Stellar balancing act — dynamic equilibrium. A star spends most of
... is squeezed down, electrons develop more “uncertainty” energy depending only on the density and independent of the temperature. The electrons’ resistance to being squeezed any closer together provides pressure independent of temperature. With this pressure, a star cannot regulate its temperature. Un ...
... is squeezed down, electrons develop more “uncertainty” energy depending only on the density and independent of the temperature. The electrons’ resistance to being squeezed any closer together provides pressure independent of temperature. With this pressure, a star cannot regulate its temperature. Un ...
PPT
... 2. Inside the core, temperature increases as gas atom collisions increase. 3. Density of the core increases as more atoms try to share the same space. 4. Gas pressure increases as atomic collisions and density (atoms/space) increase. 5. The protostar’s gas pressure RESISTS the collapse of the nebula ...
... 2. Inside the core, temperature increases as gas atom collisions increase. 3. Density of the core increases as more atoms try to share the same space. 4. Gas pressure increases as atomic collisions and density (atoms/space) increase. 5. The protostar’s gas pressure RESISTS the collapse of the nebula ...
Endpoints of stellar evolution
... (massive stars here) to account for todays observed solar abundances. To explain the origin of the elements one needs to have • constant overproduction (then the pattern is solar) • sufficiently high overproduction to explain total amount of elements observed today ...
... (massive stars here) to account for todays observed solar abundances. To explain the origin of the elements one needs to have • constant overproduction (then the pattern is solar) • sufficiently high overproduction to explain total amount of elements observed today ...
The Life Cycles of Stars
... Once massive stars reach the red giant phase, the core temperature increases as carbon atoms are formed from the fusion of helium atoms. Gravity continues to pull carbon atoms together as the temperature increases forming oxygen, nitrogen, and eventually iron. At this point, fusion stops and the iro ...
... Once massive stars reach the red giant phase, the core temperature increases as carbon atoms are formed from the fusion of helium atoms. Gravity continues to pull carbon atoms together as the temperature increases forming oxygen, nitrogen, and eventually iron. At this point, fusion stops and the iro ...
File
... Formation of the Elements • Hydrogen and most of the helium in the universe are primordial, that is they date from the earliest times. • All other elements in the universe are a result of stellar nucleosynthesis: they were formed by nuclear fusion in the heart of stars. (also by processes occurring ...
... Formation of the Elements • Hydrogen and most of the helium in the universe are primordial, that is they date from the earliest times. • All other elements in the universe are a result of stellar nucleosynthesis: they were formed by nuclear fusion in the heart of stars. (also by processes occurring ...
Critical Thinking Questions 2
... (a) α decay: the nucleus loses an α particle ( !!He!! ) (b) β decay: a neutron in the nucleus is converted into a proton and an electron. The electron is ejected from the nucleus. (c) Positron or β+ emission: a proton in the nucleus is converted into a neutron and a positron. The positron is ejected ...
... (a) α decay: the nucleus loses an α particle ( !!He!! ) (b) β decay: a neutron in the nucleus is converted into a proton and an electron. The electron is ejected from the nucleus. (c) Positron or β+ emission: a proton in the nucleus is converted into a neutron and a positron. The positron is ejected ...
Lecture 18: Supernovae
... Nuclei photodisintegrate into He, p, & n Protons & electrons combine into neutrons and neutrinos, neutrinos escape and carry off energy Makes the core collapse faster, as the insufficient pressure is decreased further ...
... Nuclei photodisintegrate into He, p, & n Protons & electrons combine into neutrons and neutrinos, neutrinos escape and carry off energy Makes the core collapse faster, as the insufficient pressure is decreased further ...
states of Matter
... hydrogen nuclei, each being only a proton, may come together to form a deuterium nucleus, having one proton and one neutron in its nucleus. Or 4 hydrogen nuclei may come together to form a helium nucleus, with 2 protons and 2 neutrons present. The small change in mass is often of the order of much l ...
