Cloudy: Numerical Simulations of Plasmas and their Spectra If a picture is worth a thousand words, a spectrum is worth a thousand pictures Understanding.

Slides:



Advertisements
Similar presentations
Astronomy Notes to Accompany the Text Astronomy Today, Chaisson, McMillan Jim Mims.
Advertisements

Big Questions If astronomers measure an object’s apparent brightness (flux), what do they need to know to figure out how far away that object is? Why are.
ASTR Spring 2008 Joel E. Tohline, Alumni Professor 247 Nicholson Hall [Slides from Lecture20]
Light and Electronic Transitions. The Big Questions What is light? How is light emitted? What do electrons have to do with light? What are emission spectra?
Emission Spectra and Flame Tests. The Big Questions What is light? How is light emitted? What do electrons have to do with light? What are emission spectra?
Lecture 3: Big Bang Nucleosynthesis Last time: particle anti-particle soup --> quark soup --> neutron-proton soup. Today: –Form 2 D and 4 He –Form heavier.
Taking the fingerprints of stars, galaxies, and interstellar gas clouds Absorption and emission from atoms, ions, and molecules.
The primordial 4 He abundance: the astrophysical perspective Valentina Luridiana Instituto de Astrofísica de Andalucía (CSIC) Granada.
Lecture 2110/24/05. Light Emission vs. Absorption Black body.
Chapter 4 Spectroscopy Chapter 4 opener. Spectroscopy is a powerful observational technique enabling scientists to infer the nature of matter by the way.
Lecture 2: Physical Processes In Astrophysical and Laboratory Plasmas Lecture 1: Temperature-Density regime Many physical processes Focus on Atomic+Plasma.
SCATTERING OF RADIATION Scattering depends completely on properties of incident radiation field, e.g intensity, frequency distribution (thermal emission.
ASTR112 The Galaxy Lecture 8 Prof. John Hearnshaw 12. The interstellar medium (ISM): gas 12.1 Types of IS gas cloud 12.2 H II regions (diffuse gaseous.
Lecture II Light spectra. The Birth of the Quantum Max Planck –The energy contained in radiation is related to the frequency of the radiation by the relationship.
What Can Spectroscopy Tell Us?. Atom or Molecular Fingerprints Every atom or molecule exists in its own unique energy state. This energy state is dependent.
New advances in photoionization codes, how and what for? New advances in photoionization codes: Barbara Ercolano, UCL How and What for?
1 Nature of Light Wave Properties Light is a self- propagating electro- magnetic wave –A time-varying electric field makes a magnetic field –A time-varying.
Introduction to Plasma- Surface Interactions Lecture 3 Atomic and Molecular Processes.
Photoionization Tim Kallman NASA/GSFC What is photoionization? Removal of a bound electron by a photon Loosely refers to any situation where external photons.
The Interstellar Medium and Star Formation Material between the stars – gas and dust.
Some atomic physics u H I, O III, Fe X are spectra –Emitted by u H 0, O 2+, Fe 9+ –These are baryons u For absorption lines there is a mapping between.
Response of the Earth’s environment to solar radiative forcing
Chemistry XXI Unit 2 How do we determine structure? The central goal of this unit is to help you develop ways of thinking that can be used to predict the.
The Meudon PDR code on complex ISM structures F. Levrier P. Hennebelle, E. Falgarone, M. Gerin (LERMA - ENS) F. Le Petit (LUTH - Observatoire de Paris)
Chapter 11 The Interstellar Medium
Chapter 4 Spectroscopy The beautiful visible spectrum of the star Procyon is shown here from red to blue, interrupted by hundreds of dark lines caused.
Electron Arrangement DP Chemistry R. Slider. Electromagnetic (EM) Spectrum Wavelength The actual length of one full wave. Notice: IR > vis > UV Wavelength.
Chapter 5 The Nature of Light. Light is a wave and white light is composed of many different wavelengths.
Simulated [CII] 158 µm observations for SPICA / SAFARI F. Levrier P. Hennebelle, E. Falgarone, M. Gerin (LERMA - ENS) F. Le Petit (LUTH - Observatoire.
Chapter 4.
8 -The Interstellar Medium. Emission-Line Nebulae H II Regions Planetary Nebulae Supernova Remnants.
Collisional-Radiative Model For Atomic Hydrogen Plasma L. D. Pietanza, G. Colonna, M. Capitelli Department of Chemistry, University of Bari, Italy IMIP-CNR,
Chapter 14 The Interstellar Medium. All of the material other than stars, planets, and degenerate objects Composed of gas and dust ~1% of the mass of.
Ionization composition of dwarf galaxies Evgenii Vasiliev Institute of Physics, Southern Federal University, Rostov on Don.
Lyα Forest Simulation and BAO Detection Lin Qiufan Apr.2 nd, 2015.
Electron Arrangement Senior Chemistry R. Slider. Electromagnetic (EM) Spectrum Wavelength The actual length of one full wave. Notice: IR > vis > UV Wavelength.
The Design of a Novel Ultra High Vacuum Surface Machine to Determine the Formation of Glycolaldehyde in the Interstellar Medium By Chris Bennett.
The Interstellar Medium (ISM)
The Solar System Lesson2 Q & A
Newton studies the Sun’s spectrum
Light and Electronic Transitions
The Interstellar Medium and Star Formation
Spectroscopy and Atoms
3.2 Bohr’s model of the Atom
Details of Equation-of-State and Opacity Models
Spectroscopy.
BOHR’S ATOM AND ATOMIC SPECTRA
Universe! Early Universe.
Chapter 6: Electromagnetic Radiation
Quantum Physics Atomic spectra and atomic energy states.
The Interstellar Medium and Star Formation
Electromagnetic Radiation
Electrons and Light Chapter 13.3.
Solar Spectrum wavelength in Å Joseph von Fraunhofer, 1814.
5.3 Properties and Phases of Matter
Light and Electronic Transitions
The Bohr Model of the Atom
Spectra.
Stars and Galaxies Lesson2 Q & A
Spectra and Energy Levels in Atoms
Sections 6.1 – 6.3 Electromagnetic Radiation and its Interaction with Atoms Bill Vining SUNY College at Oneonta.
Earth Chemistry.
What we measure: Mass Temperature Electromagnetic Radiation
The ISM and Stellar Birth
Light and The Electromagnetic Spectrum
“The difference between science and magic is that magicians usually know what they're doing.” Ashleigh Brilliant HW2 is on-line now and due next Thursday.
Electromagnetic Spectrum
Earth, Sun Chemistry.
Chapter 6: Electromagnetic Radiation
Atomic Spectra As atoms gain energy their electrons can be excited and absorb energy in discrete amounts called quanta and produce absorption spectrums.
Presentation transcript:

