Frantic Finish - Max-Planck
... THE ASTRONOMERS GUESSING It could then also be possible to solve a mystery that has increasingly moved into the research spotlight in recent years: ultrabright supernovae, or superluminous supernovae, as astronomers call them. The scientists observed the first example of this type in 2010. Although ...
... THE ASTRONOMERS GUESSING It could then also be possible to solve a mystery that has increasingly moved into the research spotlight in recent years: ultrabright supernovae, or superluminous supernovae, as astronomers call them. The scientists observed the first example of this type in 2010. Although ...
lecture 27 nuclar fusion in stars
... A star must have at least 10% of the sun’s mass in order for fusion to start. If the mass is much more than 100 times the sun’s mass, it will blow apart very quickly. In between, a star’s life cycle is determined primarily by its mass. ¤ Stars ...
... A star must have at least 10% of the sun’s mass in order for fusion to start. If the mass is much more than 100 times the sun’s mass, it will blow apart very quickly. In between, a star’s life cycle is determined primarily by its mass. ¤ Stars ...
stellar remenants
... The End of a High-Mass Star A high-mass star can continue to fuse elements in its core right up to iron (after which the fusion reaction is energetically unfavored). As heavier elements are fused, the reactions go faster and the stage is ...
... The End of a High-Mass Star A high-mass star can continue to fuse elements in its core right up to iron (after which the fusion reaction is energetically unfavored). As heavier elements are fused, the reactions go faster and the stage is ...
Lars Bildsten - nnpss
... age of an Open Cluster like Pleiades from the absence of even brighter stars ==> 120 Myr ...
... age of an Open Cluster like Pleiades from the absence of even brighter stars ==> 120 Myr ...
PPT
... White Dwarfs are supported by electron degeneracy pressure • in a low-mass star, Fusion stops after He -->C and O • Just cools off and fizzles out ...
... White Dwarfs are supported by electron degeneracy pressure • in a low-mass star, Fusion stops after He -->C and O • Just cools off and fizzles out ...
Universe CBA Review - cms16-17
... 33.) What type of EMS wave has the longest wavelength? _____________________ 34.) Does infrared or x-ray waves have a longer wavelength? __________________ 35.) What type of wave has the highest frequency in the EMS? __________________ 36.) Draw and label the visible light spectrum ...
... 33.) What type of EMS wave has the longest wavelength? _____________________ 34.) Does infrared or x-ray waves have a longer wavelength? __________________ 35.) What type of wave has the highest frequency in the EMS? __________________ 36.) Draw and label the visible light spectrum ...
dtu7ech13 - Fort Thomas Independent Schools
... Will the Sun someday cease to exist? If so, how? The Sun will shed matter as a planetary nebula in about 6 billion years and then cease nuclear fusion. Its remnant white dwarf will dim over the succeeding billions of years. What is a nova? A nova is a relatively gentle explosion of hydrogen gas on t ...
... Will the Sun someday cease to exist? If so, how? The Sun will shed matter as a planetary nebula in about 6 billion years and then cease nuclear fusion. Its remnant white dwarf will dim over the succeeding billions of years. What is a nova? A nova is a relatively gentle explosion of hydrogen gas on t ...
Integrative Studies 410 Our Place in the Universe
... • 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 20 Review of Stars` Lifetime Review
... temperatures high enough for the oxygen to combine with the helium and ...
... temperatures high enough for the oxygen to combine with the helium and ...
White dwarfs that crossed the Chandrasekhar limit
... higher the mass, greater the luminosity1. Since the mass of the progenitors of any SNe Ia is 1.44 M , the luminosity peak and spectra of all type Ia supernovae must be identical (Figure 3), but for the distance they are located from us. Therefore, cosmologists use these SNe Ia as standard candles t ...
... higher the mass, greater the luminosity1. Since the mass of the progenitors of any SNe Ia is 1.44 M , the luminosity peak and spectra of all type Ia supernovae must be identical (Figure 3), but for the distance they are located from us. Therefore, cosmologists use these SNe Ia as standard candles t ...
Observation
... GRB971214 Host galaxy GRB980425 SN association(SN1998bw) (z=0.0085, the “closet”) GRB990123 most energetic ( Eiso~3 X 1054erg ) ...
... GRB971214 Host galaxy GRB980425 SN association(SN1998bw) (z=0.0085, the “closet”) GRB990123 most energetic ( Eiso~3 X 1054erg ) ...
The Hidden Lives of Galaxies NSTA 2001
... Giants and Supergiants •These lie in the upper right of the HR diagram, meaning that they are cool but luminous (bright). •Their luminosity is high because they are very large, and so have a big surface area to radiate from. Typically they may have a radius one hundred times that of the Sun. ...
... Giants and Supergiants •These lie in the upper right of the HR diagram, meaning that they are cool but luminous (bright). •Their luminosity is high because they are very large, and so have a big surface area to radiate from. Typically they may have a radius one hundred times that of the Sun. ...
