Circumstellar Chemistry: The Effects of High Density Shells on the Distribution of Molecules in IRC+10216 Joanna Brown.

Slides:



Advertisements
Similar presentations
Sakurai’s Object Dr H F Chau Department of Physics HKU Dr H F Chau Department of Physics HKU A Case Of Superfast Stellar Evolution.
Advertisements

The Standard Solar Model and Its Evolution Marc Pinsonneault Ohio State University Collaborators: Larry Capuder Scott Gaudi.
UV Ceti Stars Jessica Windschitl Atmospheres Spring 2007.
Jeong-Eun Lee Kyung Hee University University of Texas at Austin.
The Independency of Stellar Mass-Loss Rates on Stellar X-ray Luminosity and Activity Space Telescope Science Institute – 2012.
– HCO + very abundant in molecular clouds – It’s detection in circumstellar envelopes has been elusive – Models of oxygen-rich circumstellar envelopes.
The 69 th International Symposium on Molecular Spectroscopy June 19, 2014 Comparative Chemistry of Planetary Nebulae: Jessica L. Edwards Lucy M. Ziurys.
Chemical evolution of Super-AGB stars The Giant Branches Lorentz Center, May 2009 Enrique García-Berro 1,2 1 Universitat Politècnica de Catalunya 2 Institut.
Branchings, neutron sources and poisons: evidence for stellar nucleosynthesis Maria Lugaro Astronomical Institute University of Utrecht (NL)
From the AGB to the PN phase with the PdBI From the AGB to the PN phase with the Plateau de Bure Interferometer Arancha Castro- Carrizo Jan Martin Winters.
CPD : the dust chemistry – binarity connection Orsola De Marco American Museum of Natural History New York.
Post Main Sequence Evolution PHYS390 (Astrophysics) Professor Lee Carkner Lecture 15.
Lecture 15PHYS1005 – 2003/4 Lecture 16: Stellar Structure and Evolution – I Objectives: Understand energy transport in stars Examine their internal structure.
Structure of circumstellar envelope around AGB and post-AGB stars Dinh-V-Trung Sun Kwok, P.J. Chiu, M.Y. Wang, S. Muller, A. Lo, N. Hirano, M. Mariappan,
Globules in Planetary Nebulae Review of some recent advances on the nature and origin of globules P. J. Huggins (NYU)
Hydrostatic Equilibrium Physical Astronomy Professor Lee Carkner Lecture 9.
Chemical and Physical Structures of Massive Star Forming Regions Hideko Nomura, Tom Millar (UMIST) ABSTRUCT We have made self-consistent models of the.
Stellar Winds and Mass Loss Brian Baptista. Summary Observations of mass loss Mass loss parameters for different types of stars Winds colliding with the.
1 Hydrophobic hydration at the level of primitive models Milan Predota, Ivo Nezbeda, and Peter T. Cummings Department of Chemical Engineering, University.
The Death of a Low Mass Star n Evolution of a sun-like star post helium- flash –The star moves onto the horizontal branch of the Hertzprung-Russell diagram.
Class 6 : Powering the stars Internal structure of main sequence stars Thermonuclear fusion of H  He The proton-proton chain The CNO cycle The main sequence.
Space Environment Neutral Environment Hydrogen
Near-IR Spectroscopy of Simple Organic Molecules in GV Tau N Dr. Erika Gibb June 19, 2014.
AtmospheresAtmospheres of Brown Dwarfs. Institute of Physics, Croatia mentor: dr Goran Pichler Ana Bedalov University of Zagreb.
Presolar grains and AGB stars Maria Lugaro Sterrenkundig Instituut University of Utrecht.
What is the Sun like? Chapter The Sun is the largest object in the solar system The Sun is the largest object in the solar system It’s diameter.
Lecture 17 Post-ms evolution II. Review Review Review.
Molecular Survival in Planetary Nebulae: Seeding the Chemistry of Diffuse Clouds? Jessica L. Dodd Lindsay Zack Nick Woolf Emily Tenenbaum Lucy M. Ziurys.
A Study of HCO + and CS in Planetary Nebulae Jessica L. Edwards Lucy M. Ziurys Nick J. Woolf The University of Arizona Departments of Chemistry and Astronomy.