Cloudy: Numerical Simulations of Plasmas and their Spectra If a picture is worth a thousand words, a spectrum is worth a thousand pictures Understanding Starburst Galaxies - Numerical Simulations of Diffuse Interstellar Gas Gary Ferland, Nick Abel, Ryan Porter, Gargi Shaw UK Physics

Cloudy: Numerical Simulations of Plasmas and their Spectra If a picture is worth a thousand words, a spectrum is worth a thousand pictures

Large scale structure

quasars Local structure Cosmic background radiation Primordial nucleosynthesis

Cloudy: Numerical Simulations of Plasmas and their Spectra If a picture is worth a thousand words, a spectrum is worth a thousand pictures

A non-equilibrium gas u Gas emitting spectrum has a very low density u It is exposed to a range of radiation fields and particles u Populations of levels, ionization, spectrum, determined by many micro- physical processes u Not characterized by a single temperature u Or, every level has a different temperature

Photoionization Equilibrium u energetic radiation interacts with surrounding gas –photoionization u photoelectrons heat electron bath u electrons excite heavy elements –collisionally excited line cooling u free electrons recombine –recombination lines

The He-like iso-electronic sequence u He is second most abundant element, produced in Big Bang u A two-electron system, its quantum mechanics is not trivial u Ryan Porter, PhD, in collaboration with Keith MacAdam & Rob Bauman Emission from a pure-helium plasma

Molecular hydrogen u Most baryons are in H 2 u Rotation-vibration emission in IR, electronic absorption in UV u Gargi Shaw, PhD u Energy levels, transition probabilities, well understood u Collisional rates poorly known – being done with ORNL

Heavy-element chemistry u Chemistry in a hard vacuum, at cryogenic temperatures u Series of ion- molecule reactions involving cosmic rays, H 2, and small solids (grains) u Nick Abel, PhD

Cloudy: Numerical Simulations of Plasmas and their Spectra If a picture is worth a thousand words, a spectrum is worth a thousand pictures