The Life Cycle of Stars Stars are a fascinating part of our universe
... (97%) and Helium (3%) gas. Gravity causes the dust and gas to clump together. The number of atoms in the clump increases and the mass of the clump increases. This initial mass determines the mass of the star. As the gravitational attraction in the nebula grows the clump contracts and flattens into a ...
... (97%) and Helium (3%) gas. Gravity causes the dust and gas to clump together. The number of atoms in the clump increases and the mass of the clump increases. This initial mass determines the mass of the star. As the gravitational attraction in the nebula grows the clump contracts and flattens into a ...
Folie 1
... isothermic • H burning shell core increases in mass • maximum core mass ~ 10% stellar mass core collapse • low mass stars: core degenerates first ...
... isothermic • H burning shell core increases in mass • maximum core mass ~ 10% stellar mass core collapse • low mass stars: core degenerates first ...
New Scientist - Quark Nova Project
... shedding magnetic fields. Over time, this loss of energy causes the star to spin slower and slower. As it spins down, the centrifugal forces that kept gravity at bay start weakening, allowing gravity to squish the star still further. In what is a blink of an eye in cosmic time, the neutrons can be c ...
... shedding magnetic fields. Over time, this loss of energy causes the star to spin slower and slower. As it spins down, the centrifugal forces that kept gravity at bay start weakening, allowing gravity to squish the star still further. In what is a blink of an eye in cosmic time, the neutrons can be c ...
Star in a Box
... Running out of helium • Eventually the helium is exhausted, and the star collapses again. • If it is massive enough, then the temperature increases enough to allow carbon fusion. • The cycle repeats, fusing heavier elements each time, until the core temperature cannot rise any higher. • At this poi ...
... Running out of helium • Eventually the helium is exhausted, and the star collapses again. • If it is massive enough, then the temperature increases enough to allow carbon fusion. • The cycle repeats, fusing heavier elements each time, until the core temperature cannot rise any higher. • At this poi ...
Chapter 13
... History of Stellar Evolution Theories • Aristotle wrote more than 2000 years ago that stars are heated by their passage through the heavens, but never considered that they evolved • In the 18th century, Immanuel Kant described the Sun as a fiery sphere, formed from the gases gravitated to the cente ...
... History of Stellar Evolution Theories • Aristotle wrote more than 2000 years ago that stars are heated by their passage through the heavens, but never considered that they evolved • In the 18th century, Immanuel Kant described the Sun as a fiery sphere, formed from the gases gravitated to the cente ...
Sec 29.3 - Highland High School
... A more massive star begins its life with hydrogen being converted to helium, but it is much higher on the main sequence. The star’s lifetime in this phase is short because the star is very luminous and uses up its fuel quickly. When the white dwarf cools and loses its luminosity, it becomes an undet ...
... A more massive star begins its life with hydrogen being converted to helium, but it is much higher on the main sequence. The star’s lifetime in this phase is short because the star is very luminous and uses up its fuel quickly. When the white dwarf cools and loses its luminosity, it becomes an undet ...
An absence of ex-companion stars in the type Ia supernova remnant
... A type Ia supernova is thought to begin with the explosion of a white dwarf star1. The explosion could be triggered by the merger of two white dwarfs2,3 (a ‘double-degenerate’ origin), or by mass transfer from a companion star4,5 (the ‘single-degenerate’ path). The identity of the progenitor is stil ...
... A type Ia supernova is thought to begin with the explosion of a white dwarf star1. The explosion could be triggered by the merger of two white dwarfs2,3 (a ‘double-degenerate’ origin), or by mass transfer from a companion star4,5 (the ‘single-degenerate’ path). The identity of the progenitor is stil ...
Pulsars
... • Pulsating X-ray sources / X-ray pulsators - compact objects (generally neutron stars) in binary systems Accrete matter from normal star companion (P ~ 10s, dP/dt < 0) ...
... • Pulsating X-ray sources / X-ray pulsators - compact objects (generally neutron stars) in binary systems Accrete matter from normal star companion (P ~ 10s, dP/dt < 0) ...
dark matter
... We talked about core-collapse supernovae, which are the end result of the lives of very massive stars. These are also called Type II supernovae Type Ia supernovae result from binary system in which matter is flowing from a red giant onto a white dwarf. ...
... We talked about core-collapse supernovae, which are the end result of the lives of very massive stars. These are also called Type II supernovae Type Ia supernovae result from binary system in which matter is flowing from a red giant onto a white dwarf. ...
