S1E4 Extreme Stars
... • The resulting outward pressure which keeps the electrons apart is called electron degeneracy pressure – this is what balances the weight. • Only if more energy drives the electrons into higher energy states, can the density increase. • Adding mass can drive electrons to higher energies so star shr ...
... • The resulting outward pressure which keeps the electrons apart is called electron degeneracy pressure – this is what balances the weight. • Only if more energy drives the electrons into higher energy states, can the density increase. • Adding mass can drive electrons to higher energies so star shr ...
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... star in a binary system loses its hydrogen-rich outer layers to its companion star. *The remains of the massive star could develop an ...
... star in a binary system loses its hydrogen-rich outer layers to its companion star. *The remains of the massive star could develop an ...
Chapter 18 Study Guide
... 10. According to the Hertzsprung-Russell diagram, what relationship exist between the brightness and temperature of a main sequence star? The Hertzsprung- Russell diagram shows that main sequence stars increase in brightness as they increase in temperature. 11. When is a star born? A star is born wh ...
... 10. According to the Hertzsprung-Russell diagram, what relationship exist between the brightness and temperature of a main sequence star? The Hertzsprung- Russell diagram shows that main sequence stars increase in brightness as they increase in temperature. 11. When is a star born? A star is born wh ...
Stars and Deep Time
... 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! ...
... 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! ...
Life Cycles of Stars
... form a protostar • Depending on the size of the star that forms, a different fate is met • Low and medium mass stars burn out to become white dwarfs • High mass stars burn out in an amazing explosion called a supernova, which gives birth to a new nebula ...
... form a protostar • Depending on the size of the star that forms, a different fate is met • Low and medium mass stars burn out to become white dwarfs • High mass stars burn out in an amazing explosion called a supernova, which gives birth to a new nebula ...
Astronomy 12: Introduction to Astronomy
... I. MULTIPLE CHOICE: Please fill in the letter corresponding to the most appropriate answer 1.How does the H-R diagram help astronomers identify stars? a. It plots a star’s mass and core temperature, which allows astronomers determine the colour and region of where star is formed. b. It plots a star’ ...
... I. MULTIPLE CHOICE: Please fill in the letter corresponding to the most appropriate answer 1.How does the H-R diagram help astronomers identify stars? a. It plots a star’s mass and core temperature, which allows astronomers determine the colour and region of where star is formed. b. It plots a star’ ...
Lecture 2+3 - University of Texas Astronomy Home Page
... C, N and O are produced by advanced fusion in core and layers of high-mass (M> 8 solar mass) star. (Low mass stars may produce some C, but no significant N O). When the high mass star dies - its core becomes a neutron star or black hole, - its central and outer layers of gas containing H, He, C, and ...
... C, N and O are produced by advanced fusion in core and layers of high-mass (M> 8 solar mass) star. (Low mass stars may produce some C, but no significant N O). When the high mass star dies - its core becomes a neutron star or black hole, - its central and outer layers of gas containing H, He, C, and ...
Stars Notes
... • Outer layers continue to expand and form a planetary nebula • Remaining core is now a white dwarf which is dense and slowly cools and no longer produces energy ...
... • Outer layers continue to expand and form a planetary nebula • Remaining core is now a white dwarf which is dense and slowly cools and no longer produces energy ...
02-Voyage to the Planets
... solar wind, leaving only the solid chunks behind. As they continued to circulate around the sun, they joined together forming larger chunks. This caused a strong gravity around them and pulled all the matter in space around them, forming the Terrestrial Planets (Mercury, Venus, Earth and Mars) ...
... solar wind, leaving only the solid chunks behind. As they continued to circulate around the sun, they joined together forming larger chunks. This caused a strong gravity around them and pulled all the matter in space around them, forming the Terrestrial Planets (Mercury, Venus, Earth and Mars) ...
IOSR Journal of Applied Physics (IOSR-JAP) ISSN: 2278-4861.
... began as a nebula, an area in the Milky Way Galaxy that was a swirling concentration of cold gas and dust. Due to some perturbation, possibly from the nearby supernova this cloud of gas and dust began to condense (fig. 1), or pull together under the force of its own gravity. Condensation was slow at ...
... began as a nebula, an area in the Milky Way Galaxy that was a swirling concentration of cold gas and dust. Due to some perturbation, possibly from the nearby supernova this cloud of gas and dust began to condense (fig. 1), or pull together under the force of its own gravity. Condensation was slow at ...
Stars and Galaxies
... like our own Milky Way, is thought to have a supermassive black hole at its center. The black hole at the center of the Milky Way is sort of like the Sun at the center of our solar system - the galaxy orbits the black holes like the planets in solar systems orbit the stars. ...
... like our own Milky Way, is thought to have a supermassive black hole at its center. The black hole at the center of the Milky Way is sort of like the Sun at the center of our solar system - the galaxy orbits the black holes like the planets in solar systems orbit the stars. ...
Word doc - UC-HiPACC - University of California, Santa Cruz
... supermassive stars could explode without leaving any black hole or other stellar remnant behind. Chen had been fascinated by supermassive black holes since grad school at the University of Minnesota. Every big galaxy has one of these voracious monsters at its center: a black hole millions or even bi ...
