matthewchristianstarprodject
... hydrogen atoms into helium. During this stage of the star's lifetime, it is determined by its mass, but also based upon its chemical composition and other factors. All main sequence stars are in hydrostatic equilibrium, where outward thermal pressure from the core is balanced by the inward gravita ...
... hydrogen atoms into helium. During this stage of the star's lifetime, it is determined by its mass, but also based upon its chemical composition and other factors. All main sequence stars are in hydrostatic equilibrium, where outward thermal pressure from the core is balanced by the inward gravita ...
PHYS3380_111615_bw - The University of Texas at Dallas
... can move rapidly along the magnetic field and travel several light years before radiating away their energy - move much more slowly perpendicular to the magnetic field, and travel only a short distance before losing their energy. This effect can explain the long, thin, fingers and loops, as well as ...
... can move rapidly along the magnetic field and travel several light years before radiating away their energy - move much more slowly perpendicular to the magnetic field, and travel only a short distance before losing their energy. This effect can explain the long, thin, fingers and loops, as well as ...
Astronomy 103 – Midterm 2 – October 29, 2014
... 37. Two clouds of interstellar gas contract to form stars. Suppose that no mass is lost in the contraction and that when they stop contracting, cloud A is a type A star and cloud K is a type K star. What stops the contraction of each star? a) Cloud A is stopped by fusion of helium to carbon and clou ...
... 37. Two clouds of interstellar gas contract to form stars. Suppose that no mass is lost in the contraction and that when they stop contracting, cloud A is a type A star and cloud K is a type K star. What stops the contraction of each star? a) Cloud A is stopped by fusion of helium to carbon and clou ...
The Stars - Department of Physics and Astronomy
... More On Solar Structure • Hydrogen fusion takes place in a core extending from the Sun’s center to about 0.25 solar radius • The core is surrounded by a radiative zone extending to about 0.71 solar radius – In this zone, energy travels outward through radiative diffusion ...
... More On Solar Structure • Hydrogen fusion takes place in a core extending from the Sun’s center to about 0.25 solar radius • The core is surrounded by a radiative zone extending to about 0.71 solar radius – In this zone, energy travels outward through radiative diffusion ...
Lecture 5/10 The interstellar medium and star formation Ulf
... a balance between the ionisation of neutral hydrogen atoms by the ultraviolet photons and the recombination of protons and electrons. During the recombination events the electrons cascade down through the energy levels and among other spectral lines they generate the Balmer lines that can be seen in ...
... a balance between the ionisation of neutral hydrogen atoms by the ultraviolet photons and the recombination of protons and electrons. During the recombination events the electrons cascade down through the energy levels and among other spectral lines they generate the Balmer lines that can be seen in ...
Chapter 15: The Deaths of Massive Stars
... 5. Because of greater core temperatures and pressures, supergiants produce heavier elements, such as neon, silicon, and iron. 15-2 Type II Supernovae 1. Type II supernovae, which result from massive stars, reveal prominent hydrogen lines. They are powered by gravitational energy that is released as ...
... 5. Because of greater core temperatures and pressures, supergiants produce heavier elements, such as neon, silicon, and iron. 15-2 Type II Supernovae 1. Type II supernovae, which result from massive stars, reveal prominent hydrogen lines. They are powered by gravitational energy that is released as ...
Origin of Chemical Elements
... • What can we learn from telescopes? Modern telescopes (especially space telescopes) allow us to observe all the EM waves emitted by stars, not just visible ...
... • What can we learn from telescopes? Modern telescopes (especially space telescopes) allow us to observe all the EM waves emitted by stars, not just visible ...
P2_5 The Apparent Magnitude of α Orionis Supernova
... The star α Orionis (Betelgeuse) is to become a type II supernova at the end of its life. Some have postulated that this supernova will be bright enough that it will be visible during the day. Betelgeuse will have an apparent magnitude of around -8.7, brighter than Venus, which can be seen when the s ...
... The star α Orionis (Betelgeuse) is to become a type II supernova at the end of its life. Some have postulated that this supernova will be bright enough that it will be visible during the day. Betelgeuse will have an apparent magnitude of around -8.7, brighter than Venus, which can be seen when the s ...
Stellar Evolution
... main-sequence star becomes a giant • When hydrogen fusion ceases in the core, the star will collapse inward – this causes the layer just outside the core to become so hot and dense so that hydrogen fusion will begin in this outer layer. • The energy produced by hydrogen fusion in this layer just out ...