Dark matter in the Galactic Halo Rotation curve (i.e. the orbital
... matter - made (originally) from ordinary gas ...
... matter - made (originally) from ordinary gas ...
lab 14B - atomic challenge
... atoms together to make other elements, such as helium. Along the way, a few protons get converted into neutrons and electrons. In this investigation, you will learn how these subatomic particles are arranged to make up the structure of an atom by playing the game of Atomic Challenge. ...
... atoms together to make other elements, such as helium. Along the way, a few protons get converted into neutrons and electrons. In this investigation, you will learn how these subatomic particles are arranged to make up the structure of an atom by playing the game of Atomic Challenge. ...
Astronomy 328 Midterm Exam - Department of Physics and Astronomy
... a) Here are a few questions to test your general understanding of stellar structure and evolution i) ...
... a) Here are a few questions to test your general understanding of stellar structure and evolution i) ...
Chemical Evolution of the Galaxy and its satellites
... They die as C-O white dwarfs, when single, and can die as Type Ia SNe when binaries • Massive stars (M>8-10 Msun, core-collapse SNe): they produce mainly alpha-elements (O, Mg..), some Fe, light s-process elements and r-process elements and explode as core-collapse SNe • Type Ia SNe produce mainly F ...
... They die as C-O white dwarfs, when single, and can die as Type Ia SNe when binaries • Massive stars (M>8-10 Msun, core-collapse SNe): they produce mainly alpha-elements (O, Mg..), some Fe, light s-process elements and r-process elements and explode as core-collapse SNe • Type Ia SNe produce mainly F ...
Nature paper - University of Southampton
... line with its stellar mass content when compared with the Milky Way. In the context of studying neutron star formation channels, it is useful to focus on well-defined, simple and ‘clean’ populations of neutron-star-hosting systems (that is, systems in which the orbital parameters have not yet evolve ...
... line with its stellar mass content when compared with the Milky Way. In the context of studying neutron star formation channels, it is useful to focus on well-defined, simple and ‘clean’ populations of neutron-star-hosting systems (that is, systems in which the orbital parameters have not yet evolve ...
Star and Earth Chemistry Lecture Notes (PDF
... Outline the main processes that have lead to synthesis of the elements in the universe. Describe how differentiation of the elements occurred during formation of the earth. Describe how differentiation of the elements occurred during evolution of the earth. Understand and interpret basic phase diagr ...
... Outline the main processes that have lead to synthesis of the elements in the universe. Describe how differentiation of the elements occurred during formation of the earth. Describe how differentiation of the elements occurred during evolution of the earth. Understand and interpret basic phase diagr ...
Introduction to Electromagnetism
... Dark Matter is whatever causes the observed (for decades) gravitational dynamics in galaxies – most of it does not shine Dark Energy is whatever causes the observed (since about 2001) ACCELERATING expansion of the universe What is Dark Energy? Vacuum pressure due to virtual particle creation? H ...
... Dark Matter is whatever causes the observed (for decades) gravitational dynamics in galaxies – most of it does not shine Dark Energy is whatever causes the observed (since about 2001) ACCELERATING expansion of the universe What is Dark Energy? Vacuum pressure due to virtual particle creation? H ...
Supernovae - University of Texas Astronomy Home Page
... random, so a long interval with none is not particularly surprising, just disappointing. We do observe a young expanding gaseous remnant of an exploded star, a powerful emitter of radio radiation known as Cassiopeia A. From the present size and rate of expansion of the remnant, we deduce that the ex ...
... random, so a long interval with none is not particularly surprising, just disappointing. We do observe a young expanding gaseous remnant of an exploded star, a powerful emitter of radio radiation known as Cassiopeia A. From the present size and rate of expansion of the remnant, we deduce that the ex ...
Recipe for a Star
... it forms another vital element for life, oxygen. The core region of the star now consists of a mixture of carbon, nitrogen, oxygen, helium, and hydrogen. All of those elements are undergoing nuclear fusion and beginning to separate into distinctive layers. Step 3: Form new layers as more fusion reac ...
... it forms another vital element for life, oxygen. The core region of the star now consists of a mixture of carbon, nitrogen, oxygen, helium, and hydrogen. All of those elements are undergoing nuclear fusion and beginning to separate into distinctive layers. Step 3: Form new layers as more fusion reac ...
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.