... supermassive stars could explode without leaving any black hole or other stellar remnant behind. Chen had been fascinated by supermassive black holes since grad school at the University of Minnesota. Every big galaxy has one of these voracious monsters at its center: a black hole millions or even bi ...
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... phase, it would eventually heat up and fuse the carbon and oxygen. • But for stars with masses less than 4 times solar a property called electron degeneracy kicks in. • The white dwarf acts like a giant atom with electrons in unique energy states. – This keeps the nuclei separated and the ...
... phase, it would eventually heat up and fuse the carbon and oxygen. • But for stars with masses less than 4 times solar a property called electron degeneracy kicks in. • The white dwarf acts like a giant atom with electrons in unique energy states. – This keeps the nuclei separated and the ...
supernova remnants
... Chandra 1999 Chandra 2000 • We will distinguish between – SN explosions (the actual events and the next few years) and – Remnants - what happens over the next few thousand years. SN 1987A observed in 1999, 2000 SNRs enrich the ISM by dispersing material produced both during the star’s life and at th ...
... Chandra 1999 Chandra 2000 • We will distinguish between – SN explosions (the actual events and the next few years) and – Remnants - what happens over the next few thousand years. SN 1987A observed in 1999, 2000 SNRs enrich the ISM by dispersing material produced both during the star’s life and at th ...
The Life of Stars
... Eventually, protostars give off enough light to be officially called stars Don’t forget – a star is just a big ball of gas! Our sun is just a big ball of gas ...
... Eventually, protostars give off enough light to be officially called stars Don’t forget – a star is just a big ball of gas! Our sun is just a big ball of gas ...
Chapter 20: Stellar Evolution: The Death of Stars PowerPoint
... • Appearance – Extremely bright light where a dim star was located – Supernova remnant • Wide variety of shapes & sizes ...
... • Appearance – Extremely bright light where a dim star was located – Supernova remnant • Wide variety of shapes & sizes ...
PHYS3380_111115_bw - The University of Texas at Dallas
... objects to novae (meaning new stars). • So-called by Fritz Zwicky, after Edwin Hubble estimated distance to Andromeda galaxy (through Cepheids) • Hence the luminosity of the “nova” discovered in 1885 in Andromeda was determined • Supernovae outbursts last for short periods: typically months to a few ...
... objects to novae (meaning new stars). • So-called by Fritz Zwicky, after Edwin Hubble estimated distance to Andromeda galaxy (through Cepheids) • Hence the luminosity of the “nova” discovered in 1885 in Andromeda was determined • Supernovae outbursts last for short periods: typically months to a few ...
6. Star Colors and the Hertzsprung
... Type Ia supernova rivals that of a large galaxy - 1043 erg s-1, or several billion solar luminosities. ...
... Type Ia supernova rivals that of a large galaxy - 1043 erg s-1, or several billion solar luminosities. ...
radio_poster
... this variation and propose scaling relations between synchrotron luminosity and gas density. These models enable us to roughly age date and classify radio spectra of star-forming galaxies into active (e.g., SBS0335–052)/passive (e.g., I Zw 18) classes. ...
... this variation and propose scaling relations between synchrotron luminosity and gas density. These models enable us to roughly age date and classify radio spectra of star-forming galaxies into active (e.g., SBS0335–052)/passive (e.g., I Zw 18) classes. ...
Section 25.2 Stellar Evolution
... Death of Low-Mass Stars Stars less than one-half the mass of the sun never evolve to the red giant stage but remain in the stable main-sequence stage until they consume all their hydrogen fuel and collapse into a white dwarf. Death of Medium-Mass Stars Stars with masses similar to the sun evolve ...
... Death of Low-Mass Stars Stars less than one-half the mass of the sun never evolve to the red giant stage but remain in the stable main-sequence stage until they consume all their hydrogen fuel and collapse into a white dwarf. Death of Medium-Mass Stars Stars with masses similar to the sun evolve ...
11.1 Stars - St John Brebeuf
... Large high mass stars often explode as supernovas, spreading elements throughout the universe. ...
... Large high mass stars often explode as supernovas, spreading elements throughout the universe. ...
ULTRASAT in a nutshell (Feb 2017)
... An alternative- Early, <1d, UV emission carries unique signatures of the progenitor (“erased” at later time): ...
... An alternative- Early, <1d, UV emission carries unique signatures of the progenitor (“erased” at later time): ...
Lecture 17, PPT version
... lines. The “synchrotron radiation” pulses are proof of the fast rotation rates of neutron stars and the presence of an incredibly strong magnetic field. ...
... lines. The “synchrotron radiation” pulses are proof of the fast rotation rates of neutron stars and the presence of an incredibly strong magnetic field. ...
History of supernova observation
The known history of supernova observation goes back to 185 CE, when, supernova SN 185 appeared, the oldest appearance of a supernova recorded by humankind. Several additional supernovae within the Milky Way galaxy have been recorded since that time, with SN 1604 being the most recent supernova to be observed in this galaxy.Since the development of the telescope, the field of supernova discovery has expanded to other galaxies. These occurrences provide important information on the distances of galaxies. Successful models of supernova behavior have also been developed, and the role of supernovae in the star formation process is now increasingly understood.