... main-sequence star becomes a giant • When hydrogen fusion ceases in the core, the star will collapse inward – this causes the layer just outside the core to become so hot and dense so that hydrogen fusion will begin in this outer layer. • The energy produced by hydrogen fusion in this layer just out ...
CHP 13
... c. white dwarfs must contain more than 1.4 solar masses. d. not all stars will end up as white dwarfs. e. stars with a mass less than 0.5 solar masses will not go through helium flash. 4. In A.D. 1054, Chinese astronomers observed the appearance of a new star, whose location is now occupied by a. a ...
... c. white dwarfs must contain more than 1.4 solar masses. d. not all stars will end up as white dwarfs. e. stars with a mass less than 0.5 solar masses will not go through helium flash. 4. In A.D. 1054, Chinese astronomers observed the appearance of a new star, whose location is now occupied by a. a ...
The Death of Stars
... c. white dwarfs must contain more than 1.4 solar masses. d. not all stars will end up as white dwarfs. e. stars with a mass less than 0.5 solar masses will not go through helium flash. 4. In A.D. 1054, Chinese astronomers observed the appearance of a new star, whose location is now occupied by a. a ...
... c. white dwarfs must contain more than 1.4 solar masses. d. not all stars will end up as white dwarfs. e. stars with a mass less than 0.5 solar masses will not go through helium flash. 4. In A.D. 1054, Chinese astronomers observed the appearance of a new star, whose location is now occupied by a. a ...
Thermonuclear supernovae and cosmology
... • SNIa: Thermonuclear supernovae. Theory • Core-collapse supernovae: theory ...
... • SNIa: Thermonuclear supernovae. Theory • Core-collapse supernovae: theory ...
pdf of paper
... protons. Amazingly enough, another heliwn nucleus collides \\ith this shortlived target, leading to the formation of carbon. The process would seem about as likely as crossing a stream by stepping fleetingly on a log. A delicate match between the energies of helium, the unstable berylJium and the re ...
... protons. Amazingly enough, another heliwn nucleus collides \\ith this shortlived target, leading to the formation of carbon. The process would seem about as likely as crossing a stream by stepping fleetingly on a log. A delicate match between the energies of helium, the unstable berylJium and the re ...
Xtra_credit_MC_chapt_10−12_2014.txt Xtra_credit_MC_chapt_10
... outer shells of the star is expelled with velocities up to: a) 1% the speed of light b) 5% the speed of light c) 10% the speed of light d) 20% the speed of light e) 50% the speed of light 6) In the video it is said that if the initial mass of the star is GREATER than ____________ times the mass of t ...
... outer shells of the star is expelled with velocities up to: a) 1% the speed of light b) 5% the speed of light c) 10% the speed of light d) 20% the speed of light e) 50% the speed of light 6) In the video it is said that if the initial mass of the star is GREATER than ____________ times the mass of t ...
Astronomy
... Which of the following can actually escape a black hole? A. Electrons. B. Very high energy gamma-rays. C. Visible light. D. Very low energy radio waves. E. None of the above. ...
... Which of the following can actually escape a black hole? A. Electrons. B. Very high energy gamma-rays. C. Visible light. D. Very low energy radio waves. E. None of the above. ...
Deaths of Stars - Chabot College
... if white dwarf mass greater than 1.4 M Chandrasekhar Limit Subrahmanyan Chandrasekhar ...
... if white dwarf mass greater than 1.4 M Chandrasekhar Limit Subrahmanyan Chandrasekhar ...
Merging white dwarfs and thermonuclear supernovae
... (a) The paucity of possible progenitor systems Over the age of the Universe, for every Solar mass of stars formed, approximately 0.0023 ± 0.0006 SN Ia seem to occur [5,6]. Because approximately 0.22 white dwarfs are expected for every Solar mass formed (the remainder being in low-mass stars that are ...
... (a) The paucity of possible progenitor systems Over the age of the Universe, for every Solar mass of stars formed, approximately 0.0023 ± 0.0006 SN Ia seem to occur [5,6]. Because approximately 0.22 white dwarfs are expected for every Solar mass formed (the remainder being in low-mass stars that are ...
