10. The Lives of the Stars
... larger, redder, and much more luminous — at least for a while. . . ...
... larger, redder, and much more luminous — at least for a while. . . ...
Implies dark halo for self-enrichment
... Low mass stars enriched by only Type II SNe show enhanced ratio of -elements to iron, with value dependent on mass distribution of SNe progenitors – if well-mixed system, see IMF-average Type Ia SNe produce very significant iron, on longer timescales, few x 108 – several 1010yr (WD in binaries) ...
... Low mass stars enriched by only Type II SNe show enhanced ratio of -elements to iron, with value dependent on mass distribution of SNe progenitors – if well-mixed system, see IMF-average Type Ia SNe produce very significant iron, on longer timescales, few x 108 – several 1010yr (WD in binaries) ...
PPT - El Camino College
... • Big picture: carbon and stuff fuses until you get to a core made of … • Iron (Fe on the periodic table, #26, middle section, ...
... • Big picture: carbon and stuff fuses until you get to a core made of … • Iron (Fe on the periodic table, #26, middle section, ...
No Slide Title
... theory they can be seen up to 8000 Mly from Earth. This makes them potentially very interesting as Standard Candles. • Supernovae are divided into various types. Type 1 are thought to be formed by the same kind of event that causes novae. In this case however the White Dwarf collects so much materia ...
... theory they can be seen up to 8000 Mly from Earth. This makes them potentially very interesting as Standard Candles. • Supernovae are divided into various types. Type 1 are thought to be formed by the same kind of event that causes novae. In this case however the White Dwarf collects so much materia ...
Expected Coalescence Rate of NS/NS Binaries for Laser Beam
... index (Rocha-Tinto et al., 2000) enhanced periods of star formation at 1 Gyr, 2-5 Gyr and 79 Gyr probably associated with accretion and merger episodes from which the disk grows and acquires angular ...
... index (Rocha-Tinto et al., 2000) enhanced periods of star formation at 1 Gyr, 2-5 Gyr and 79 Gyr probably associated with accretion and merger episodes from which the disk grows and acquires angular ...
OBAFGKM(LT) extra credit due today. Mid
... Last Time: Stars “Luminosity class” is added to the spectral type, telling you if it’s main-sequence (a “dwarf”, V), giant (III), or super-giant star (I). The sun is a G2 V. Stars occur in smaller “open” and giant “globular” clusters, with hundreds to millions of stars. Stars in clusters born at th ...
... Last Time: Stars “Luminosity class” is added to the spectral type, telling you if it’s main-sequence (a “dwarf”, V), giant (III), or super-giant star (I). The sun is a G2 V. Stars occur in smaller “open” and giant “globular” clusters, with hundreds to millions of stars. Stars in clusters born at th ...
From galaxies to stars
... gets hot enough for the next ignition stage. Instead, the star ejects its outer layers in a series of belches, and this gas expands into space. Lit by the central remnant, which is now a white dwarf, we see this glowing gas as a planetary nebula. ...
... gets hot enough for the next ignition stage. Instead, the star ejects its outer layers in a series of belches, and this gas expands into space. Lit by the central remnant, which is now a white dwarf, we see this glowing gas as a planetary nebula. ...
Atypical thermonuclear supernovae from tidally crushed white dwarfs
... et al. 2007), but could be frequent enough to warrant a search for this new class of optical transient. The transient sky at faint magnitudes is poorly known, but there are major efforts under way that would increase the discovery rate for type Ia supernovae from a few thousands (Aldering et al. 2007 ...
... et al. 2007), but could be frequent enough to warrant a search for this new class of optical transient. The transient sky at faint magnitudes is poorly known, but there are major efforts under way that would increase the discovery rate for type Ia supernovae from a few thousands (Aldering et al. 2007 ...
Study Guide
... Post-Main Sequence Evolution of a High Mass Star • End of the Life of a Massive Star: – Burn H through Si in successive cores – Finally build a massive Iron core ...
... Post-Main Sequence Evolution of a High Mass Star • End of the Life of a Massive Star: – Burn H through Si in successive cores – Finally build a massive Iron core ...
M = 5.5 - The Millstone
... stellar distance (by other means). Absolute magnitude, M, expresses the brightness of a star as it would be if it were placed 10 parsecs away. Since all stars would be placed at the same distance, absolute magnitudes show differences in actual luminosities. It is a measure based on stellar analysis ...
... stellar distance (by other means). Absolute magnitude, M, expresses the brightness of a star as it would be if it were placed 10 parsecs away. Since all stars would be placed at the same distance, absolute magnitudes show differences in actual luminosities. It is a measure based on stellar analysis ...
minnesota
... The calculation at the right (Herant and Woosley, ApJ, 1995) shows a 60 degree wedge of a 15 solar mass supernova modelled using SPH and 20,000 particles. At 9 hours and 36 hours, the growth of the non-linear RT instability is apparent. Red is hydrogen, yellow is helium, green is oxygen, and blue is ...
... The calculation at the right (Herant and Woosley, ApJ, 1995) shows a 60 degree wedge of a 15 solar mass supernova modelled using SPH and 20,000 particles. At 9 hours and 36 hours, the growth of the non-linear RT instability is apparent. Red is hydrogen, yellow is helium, green is oxygen, and blue is ...
... now-extinct radioactive isotopes. It might seem to be an odd way to make a living, studying something that no longer exists, but the payoff in understanding element formation, the formation of the Solar System, and the timing of events during its formation is well worth the effort. Robert Nichols an ...
Type II Supernovae
... An observer in the orbital plane has θ = π/2 and h× = 0. The observed frequency of gravitational waves is ν = Ω/π. The intensity of gravitational waves decreases as 1/r. Consider two 1.4 M⊙ neutron stars in a binary with separation of R⊙ observed from a distance of 1 kpc: P ≃ 7000 s, ν ≃ 2.9 · 10−4 ...
