparent magnitude is about 10.5 (where each p ...
... all RR Lyrae stars have absolute magnitudes very near MV = 0.5. However, since they are small, faint stars, they cannot be seen at large distances. Figure 2 shows the variation in the apparent magnitude of the RR Lyrae star VX Her. Note that the average apparent magnitude is about 10.5 (where each p ...
Neutron Stars - Otterbein University
... • A shock wave travels through the star and blows off the outer layers, including the heavy elements – a supernova • A million times brighter than a nova!! • The actual explosion takes less than a second ...
... • A shock wave travels through the star and blows off the outer layers, including the heavy elements – a supernova • A million times brighter than a nova!! • The actual explosion takes less than a second ...
Chapter 27.2
... inward due to gravity, forming a hot, dense white dwarf star. • It shines for billions of years, but eventually becomes cooler and fainter, until energy emmission stops, and it becomes a black dwarf. ...
... inward due to gravity, forming a hot, dense white dwarf star. • It shines for billions of years, but eventually becomes cooler and fainter, until energy emmission stops, and it becomes a black dwarf. ...
Stellar Evolution
... A star with 3x the sun’s mass or more has enough mass so that when it collapses the gravitational field becomes so strong that the escape velocity near it becomes faster than light. Light itself cannot escape…. A Black Hole. The distance from the star called the Event Horizon is where escape velocit ...
... A star with 3x the sun’s mass or more has enough mass so that when it collapses the gravitational field becomes so strong that the escape velocity near it becomes faster than light. Light itself cannot escape…. A Black Hole. The distance from the star called the Event Horizon is where escape velocit ...
Lecture19
... is 3.72 MeV. Given 0.075 MSun of this isotope (this is how much was estimated to have been produced in SN1987A) how much energy does the decay release? ...
... is 3.72 MeV. Given 0.075 MSun of this isotope (this is how much was estimated to have been produced in SN1987A) how much energy does the decay release? ...
Time From the Perspective of a Particle Physicist
... For heavy white dwarves with a companion star • acquire mass, if becomes > 1.4 M(Sun) SUPERNOVA (Ia). p + e n + neutrino • Usually leaves neutron star For high mass stars • fusion continues beyond C,O to Iron • if Mass(core) > 1.4 M(Sun) core collapses in SUPERNOVA (II) • leaves either Neutron Sta ...
... For heavy white dwarves with a companion star • acquire mass, if becomes > 1.4 M(Sun) SUPERNOVA (Ia). p + e n + neutrino • Usually leaves neutron star For high mass stars • fusion continues beyond C,O to Iron • if Mass(core) > 1.4 M(Sun) core collapses in SUPERNOVA (II) • leaves either Neutron Sta ...
White Dwarf Stars
... • These objects act as cosmic clocks and are useful for probing the dynamics of stars. ...
... • These objects act as cosmic clocks and are useful for probing the dynamics of stars. ...
White Dwarf Stars - University of California Observatories
... • These objects act as cosmic clocks and are useful for ...
... • These objects act as cosmic clocks and are useful for ...
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.