WEEK 8: CSI UCSC: ASTRO EDITION SOLUTIONS This week you
... Remember that really massive stars die to become black holes. (1) Which force has triumphed in a black hole? Gravity has triumphed in a black hole. Not even neutron degeneracy pressure was sufficient to fight against gravity, and since the star cannot muster up anything else, gravity wins. (2) Where ...
... Remember that really massive stars die to become black holes. (1) Which force has triumphed in a black hole? Gravity has triumphed in a black hole. Not even neutron degeneracy pressure was sufficient to fight against gravity, and since the star cannot muster up anything else, gravity wins. (2) Where ...
Talk
... The temperature rise increases the pressure, expanding the gas just enough to cool the gas back down and stabilize the rate of fusion Thermal equilibrium is maintained ...
... The temperature rise increases the pressure, expanding the gas just enough to cool the gas back down and stabilize the rate of fusion Thermal equilibrium is maintained ...
answers2008_09_BC
... Explain how the heavy elements are produced in stars and disseminated into the interstellar gas. Your account should include the following terms: fusion; s-process; r-process; β-decay; planetary nebula; supernova. [5] convection currents in helium-burning stars carry heavy elements up from core to ...
... Explain how the heavy elements are produced in stars and disseminated into the interstellar gas. Your account should include the following terms: fusion; s-process; r-process; β-decay; planetary nebula; supernova. [5] convection currents in helium-burning stars carry heavy elements up from core to ...
OVERVIEW: Stars and space
... Explain the additional stages undergone by the most massive stars. Your account should include what is meant by (a) supernova, (b) neutron star, and (c) black hole. (a) How does a star produce energy? (b) Explain why the Sun is neither expanding or contracting at the present time. Copy and answer qu ...
... Explain the additional stages undergone by the most massive stars. Your account should include what is meant by (a) supernova, (b) neutron star, and (c) black hole. (a) How does a star produce energy? (b) Explain why the Sun is neither expanding or contracting at the present time. Copy and answer qu ...
Forging the elements
... What mass of hydrogen is converted to helium in one second? Mass s-1 = luminosity / c2: 4 x 109 kg s-1 How long can the sun survive by burning hydrogen? Hydrogen burning lifetime = Total mass available for conversion Rate of conversion Lifetime ~ mass available x c2 / L ~ 1010 years. Our sun is roug ...
... What mass of hydrogen is converted to helium in one second? Mass s-1 = luminosity / c2: 4 x 109 kg s-1 How long can the sun survive by burning hydrogen? Hydrogen burning lifetime = Total mass available for conversion Rate of conversion Lifetime ~ mass available x c2 / L ~ 1010 years. Our sun is roug ...
Where Do Chemical Elements Come From?
... of the first 26 elements in the periodic table, from simple elements, such as helium and carbon, to more complex ones, such as manganese and iron; and the giant explosion sprayed them in space. During the explosion, other elements were created as well, and after the explosion, the chemicals in space ...
... of the first 26 elements in the periodic table, from simple elements, such as helium and carbon, to more complex ones, such as manganese and iron; and the giant explosion sprayed them in space. During the explosion, other elements were created as well, and after the explosion, the chemicals in space ...
Teachers` guide
... appearance. Also, a part of supernova explosion which is called as Type Ia has a feature that the absolute magnitude of maximum brightness becomes the same in any case. The absolute magnitude is known in that type; therefore, by comparing with the apparent magnitude, we can get a clue about measurin ...
... appearance. Also, a part of supernova explosion which is called as Type Ia has a feature that the absolute magnitude of maximum brightness becomes the same in any case. The absolute magnitude is known in that type; therefore, by comparing with the apparent magnitude, we can get a clue about measurin ...
Publisher: Emily Barrosse Acquisitions Editor: Kelley Tyner
... Somehow, through a series of winds and planetary-nebula ejections, all stars up to 8 (or perhaps even 10) times the Sun’s mass manage to lose most of their mass, so the remaining stellar core is below 1.4 times the Sun’s mass. (The Sun itself will have only 0.6 of its current mass at that time, in a ...
... Somehow, through a series of winds and planetary-nebula ejections, all stars up to 8 (or perhaps even 10) times the Sun’s mass manage to lose most of their mass, so the remaining stellar core is below 1.4 times the Sun’s mass. (The Sun itself will have only 0.6 of its current mass at that time, in a ...
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.