... An observer in the orbital plane has θ = π/2 and h× = 0. The observed frequency of gravitational waves is ν = Ω/π. The intensity of gravitational waves decreases as 1/r. Consider two 1.4 M⊙ neutron stars in a binary with separation of R⊙ observed from a distance of 1 kpc: P ≃ 7000 s, ν ≃ 2.9 · 10−4 ...
11 Solar Masses
... of the nuclear force is communicated throughout its volume by sound waves, but not beyond its edge. Thus the outer edge of the homologous core is where the shock is first born. Typically, MHC = 0.6 – 0.8 solar masses. The larger MHC and the smaller the mass of the iron core, the less dissipation the ...
... of the nuclear force is communicated throughout its volume by sound waves, but not beyond its edge. Thus the outer edge of the homologous core is where the shock is first born. Typically, MHC = 0.6 – 0.8 solar masses. The larger MHC and the smaller the mass of the iron core, the less dissipation the ...
Chapter 17 Star Stuff
... Helium fusion does not begin right away because it requires higher temperatures than hydrogen fusion—larger charge leads to greater repulsion Fusion of two helium nuclei doesn’t work, so helium fusion must combine three He nuclei to make carbon ...
... Helium fusion does not begin right away because it requires higher temperatures than hydrogen fusion—larger charge leads to greater repulsion Fusion of two helium nuclei doesn’t work, so helium fusion must combine three He nuclei to make carbon ...
Chapter 17 Star Stuff How does a star`s mass affect nuclear fusion
... carbon in a shell around the carbon core, and H fuses to He in a shell around the helium layer • This double-shell burning stage never reaches equilibrium—fusion rate periodically spikes upward in a series of thermal pulses • With each spike, convection dredges carbon up from core and transports it ...
... carbon in a shell around the carbon core, and H fuses to He in a shell around the helium layer • This double-shell burning stage never reaches equilibrium—fusion rate periodically spikes upward in a series of thermal pulses • With each spike, convection dredges carbon up from core and transports it ...
TMSP Stellar Evolution & Life
... laboratories with elements heated to gaseous states, we now have a catalog of elemental spectra. •Using this catalog, we now look at stars through a spectroscope and see what they’re made of… ...
... laboratories with elements heated to gaseous states, we now have a catalog of elemental spectra. •Using this catalog, we now look at stars through a spectroscope and see what they’re made of… ...
Test - Scioly.org
... B. It was detected very early C. It was first classified as a Type II supernova D. It had a much higher absolute magnitude than expected E. It had a much lower absolute magnitude than expected 49. Which of the following are true about Tycho’s SNR? A. It was one of eight supernovae visible to the nak ...
... B. It was detected very early C. It was first classified as a Type II supernova D. It had a much higher absolute magnitude than expected E. It had a much lower absolute magnitude than expected 49. Which of the following are true about Tycho’s SNR? A. It was one of eight supernovae visible to the nak ...
Written in the stars THE NOBEL PRIZE IN PHYSICS 2011
... The newest tool in the astronomer’s toolbox is a special kind of star explosion, the type Ia supernova. During a few weeks, a single such supernova can emit as much light as an entire galaxy. This type of supernova is the explosion of an extremely compact old star that is as heavy as the Sun but as ...
... The newest tool in the astronomer’s toolbox is a special kind of star explosion, the type Ia supernova. During a few weeks, a single such supernova can emit as much light as an entire galaxy. This type of supernova is the explosion of an extremely compact old star that is as heavy as the Sun but as ...
What is a white dwarf?
... • Adding mass to a white dwarf increases its gravity, forcing electrons into a smaller space • In order to avoid being in the same state in the same place some of the electrons need to move faster. That increases the temperature, but not the pressure degeneracy pressure doesn't depend on tempe ...
... • Adding mass to a white dwarf increases its gravity, forcing electrons into a smaller space • In order to avoid being in the same state in the same place some of the electrons need to move faster. That increases the temperature, but not the pressure degeneracy pressure doesn't depend on tempe ...
Geol. 655 Isotope Geochemistry
... mass. Nuclear reactions in small stars cease and they simply contract, their exteriors heating up as they do so, to become white dwarfs. The energy released is that produced by previous nuclear reactions and released gravitational potential energy. This is the likely fate of the Sun. White Dwarfs ar ...
... mass. Nuclear reactions in small stars cease and they simply contract, their exteriors heating up as they do so, to become white dwarfs. The energy released is that produced by previous nuclear reactions and released gravitational potential energy. This is the likely fate of the Sun. White Dwarfs ar ...
Mysterious transient objects - NCRA
... Repeated flares in Soft Gamma Ray or hard X-ray band Less energetic then supernovae and GRBs but Galactic In 1/10 of a second as much energy as sun emits in 100,000 years continuously. 1000 times more bright than combining all the stars of Milky Way together. Only handful of SGRs are known ...
... Repeated flares in Soft Gamma Ray or hard X-ray band Less energetic then supernovae and GRBs but Galactic In 1/10 of a second as much energy as sun emits in 100,000 years continuously. 1000 times more bright than combining all the stars of Milky Way together. Only handful of SGRs are known ...
When Stars Go Boom
... they don’t release energy. So, if a star gets to the point where it forms an iron core, it is in trouble. Big trouble. The huge gravitational forces in these massive stars commence to crush the core of the star in less than a second, triggering a massive explosion called a supernova. The explosions ...
... they don’t release energy. So, if a star gets to the point where it forms an iron core, it is in trouble. Big trouble. The huge gravitational forces in these massive stars commence to crush the core of the star in less than a second, triggering a massive explosion called a supernova. The explosions ...
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.