test - Scioly.org
... during this event, the condition is temporary. 13) AM CVn stars differ from most other cataclysmic variables (CVs) in the abundance of hydrogen lines from their spectra. 14) Neutron Stars result from the supernova explosion of a massive star, combined with gravitational collapse, that compresses the ...
... during this event, the condition is temporary. 13) AM CVn stars differ from most other cataclysmic variables (CVs) in the abundance of hydrogen lines from their spectra. 14) Neutron Stars result from the supernova explosion of a massive star, combined with gravitational collapse, that compresses the ...
Notes - Michigan State University
... For radial motion (with respect to the center of the nucleus), angular momentum conservation (central potential !) leads to an energy barrier for non zero angular momentum. Classically, one needs the radial kinetic energy to overcome the central potential, but if d != 0 then there is an increasing a ...
... For radial motion (with respect to the center of the nucleus), angular momentum conservation (central potential !) leads to an energy barrier for non zero angular momentum. Classically, one needs the radial kinetic energy to overcome the central potential, but if d != 0 then there is an increasing a ...
Star formation - Grosse Pointe Public School System
... achieve high enough temperatures and pressures in their cores. • These “wanna-be” stars still glow red from light generated due to gravitational contraction. They are known as brown dwarfs, but aren’t really brown! • How does gravity create heat? When a gas is compressed, it converts some of its kin ...
... achieve high enough temperatures and pressures in their cores. • These “wanna-be” stars still glow red from light generated due to gravitational contraction. They are known as brown dwarfs, but aren’t really brown! • How does gravity create heat? When a gas is compressed, it converts some of its kin ...
exercises.electrostatics.2
... oppositely charged parallel plates. A proton is released from rest at the surface of the positively charged plate and strikes the surface of the opposite plate, 1.6 cm distant from the first, in a time interval of 1.5 10 6 s . Find i) the magnitude of the electric field and ii) the speed of the p ...
... oppositely charged parallel plates. A proton is released from rest at the surface of the positively charged plate and strikes the surface of the opposite plate, 1.6 cm distant from the first, in a time interval of 1.5 10 6 s . Find i) the magnitude of the electric field and ii) the speed of the p ...
AST1001.ch13
... The White Dwarf Limit • Quantum mechanics says that electrons must move faster as they are squeezed into a very small space. • As a white dwarf’s mass approaches 1.4MSun, its electrons must move at nearly the speed of light. • Because nothing can move faster than light, a white dwarf cannot be more ...
... The White Dwarf Limit • Quantum mechanics says that electrons must move faster as they are squeezed into a very small space. • As a white dwarf’s mass approaches 1.4MSun, its electrons must move at nearly the speed of light. • Because nothing can move faster than light, a white dwarf cannot be more ...
AY5 Announcements
... enormous explosions that end the lives of massive stars - Use of supernova explosions to map the Universe ...
... enormous explosions that end the lives of massive stars - Use of supernova explosions to map the Universe ...
black hole
... This wobble may be caused by the combined gravitational pull of two planets with 67 and 98 day orbital periods. ...
... This wobble may be caused by the combined gravitational pull of two planets with 67 and 98 day orbital periods. ...
galaxy
... of a single star. The galaxy can’t be any YOUNGER than its oldest stars, so this technique yields a MINIMUM age for the Milky Way. – Astronomers determined the star’s age by measuring its chemistry. They found that it contains only minute traces of anything heavier than hydrogen and helium, the two ...
... of a single star. The galaxy can’t be any YOUNGER than its oldest stars, so this technique yields a MINIMUM age for the Milky Way. – Astronomers determined the star’s age by measuring its chemistry. They found that it contains only minute traces of anything heavier than hydrogen and helium, the two ...
Test #4 (Ch. 13-16) ASTR 10 You have 1 hour to take the exam, and
... A. All the stars in the cluster will become main-sequence stars at about the same time. B. All the stars in the cluster will be of about the same mass. C. A few massive stars will form, live, and die before the majority of the star's clusters even complete their protostar stage. D. All the stars in ...
... A. All the stars in the cluster will become main-sequence stars at about the same time. B. All the stars in the cluster will be of about the same mass. C. A few massive stars will form, live, and die before the majority of the star's clusters even complete their protostar stage. D. All the stars in ...
Chapter 21 Notes
... Iron-56 is the most stable nucleus, so it neither fuses nor decays. However, within the cores of the most massive stars, neutron capture can create heavier elements, all the way up to ...
... Iron-56 is the most stable nucleus, so it neither fuses nor decays. However, within the cores of the most massive stars, neutron capture can create heavier elements, all the way up to ...
White Dwarfs
... • Low mass stars are unable to reach high enough temperatures to ignite elements heavier than carbon in their core become white dwarfs. • Hot exposed core of an evolved low mass star. • Supported by electron degeneracy pressure. This is the tendency of atoms to resist compression. • The more mas ...
... • Low mass stars are unable to reach high enough temperatures to ignite elements heavier than carbon in their core become white dwarfs. • Hot exposed core of an evolved low mass star. • Supported by electron degeneracy pressure. This is the tendency of atoms to resist compression. • The more mas ...