... hydrogen nuclei, each being only a proton, may come together to form a deuterium nucleus, having one proton and one neutron in its nucleus. Or 4 hydrogen nuclei may come together to form a helium nucleus, with 2 protons and 2 neutrons present. The small change in mass is often of the order of much l ...
Folie 1
... The star is no longer in hydrostatic equilibrium. – Gravity wins out over pressure, and the core begins to collapse and heats up. – As the core shrinks, the energy of the inward falling material is converted to heat. – Just outside the core, the hydrogen was almost, but not quite, hot enough to unde ...
... The star is no longer in hydrostatic equilibrium. – Gravity wins out over pressure, and the core begins to collapse and heats up. – As the core shrinks, the energy of the inward falling material is converted to heat. – Just outside the core, the hydrogen was almost, but not quite, hot enough to unde ...
File
... the mass of the element. Isotopes are identified by their mass, which is the total number of protons and neutrons. There are two ways that isotopes are generally written. They both use the mass of the atom where mass = (number of protons + number of neutrons). The first way is to put the mass as a s ...
... the mass of the element. Isotopes are identified by their mass, which is the total number of protons and neutrons. There are two ways that isotopes are generally written. They both use the mass of the atom where mass = (number of protons + number of neutrons). The first way is to put the mass as a s ...
TEST I 2-12-09
... Hints about exam I on Thursday 2/12/09-----I will not be able to answer emails till Monday next week. Please bring small blue Scranton that has 50 answers on one side. That way you all are at the same page. Do not bring a big one. May be just bring two of these. Just in case one goes bad or you may ...
... Hints about exam I on Thursday 2/12/09-----I will not be able to answer emails till Monday next week. Please bring small blue Scranton that has 50 answers on one side. That way you all are at the same page. Do not bring a big one. May be just bring two of these. Just in case one goes bad or you may ...
Chapter 14
... ...are stellar remnants for high-mass stars. – i.e. remnant cores with masses greater than 3 solar masses ...
... ...are stellar remnants for high-mass stars. – i.e. remnant cores with masses greater than 3 solar masses ...
PowerPoint - UCSD Department of Physics
... This is accomplished by setting Planck’s constant, the speed of light, and Boltzmann’s constant to unity, i.e., ...
... This is accomplished by setting Planck’s constant, the speed of light, and Boltzmann’s constant to unity, i.e., ...
Document
... which the Equivalence Principle guarantees are always there, the effects of gravitation are absent! The Einstein Field equations have as their solutions global coordinate systems which cover big patches of spacetime ...
... which the Equivalence Principle guarantees are always there, the effects of gravitation are absent! The Einstein Field equations have as their solutions global coordinate systems which cover big patches of spacetime ...
Life Cycles of Stars
... white dwarf star that suddenly increases in brightness by several magnitudes. It fades very slowly. ...
... white dwarf star that suddenly increases in brightness by several magnitudes. It fades very slowly. ...
Life cycle of the Stars - Christos N. Hadjichristidis
... Throughout its life, these two forces determine the stages of a star’s life. ...
... Throughout its life, these two forces determine the stages of a star’s life. ...
Radioactivityunit6
... Rutherford figured out the charged by placing an electric and magnetic field around the radioactive element to see where the particles curved. ...
... Rutherford figured out the charged by placing an electric and magnetic field around the radioactive element to see where the particles curved. ...
Document
... stable isotopes by moving along the valley of stability. Occurs in massive stars, particular AGB stars. • R-process (Rapid) – Rate of neutron capture fast compared to beta decay. Forms unstable neutron rich nuclei which decay to stable nuclei. ...
... stable isotopes by moving along the valley of stability. Occurs in massive stars, particular AGB stars. • R-process (Rapid) – Rate of neutron capture fast compared to beta decay. Forms unstable neutron rich nuclei which decay to stable nuclei. ...
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.