Astronomy Homework - Life
... 5. As the helium core contracts, temperatures and pressures (increase/decrease). 6. Stars leave the main sequence when (they fuse hydrogen in their cores/they run out of hydrogen to fuse in their cores). 7. Hydrogen begins to fuse in a (shell/core) around the contracting helium core. 8. As the core ...
... 5. As the helium core contracts, temperatures and pressures (increase/decrease). 6. Stars leave the main sequence when (they fuse hydrogen in their cores/they run out of hydrogen to fuse in their cores). 7. Hydrogen begins to fuse in a (shell/core) around the contracting helium core. 8. As the core ...
Chapter 14
... High Mass Stars – Less than 100 M on Main Sequence – Become Neutron Stars (1.4M < M < 3M) » Neutron Degeneracy Pressure ...
... High Mass Stars – Less than 100 M on Main Sequence – Become Neutron Stars (1.4M < M < 3M) » Neutron Degeneracy Pressure ...
Yes, we are all star dust. Even Gary!
... Carbon … As carbon life-forms, we are indeed star dust! • Massive Stellar Nuc. (fusion in massive stars) = Oxygen to Iron • Supernovae (exploding massive stars) = all other naturally occurring elements heavier than Iron (ie the metals and rare earths) ...
... Carbon … As carbon life-forms, we are indeed star dust! • Massive Stellar Nuc. (fusion in massive stars) = Oxygen to Iron • Supernovae (exploding massive stars) = all other naturally occurring elements heavier than Iron (ie the metals and rare earths) ...
Ginger Dublin 6th Grade Science
... Starlight Brightness • Apparent Magnitude: How bright a star appears to be from earth when viewed with the unaided eye. Distance can cause a dimmer star to appear to be brighter than a brighter star that is farther away. • Absolute Magnitude: The amount of light (brightness) a star actually has. Th ...
... Starlight Brightness • Apparent Magnitude: How bright a star appears to be from earth when viewed with the unaided eye. Distance can cause a dimmer star to appear to be brighter than a brighter star that is farther away. • Absolute Magnitude: The amount of light (brightness) a star actually has. Th ...
Stellar Deaths - Mid
... Higher mass stars burn out faster and fuse heavier elements. Example: 20 MSun star lives "only" ~10 million years. Heaviest element made in core of any star is iron. ...
... Higher mass stars burn out faster and fuse heavier elements. Example: 20 MSun star lives "only" ~10 million years. Heaviest element made in core of any star is iron. ...
Supernova and Supernova Remnants lec 1-2
... Type I SN and Cosmology • how old is the universe, how fast is it expanding, how much material and of what type is in it, what is its fate? • Need to determine the relationship between distance and redshift – Redshift (‘z’) is the measure of Doppler shift by the expansion of the universe- (1+z)~v/c ...
... Type I SN and Cosmology • how old is the universe, how fast is it expanding, how much material and of what type is in it, what is its fate? • Need to determine the relationship between distance and redshift – Redshift (‘z’) is the measure of Doppler shift by the expansion of the universe- (1+z)~v/c ...
Explosion and remnants of massive stars
... also present. SNe II occur in the spiral arms of galaxies where star formation takes place, and therefore correspond to the explosion of massive stars with short lifetimes. They form the main class of explosions associated with the core collapse of massive stars that have hydrogen-rich envelopes (re ...
... also present. SNe II occur in the spiral arms of galaxies where star formation takes place, and therefore correspond to the explosion of massive stars with short lifetimes. They form the main class of explosions associated with the core collapse of massive stars that have hydrogen-rich envelopes (re ...
NASA`s Chandra Sees Brightest Supernova Ever
... With the observed Hα luminosity and densities, it is difficult to avoid a nebular mass below 2 M⊙, and it could plausibly be as high as 20–30 M⊙. The nebular shells around LBVs with L > 106 L⊙, which descend from stars have initial masses of 80–150 M⊙. Interestingly, such large masses are consiste ...
... With the observed Hα luminosity and densities, it is difficult to avoid a nebular mass below 2 M⊙, and it could plausibly be as high as 20–30 M⊙. The nebular shells around LBVs with L > 106 L⊙, which descend from stars have initial masses of 80–150 M⊙. Interestingly, such large masses are consiste ...
Oct5
... just massive stars evolve faster and are much brighter A star with 20 solar masses spends 8 million years on the Main sequence, and 1 million years as a red giant, before blowing up as a supernova ...
... just massive stars evolve faster and are much brighter A star with 20 solar masses spends 8 million years on the Main sequence, and 1 million years as a red giant, before blowing up as a supernova ...
High Mass Stellar Evolution
... the neutrons is sufficient to stop the collapse of the stellar core neutron degeneracy pressure. ...
... the neutrons is sufficient to stop the collapse of the stellar core neutron degeneracy pressure. ...
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.