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... 3. Students incorrectly think that our Sun will end as a supernova explosion. All stars that are about 8 MSun or greater will end as a supernova, leaving some kind of stellar remnant (e.g., a neutron star or black hole). Specifically, these massive stars will end as a Type II supernova. In massive ...
... 3. Students incorrectly think that our Sun will end as a supernova explosion. All stars that are about 8 MSun or greater will end as a supernova, leaving some kind of stellar remnant (e.g., a neutron star or black hole). Specifically, these massive stars will end as a Type II supernova. In massive ...
key - Scioly.org
... B0IVe. Which of the following inferences about the two stars is incorrect? [2] (a) Cygnus OB2-12 is younger than Gamma Cassiopeiea (b) Cygnus OB2-12 is a variable star, whereas Gamma Cassiopeiea is not (c) Gamma Cassiopeiea has a circumstellar disk, while Cygnus OB2-12 does not (d) Gamma Cassiopeiea ...
... B0IVe. Which of the following inferences about the two stars is incorrect? [2] (a) Cygnus OB2-12 is younger than Gamma Cassiopeiea (b) Cygnus OB2-12 is a variable star, whereas Gamma Cassiopeiea is not (c) Gamma Cassiopeiea has a circumstellar disk, while Cygnus OB2-12 does not (d) Gamma Cassiopeiea ...
Life as a Low
... clusters show star becomes larger, redder, and more luminous after its time on the main sequence is over. ...
... clusters show star becomes larger, redder, and more luminous after its time on the main sequence is over. ...
white dwarfs.
... Question 16 As stars evolve during their main-sequence lifetime, a) they gradually become cooler and dimmer (spectral type O to type M). b) they gradually become hotter and brighter (spectral type M to type O). c) they don’t change their spectral type. Explanation: A star’s main-sequence characteri ...
... Question 16 As stars evolve during their main-sequence lifetime, a) they gradually become cooler and dimmer (spectral type O to type M). b) they gradually become hotter and brighter (spectral type M to type O). c) they don’t change their spectral type. Explanation: A star’s main-sequence characteri ...
Lecture7
... in finally in the core, elements heavier than C and O would be synthesized. So, their core will consist of elements heavier than C and O, e.g., Mg, Si, but not Fe. However, some calculations show that some of these stars on the heavier side, near 8M☉, may manage to become a supernova, but it will be ...
... in finally in the core, elements heavier than C and O would be synthesized. So, their core will consist of elements heavier than C and O, e.g., Mg, Si, but not Fe. However, some calculations show that some of these stars on the heavier side, near 8M☉, may manage to become a supernova, but it will be ...
Solutions
... by the newly formed OB Association stars that emit most of their energy as high-energy short-wavelength hardUV photons. The photons from the OB Association stars “power up” the HII region and keep it fluorescing. Thus the OB Association forms first and then the HII region is created around the vicin ...
... by the newly formed OB Association stars that emit most of their energy as high-energy short-wavelength hardUV photons. The photons from the OB Association stars “power up” the HII region and keep it fluorescing. Thus the OB Association forms first and then the HII region is created around the vicin ...
AST1100 Lecture Notes
... in another helium shell flash. The star is very unstable and the repeated helium flashes result in huge mass losses from the star. The outer layers of the star are blown away in the helium flashes (this is one of the theories describing the huge mass losses the star undergoes in this period). A huge ...
... in another helium shell flash. The star is very unstable and the repeated helium flashes result in huge mass losses from the star. The outer layers of the star are blown away in the helium flashes (this is one of the theories describing the huge mass losses the star undergoes in this period). A huge ...
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... Share and discuss your results with the rest of the class. Determine if your team’s answers are reasonable. ...
... Share and discuss your results with the rest of the class. Determine if your team’s answers are reasonable. ...
the life cycles of stars (5) - U3A Bendigo Courses / Activities
... Ceti is an LPV (Long Period Variable) with a pulsation period of about 11 months. When bright (for about 2 months) it is about 3rd or 4th magnitude. When dim (most of the time) it is invisible. There would be some years when it was not seen at all, hence its name. This photograph in UV was taken i ...
... Ceti is an LPV (Long Period Variable) with a pulsation period of about 11 months. When bright (for about 2 months) it is about 3rd or 4th magnitude. When dim (most of the time) it is invisible. There would be some years when it was not seen at all, hence its name. This photograph in UV was taken i ...
LAGUNA
... Study of gravitational collapse (Supernova Neutrinos) Study of star formation in the early universe (Diffuse Supernovae Neutrinos Background) Precision study of thermonuclear fusion processes (Solar Neutrinos) Test of geophysical models ...
... Study of gravitational collapse (Supernova Neutrinos) Study of star formation in the early universe (Diffuse Supernovae Neutrinos Background) Precision study of thermonuclear fusion processes (Solar Neutrinos) Test of geophysical models ...
The correct answers are written in bold, italic and underlined. The
... • The iron is thrown out into space, enriching the interstellar medium. The temperature reaches about 5 billion K during the core collapse that initiates the supernova explosion, and at this temperature the gamma-ray photons are energetic enough to photodisintegrate the iron nuclei into protons and ...
... • The iron is thrown out into space, enriching the interstellar medium. The temperature reaches about 5 billion K during the core collapse that initiates the supernova explosion, and at this temperature the gamma-ray photons are energetic enough to photodisintegrate the iron nuclei into protons and ...
Distance Ladder
... •Typically 300 km/s or so How to to determine distances: is moving away from us at •Measure v using Doppler shift 2100 km/s? A) 1 Mly D) 484 Mly •Deduce the distance from: B) 10 Mly E) 4,840 Mly v = H0d C) 100 Mly F) 48,400 Mly ...
