http://astro.phys.utk.edu/ 2015-04-06T05:59:20-04:00 http://astro.phys.utk.edu/ http://astro.phys.utk.edu/lib/images/favicon.ico text/html 2010-02-02T12:58:08-04:00 http://astro.phys.utk.edu/activities:atomscouldtell.mov?rev=1265133488&do=diff This movie discusses the origin of the chemical elements that make up our bodies and our world. This story links us to a wide range of astronomical events far away in space and time. The movie is based on a slide show given by Hix at the 2006 Sigma Xi annual metting. text/html 2009-03-31T16:46:54-04:00 http://astro.phys.utk.edu/activities:boltztran?rev=1238532414&do=diff Spherically Symmetric Models Agile-BOLTZTRAN is our platform for high-quality, detailed one-dimensional simulations of stellar core-collapse and supernovae. Agile is a spherically symmetric, adaptive-mesh hydrodynamics code with a complete treatment of general relativity. Agile is coupled to BOLTZTRAN, a spherically symmetric, multi-flavor, multi-group, discrete ordinates Boltzmann neutrino transport code with detailed neutrino-matter interactions. Agile-BOLTZTRAN remains a valuable tool for … text/html 2009-03-31T16:46:19-04:00 http://astro.phys.utk.edu/activities:ccsn?rev=1238532379&do=diff The Mechanism of Core Collapse Supernovae Core-collapse supernovae are the death throes of massive stars, more than 8-10 times the mass of our sun. They are a dominant source of elements in the Universe, without which life would be impossible. Our group is focused on ascertaining the core-collapse supernova mechanism - how the explosions of these stars are initiated - and understanding the new elements that are produced in the explosion. Core-collapse supernovae are three-dimensional, multi-ph… text/html 2012-12-10T20:15:41-04:00 http://astro.phys.utk.edu/activities:chimera?rev=1355188541&do=diff 2D/3D Ray-by-Ray Neutrino Radiation Hydrodynamics with CHIMERA Our current tool for 2D and 3D supernova simulations is the CHIMERA code. Developed by the CHIMERA team including Steve Bruenn (FAU), John Blondin (NCSU) & Pedro Marronetti (FAU), and UT/ORNL group members Raph Hix, Eric Lentz, Bronson Messer and Tony Mezzacappa, the CHIMERA code employs “ray-by-ray” (RBR) neutrino transport, using Bruenn’s multi-group flux limited diffusion (MGFLD) code, coupled to the Blondin's MVH-3 hydrodyn… text/html 2009-03-31T16:49:40-04:00 http://astro.phys.utk.edu/activities:conuc?rev=1238532580&do=diff Nucleosynthesis in Novae and X-ray Bursts We have study nova nucleosynthesis, collaborating with S. Starrfield (AZ State) in modeling novae. An article has been accepted for publication in the Astrophysical Journal detailing a series of simulations using nuclear datasets prepared by C. Iliadis (UNC) that illustrate the impact that recent reaction rate measurements have on nova outburst modeling. In addition to factor of 2-3 differences in the abundances of key nuclear species thought to resu… text/html 2014-08-22T15:40:22-04:00 http://astro.phys.utk.edu/activities:genasis?rev=1408736422&do=diff GenASiS: AMR code for True 2D/3D Neutrino Transport To study the mechanism of core-collapse supernova with true 2D/3D neutrino transport, we are developing a new adaptive mesh refinement (AMR) code that couples six-dimensional (three space, three momentum space) special relativistic Boltzmann neutrino transport to three-dimensional special relativistic magnetohydrodynamics, Newtonian self gravity, a nuclear equation of state, and state of the art neutrino opacities. text/html 2015-01-02T13:47:56-04:00 http://astro.phys.utk.edu/activities:index?rev=1420224476&do=diff The ultimate fate of a star depends primarily on its mass when thermonuclear fusion first ignites in its center and whether it is a single star, streaming alone through the Galaxy, or if it shares an orbit with companion star. For single stars whose mass is less than approximately 8 times the mass of the sun, their ultimate fate is to become a Red Giant star and ultimately loose their hydrogen-rich envelope as a Planetary Nebula. The core of such a star becomes a White Dwarf, composed of Heliu… text/html 2009-03-31T16:50:01-04:00 http://astro.phys.utk.edu/activities:kinetics?rev=1238532601&do=diff Numerical Methods for Thermonuclear Kinetics The need for using larger, more complete thermonuclear reaction networks in multi-dimensional astrophysics simulations, driven by the need to compare these simulations to the detailed nucleosynthesis revealed by observations, creates a need for more efficient ways to solve systems of equations. Numerical stiffness, the computational manifestation of the wide range of physical timescales active in these systems, greatly restricts the available solut… text/html 2014-10-21T13:57:23-04:00 http://astro.phys.utk.edu/activities:seminar?rev=1413914243&do=diff Date Speaker Title8/27 Organizational Meeting9/3 Eric Lentz CHIMERA supernova simulations9/10 Yuri Kamyshkov Potential Neutron Regeneration Experiment9/17 Konstantin Yakunin Gravitational Waves from Supernovae9/24 Eleftherios MoschandreouHeavy Quarkonia Bound state models10/1 Michael Smith Fires of Creation: Nuclear Information for Big Bang Studies10/8 Stefan Spanier Particle Hunt with the Large Hadron Collider10/15 Fall Break10/22Ben Rybolt Reactor Anti-neutrino Spectrum Structure10/29Loui… text/html 2009-03-31T16:48:56-04:00 http://astro.phys.utk.edu/activities:snnuc?rev=1238532536&do=diff Nucleosynthesis in Core Collapse Supernovae Among the most distinctive and important observables from supernova events are their nucleosynthesis and prodigious neutrino emission. As the source of most intermediate mass elements from oxygen to calcium, perhaps half of the iron-peak elements (including all such nuclei found in young galaxies) and the most probable site for the r-process that produces half of the species heavier than iron, core collapse supernovae are the preeminent foundry of o… text/html 2010-10-18T23:13:40-04:00 http://astro.phys.utk.edu/activities:tnsn?rev=1287458020&do=diff Thermonuclear Supernovae For single stars whose mass is less than approximately 8 times the mass of the sun, their ultimate fate is to become a Red Giant star and ultimately loose their hydrogen-rich envelope as a Planetary Nebula. The core of the star becomes a White Dwarf, composed of Helium or mixtures of Carbon and Oxygen or Oxygen and Neon, depending on the original mass of the star. Left alone, this white dwarf slowly cools and fades from view.