Spiral shock triggering of star formation
... •Local dissipation of turbulence •Star formation • SF involves ~10% of mass ...
... •Local dissipation of turbulence •Star formation • SF involves ~10% of mass ...
Powerpoint of lecture 16
... in high-energy states may be captured by Ne or Mg nuclei • Pressure drops, core cannot support itself, collapses catastrophically (timescale: 10s of milliseconds!) to nuclear densities, and bounces, leading to outward-travelling shock wave • Shock also accelerated by pressure of neutrinos, produced ...
... in high-energy states may be captured by Ne or Mg nuclei • Pressure drops, core cannot support itself, collapses catastrophically (timescale: 10s of milliseconds!) to nuclear densities, and bounces, leading to outward-travelling shock wave • Shock also accelerated by pressure of neutrinos, produced ...
Lecture102802 - FSU High Energy Physics
... gains a lot of energy “falling into” small, dense white dwarf heats up collects in shell on outside of white dwarf ...
... gains a lot of energy “falling into” small, dense white dwarf heats up collects in shell on outside of white dwarf ...
HW2 due - Yale Astronomy
... 3. (15 points) One of the nearest stars is Sirius B, a white dwarf star which orbits Sirius A, the brightest star in the sky. Sirius B has a radius of 0.0084 Rsun and a luminosity of 0.02 ...
... 3. (15 points) One of the nearest stars is Sirius B, a white dwarf star which orbits Sirius A, the brightest star in the sky. Sirius B has a radius of 0.0084 Rsun and a luminosity of 0.02 ...
Energy Generation in Stars
... Thus for a star like the sun, it will take about 10 billion years for the core hydrogen to be fully converted to Helium. We are about 1/2 way through that process now. Overall the evolutionary timescale of main sequence stars is entirely driven by stellar mass in the sense that massive stars evolve ...
... Thus for a star like the sun, it will take about 10 billion years for the core hydrogen to be fully converted to Helium. We are about 1/2 way through that process now. Overall the evolutionary timescale of main sequence stars is entirely driven by stellar mass in the sense that massive stars evolve ...
CELT Review: 1,2 May 2002 Session 1
... – Lesson from Keck is that it is difficult to anticipate the most exciting science areas a decade in advance. Major advances in capability have always resulted in unexpected new discoveries. ...
... – Lesson from Keck is that it is difficult to anticipate the most exciting science areas a decade in advance. Major advances in capability have always resulted in unexpected new discoveries. ...
Multi-physics simulations using a hierarchical interchangeable
... combined to conduct numerical experiments. The community codes are generally written independently, so AMUSE encompasses a wide variety of computer languages and programming styles. The fundamental design feature of the framework is the abstraction of the functionality of individual community codes ...
... combined to conduct numerical experiments. The community codes are generally written independently, so AMUSE encompasses a wide variety of computer languages and programming styles. The fundamental design feature of the framework is the abstraction of the functionality of individual community codes ...
Supernovae – the biggest bangs since the Big Bang
... Sun, it will make a huge explosion. The entire white dwarf will explode with the energy of four billion Suns. This is called a “white dwarf supernova” (also known as a “Type Ia supernova”). Imagine you made a series of bombs, each with the same amount of the same material. The bombs would all hav ...
... Sun, it will make a huge explosion. The entire white dwarf will explode with the energy of four billion Suns. This is called a “white dwarf supernova” (also known as a “Type Ia supernova”). Imagine you made a series of bombs, each with the same amount of the same material. The bombs would all hav ...
Variables, Star Clusters, and Nebulae (Professor Powerpoint)
... appears redder than it actually is . This happens because short wavelength , mainly blue starlight, is scattered more by dust than longer wavelength red light. This interstellar reddening is different from reddening due to the doppler shift. Doppler shift causes all wavelengths to lengthen equally, ...
... appears redder than it actually is . This happens because short wavelength , mainly blue starlight, is scattered more by dust than longer wavelength red light. This interstellar reddening is different from reddening due to the doppler shift. Doppler shift causes all wavelengths to lengthen equally, ...
Low Mass
... hydrogen in their core. • No hydrogen fusion in core • Core collapses because there is no longer balance between gravity and outward pressure (no more hydrostatic equilibrium) ...
... hydrogen in their core. • No hydrogen fusion in core • Core collapses because there is no longer balance between gravity and outward pressure (no more hydrostatic equilibrium) ...
Ecosystems, from life, to the Earth, to the Galaxy
... The stars themselves are far from thermal equilibrium, with the energy flows from their surface's radiating into cold space. The stars are stable, but non-equilibrium systems, that have their own cycle of birth, life and death. The timescale for the Galactic ecology is determined by the rate of star ...
... The stars themselves are far from thermal equilibrium, with the energy flows from their surface's radiating into cold space. The stars are stable, but non-equilibrium systems, that have their own cycle of birth, life and death. The timescale for the Galactic ecology is determined by the rate of star ...