मराठ% &व( सा+ह-य-&व(: /डस1बर २००९ – जानेवार7 २०१० :ैमा<सक वष? २१ वे अंक Cतसरा
... why it stays the size it is. It shines because the Hydrogen inside it is being converted to Helium (and the Helium to higher elements). These fusion processes are what produce the heat and light. This radiation being generated in the innards of the sun also has pressure. This pressure keeps the oute ...
... why it stays the size it is. It shines because the Hydrogen inside it is being converted to Helium (and the Helium to higher elements). These fusion processes are what produce the heat and light. This radiation being generated in the innards of the sun also has pressure. This pressure keeps the oute ...
Stars: from Adolescence to Old Age
... Dying Process of Massive Stars At the end of the helium-fusion stage, a star with a mass greater than about 8 solar masses has not yet exhausted its inner resources Such a star is massive enough to cause more contraction that can trigger other kinds of fusion in its center Carbon can fuse into stil ...
... Dying Process of Massive Stars At the end of the helium-fusion stage, a star with a mass greater than about 8 solar masses has not yet exhausted its inner resources Such a star is massive enough to cause more contraction that can trigger other kinds of fusion in its center Carbon can fuse into stil ...
AST1001.ch13
... The White Dwarf Limit • Quantum mechanics says that electrons must move faster as they are squeezed into a very small space. • As a white dwarf’s mass approaches 1.4MSun, its electrons must move at nearly the speed of light. • Because nothing can move faster than light, a white dwarf cannot be more ...
... The White Dwarf Limit • Quantum mechanics says that electrons must move faster as they are squeezed into a very small space. • As a white dwarf’s mass approaches 1.4MSun, its electrons must move at nearly the speed of light. • Because nothing can move faster than light, a white dwarf cannot be more ...
I. Abundances – The Composition of the Universe
... Problem: chemical fractionation modified the local composition strongly compared to pre solar nebula and overall solar system. for example: Quarz is 1/3 Si and 2/3 Oxygen and not much else. This is not the composition of the solar system. But: Isotopic compositions mostly unaffected (as chemistry is ...
... Problem: chemical fractionation modified the local composition strongly compared to pre solar nebula and overall solar system. for example: Quarz is 1/3 Si and 2/3 Oxygen and not much else. This is not the composition of the solar system. But: Isotopic compositions mostly unaffected (as chemistry is ...
Lecture 11
... • What is a neutron star? – A ball of neutrons left over from a massive star supernova and supported by neutron degeneracy pressure • How were neutron stars discovered? – Beams of radiation from a rotating neutron star sweep through space like lighthouse beams, making them appear to pulse – Obs ...
... • What is a neutron star? – A ball of neutrons left over from a massive star supernova and supported by neutron degeneracy pressure • How were neutron stars discovered? – Beams of radiation from a rotating neutron star sweep through space like lighthouse beams, making them appear to pulse – Obs ...
Part B
... pressure. This sets max mass for a white dwarf, Chandrasekhar limit, at approximately 1.4 solar masses. Beyond this it cannot be supported by degeneracy pressure alone. Type I supernova occurs when white dwarf acquires additional mass from a companion star, usually a red giant. At critical mass (> 1 ...
... pressure. This sets max mass for a white dwarf, Chandrasekhar limit, at approximately 1.4 solar masses. Beyond this it cannot be supported by degeneracy pressure alone. Type I supernova occurs when white dwarf acquires additional mass from a companion star, usually a red giant. At critical mass (> 1 ...
Life Cycle of a Star - Intervention Worksheet
... A dying red super giant star can suddenly explode. The explosion is called a supernova. After the star explodes, some of the materials from the star are left behind. This material may form a neutron star. Neutron stars are the remains of high-mass stars. The most massive stars become black holes whe ...
... A dying red super giant star can suddenly explode. The explosion is called a supernova. After the star explodes, some of the materials from the star are left behind. This material may form a neutron star. Neutron stars are the remains of high-mass stars. The most massive stars become black holes whe ...
Energy Sources in Stars
... MH available = 0.1 Msun MH destroyed through fusion = 0.1 Msun x 0.007 total nuclear energy available Etot = (7 x 10-4 Msun)c2 ~ 1.3 x 1044 J Sun’s total lifetime energy output = 6 x 1043 J Etot ~ 2 x the total energy Sun has emitted!! Sun could shine for at least another 5 x 109 yr at its curren ...
... MH available = 0.1 Msun MH destroyed through fusion = 0.1 Msun x 0.007 total nuclear energy available Etot = (7 x 10-4 Msun)c2 ~ 1.3 x 1044 J Sun’s total lifetime energy output = 6 x 1043 J Etot ~ 2 x the total energy Sun has emitted!! Sun could shine for at least another 5 x 109 yr at its curren ...
P-nuclei
p-Nuclei (p stands for proton-rich) are certain proton-rich, naturally occurring isotopes of some elements between selenium and mercury which cannot be produced in either s- or r-process.