... •Typically 300 km/s or so How to to determine distances: is moving away from us at •Measure v using Doppler shift 2100 km/s? A) 1 Mly D) 484 Mly •Deduce the distance from: B) 10 Mly E) 4,840 Mly v = H0d C) 100 Mly F) 48,400 Mly ...
Stellar Evolution
... star (in the region where the temperature is above 15 million degrees Kelvin), and it will do so for roughly 100 thousand (massive stars) to 100 billion years (low mass stars). Changes do occur, but over long, long time scales, so that main sequence stars are indeed in thermal and hydrostatic equili ...
... star (in the region where the temperature is above 15 million degrees Kelvin), and it will do so for roughly 100 thousand (massive stars) to 100 billion years (low mass stars). Changes do occur, but over long, long time scales, so that main sequence stars are indeed in thermal and hydrostatic equili ...
1:45 PM TuTh This is a one-quarter course on
... has some familiarity with basic scientific concepts and reasoning. Elementary calculus will some times be used in classroom derivations because, for those understanding calculus, it is the easiest and clearest way of obtaining results. It is not expected, however, that the student will need to use c ...
... has some familiarity with basic scientific concepts and reasoning. Elementary calculus will some times be used in classroom derivations because, for those understanding calculus, it is the easiest and clearest way of obtaining results. It is not expected, however, that the student will need to use c ...
Ch12&13 Life and Death of Stars
... What happens to a white dwarf when it accretes enough matter to reach the 1.4 MSun limit? A. It explodes B. It collapses into a neutron star C. It gradually begins fusing carbon in its core ...
... What happens to a white dwarf when it accretes enough matter to reach the 1.4 MSun limit? A. It explodes B. It collapses into a neutron star C. It gradually begins fusing carbon in its core ...
Life on the Main Sequence + Expansion to Red Giant
... Stars form from the interstellar medium and reach stability fusing hydrogen in their cores. This chapter is about the long, stable middle age of stars on the main sequence and their old age as they swell to become giant stars. Here you will answer four essential questions: • Why is there a main sequ ...
... Stars form from the interstellar medium and reach stability fusing hydrogen in their cores. This chapter is about the long, stable middle age of stars on the main sequence and their old age as they swell to become giant stars. Here you will answer four essential questions: • Why is there a main sequ ...
The Lives of Stars
... “evaporate,” from such a cluster • A stellar association is a group of newborn stars that are moving apart so rapidly that their gravitational attraction for one another cannot pull them into orbit about one another ...
... “evaporate,” from such a cluster • A stellar association is a group of newborn stars that are moving apart so rapidly that their gravitational attraction for one another cannot pull them into orbit about one another ...
Helium Fusion What Will Happen When There Is No More Helium in
... • Low mass: < 2 times the Sun • Intermediate mass: 2-8 times the Sun • High mass: > 8 times the Sun ...
... • Low mass: < 2 times the Sun • Intermediate mass: 2-8 times the Sun • High mass: > 8 times the Sun ...
Encyclopedia of Optical Engineering Stellar Evolution
... on the helium core compresses the electrons into the quantum mechanical state known as electron degeneracy. In this configuration, the electrons become closely ‘‘stacked’’ in space, separated by the Pauli exclusion principle: No two electrons can have the same four quantum numbers relating to energy ...
... on the helium core compresses the electrons into the quantum mechanical state known as electron degeneracy. In this configuration, the electrons become closely ‘‘stacked’’ in space, separated by the Pauli exclusion principle: No two electrons can have the same four quantum numbers relating to energy ...
Why is there a main sequence?
... Stars form from the interstellar medium and reach stability fusing hydrogen in their cores. This chapter is about the long, stable middle age of stars on the main sequence, and their old age as they swell to become giant stars. Here you will answer four important questions: • Why is there a main seq ...
... Stars form from the interstellar medium and reach stability fusing hydrogen in their cores. This chapter is about the long, stable middle age of stars on the main sequence, and their old age as they swell to become giant stars. Here you will answer four important questions: • Why is there a main seq ...
55-80 BIOGRAPHY_of_A STAR
... forming a much smaller (~10km~Boston) neutron star (me/mn ~ 1/2000) … then collapsing to a black hole if 12 msun ...
... forming a much smaller (~10km~Boston) neutron star (me/mn ~ 1/2000) … then collapsing to a black hole if 12 msun ...
Nucleosynthesis and the death of stars
... • A Type I supernova is a massive explosion of a star that occurs under two possible scenarios. The first is that a white dwarf star undergoes a nuclear based explosion after it reaches its Chandrasekhar limit (1.44 solar masses) from absorbing mass from a neighboring star (usually a red giant). • A ...
... • A Type I supernova is a massive explosion of a star that occurs under two possible scenarios. The first is that a white dwarf star undergoes a nuclear based explosion after it reaches its Chandrasekhar limit (1.44 solar masses) from absorbing mass from a neighboring star (usually a red giant). • A ...
Penentuan Jarak dalam Astronomi II
... Last two SNe in our Milky Way Galaxy: SN 1572 (Tycho Brage’s supernova Ia (?) in the Cassiopeia constellation) achieved -4m at the maximun brightness SN 1604 (Kepler’s supernova Ia in the Ophiuchus constellation) achieved -2.5m As expected, we could have miss a number of Supernovae events that have ...
... Last two SNe in our Milky Way Galaxy: SN 1572 (Tycho Brage’s supernova Ia (?) in the Cassiopeia constellation) achieved -4m at the maximun brightness SN 1604 (Kepler’s supernova Ia in the Ophiuchus constellation) achieved -2.5m As expected, we could have miss a number of Supernovae events that have ...
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.