LIGO Star Chart
... reach us, the distance between the two galaxies is getting smaller. Andromeda is moving toward the Milky Way at about 700,000 miles per hour! The best explanation for this is that the Milky Way and Andromeda are in fact a bound pair of galaxies in orbit around one another. Both galaxies are thought ...
... reach us, the distance between the two galaxies is getting smaller. Andromeda is moving toward the Milky Way at about 700,000 miles per hour! The best explanation for this is that the Milky Way and Andromeda are in fact a bound pair of galaxies in orbit around one another. Both galaxies are thought ...
Astronomy Quiz 12 “Stars
... _____2. 80% of all stars in the galaxy are __ while only 1 in 10,000 is a __. A. white dwarfs / red giant C. red giants / blue dwarfs B. yellow dwarfs / red supergiant D. red dwarfs / blue supergiant _____3. The actual 3D motion of stars relative to each other in a rotating and swirling galaxy is ca ...
... _____2. 80% of all stars in the galaxy are __ while only 1 in 10,000 is a __. A. white dwarfs / red giant C. red giants / blue dwarfs B. yellow dwarfs / red supergiant D. red dwarfs / blue supergiant _____3. The actual 3D motion of stars relative to each other in a rotating and swirling galaxy is ca ...
2. A giant hand took one of the planets discovered
... 2. A giant hand took one of the planets discovered around other stars and put it in the solar system at the same distance from the sun as from its star. The mass of the planet is approximately that of Jupiter and the orbit is approximately that of Earth. These are the “hot Jupiters”, as big as Jupit ...
... 2. A giant hand took one of the planets discovered around other stars and put it in the solar system at the same distance from the sun as from its star. The mass of the planet is approximately that of Jupiter and the orbit is approximately that of Earth. These are the “hot Jupiters”, as big as Jupit ...
Why do the stars shine?
... is U(initial)-U(final), but U(initial)=0 since the cloud radius is so much larger than the final star. • Assume the Sun has shown at constant luminosity for t years. Total energy radiated = L0x t=4x1033 ergs/sec x t. • (We know today that main sequence stars do not change luminosity over the life of ...
... is U(initial)-U(final), but U(initial)=0 since the cloud radius is so much larger than the final star. • Assume the Sun has shown at constant luminosity for t years. Total energy radiated = L0x t=4x1033 ergs/sec x t. • (We know today that main sequence stars do not change luminosity over the life of ...
Section 1
... A model atmosphere is a numerical simulation of a real stellar atmosphere, typically presented as the run of physical parameters (such as temperature) as a function of depth; here ‘depth’ generally refers to optical depth (§3.4), measured inwards. Observationally, the most easily accessible part of ...
... A model atmosphere is a numerical simulation of a real stellar atmosphere, typically presented as the run of physical parameters (such as temperature) as a function of depth; here ‘depth’ generally refers to optical depth (§3.4), measured inwards. Observationally, the most easily accessible part of ...
superbubbles vs super-galactic winds
... properties of stellar clusters, given an IMF and a stellar mass range. These are the so called synthesis models of starbursts (Mas-Hesse and Kunth 1991, Leitherer & Heckman 1995) which predict a variety of observable quantities, as well as the energetics that one is to expect from a stellar cluster, ...
... properties of stellar clusters, given an IMF and a stellar mass range. These are the so called synthesis models of starbursts (Mas-Hesse and Kunth 1991, Leitherer & Heckman 1995) which predict a variety of observable quantities, as well as the energetics that one is to expect from a stellar cluster, ...
Star Birth - Sierra College Astronomy Home Page
... radiative diffusion within the protostar • Even with radius decreasing, luminosity increases slightly • Fusion in core commences ...
... radiative diffusion within the protostar • Even with radius decreasing, luminosity increases slightly • Fusion in core commences ...
Measuring Stellar Distances
... Furthermore, the volume defined by r = 20 parsecs is only one ten-millionth of the total volume of the disk of our Galaxy. How can we be sure that this tiny volume contains a representative sample of stars? Fortunately, a theoretical argument involving stellar lifetimes serves as a consistency check ...
... Furthermore, the volume defined by r = 20 parsecs is only one ten-millionth of the total volume of the disk of our Galaxy. How can we be sure that this tiny volume contains a representative sample of stars? Fortunately, a theoretical argument involving stellar lifetimes serves as a consistency check ...
PHS 111 Test 3 Review Chapters 26-28
... outward pressure, causing spacetime to expand. All of the above Heat death refers to the universe: reaching the lowest energy state possible. ending after a massive fire. reaching a state where all stars expand and merge into each other. reaching the point where the process of radioactive decay is n ...
... outward pressure, causing spacetime to expand. All of the above Heat death refers to the universe: reaching the lowest energy state possible. ending after a massive fire. reaching a state where all stars expand and merge into each other. reaching the point where the process of radioactive decay is n ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.