14 N/ 15 N ratios in AGB C-stars and the origin of SiC grains Eurogenesis- Perugia Workshop, Nov 12-14, 2012 C. Abia R. Hedrosa (Granada) B. Plez (Montpellier)
The Sun.
Revised Term Values for the A – X (v′=0-9, v′′=0) Bands in 13 C 16 O from High- Resolution Spectra Acquired at the SOLEIL Synchrotron L. Gavilan, J.L.
Yields from single AGB stars Amanda Karakas Research School of Astronomy & Astrophysics Mt Stromlo Observatory.
June 21, th International Symposium on Molecular Spectroscopy Detection of FeCN (X 4  i ) in the Circumstellar Envelope of IRC Lindsay N.
Interstellar Chemical Models with Molecular Anions Eric Herbst, OSU T. Millar, M. Cordiner, C. Walsh Queen’s Univ. Belfast R. Ni Chiumin, U. Manchester.
Our Sun & Nuclear Fusion (Chapter 7). Student Learning Objectives Compare properties of the Earth and Sun Describe the layers of the Sun and how energy.
The AU Mic Debris Ring Density profiles & Dust Dynamics J.-C. Augereau & H. Beust Grenoble Observatory (LAOG)
Classical Novae on a Helium White Dwarf Irit Idan (Technion) Lars Bildsten ((KITP, UCSB) Ken Shen (UCSB)
64th International Symposium on Molecular Spectroscopy June 22 – 26, 2009 Millimeter Detection of AlO (X 2 Σ + ): Metal Oxide Chemistry in the Envelope.
Progenitor stars of supernovae Poonam Chandra Royal Military College of Canada.
ISM & Astrochemistry Lecture 6. Stellar Evolution.
6 - Stellar Evolution-I. The life history of a star is determined by its mass…..
70 th International Symposium on Molecular Spectroscopy June 2015 First Scientific Observations with the New ALMA Prototype Antenna of the Arizona Radio.
Chapter 3 Molecules, Compounds, & Chemical Equations CHE 123: General Chemistry I Dr. Jerome Williams, Ph.D. Saint Leo University.
Astrochemistry University of Helsinki, December 2006 Lecture 4 T J Millar, School of Mathematics and Physics Queen’s University Belfast,Belfast BT7 1NN,
The Chemistry of PPN T. J. Millar, School of Physics and Astronomy, University of Manchester.
Lecture 16 Post-ms evolution. Overview: evolution.
Theoretical Studies of Electronic Spectra and Bonding in AlCl/AlF Jeff Leiding, D. E. Woon and T. H. Dunning, Jr. University of Illinois at Urbana-Champaign.
ERIC HERBST DEPARTMENTS OF PHYSICS AND ASTRONOMY THE OHIO STATE UNIVERSITY The Production of Complex Molecules in Interstellar and Circumstellar Sources.
Oscillator Strengths for Rydberg Transitions in CO between 925 and 956 Å S.R. Federman, Y. Sheffer (Univ. of Toledo) M. Eidelsberg, J.L. Lemaire, J.H.
Dept. of Chemistry University of Arizona A. Janczyk L. M. Ziurys The Millimeter/Submillimeter Spectrum of AlSH (X 1 A) : Further Investigation of the Metal.
ISM & Astrochemistry Lecture 1. Interstellar Matter Comprises Gas and Dust Dust absorbs and scatters (extinguishes) starlight Top row – optical images.
65th International Symposium on Molecular Spectroscopy June 21 – 25, 2010 Exotic Metal Molecules In Oxygen-Rich Envelopes: Detection of AlOH(X 1 Σ + )
ERIC HERBST DEPARTMENTS OF PHYSICS AND ASTRONOMY THE OHIO STATE UNIVERSITY Chemistry in Protoplanetary Disks.
Naomi Pequette. 1.Core Hydrogen Burning 2.Shell Hydrogen Burning 3.First Dredge Up 4.The Bump in the Luminosity Function 5.Core Helium Flash 6.Core Helium.
The Adventures of a Thermally Pulsating AGB Star
Multiphase Porous Media Transport in Apple Tissue During Drying
Our Sun & Nuclear Fusion
From Birth to Death (Dust to Dust)
Stoichiometry.
Stellar Evolution Chapter 19.
الاحتراق.
Multi-transition VLBA observations of circumstellar SiO masers
New Trends of Physics 2005, Hokkaido University, March 1
Our Sun & Nuclear Fusion
MASS RELATIONSHIPS IN CHEMICAL REACTIONS.
Unit 5 STOICHIOMETRY.
Our Star.
Stellar Evolution In post-Main-Sequence evolution, what you see on the surface is not a good indicator of what is happening deep in the interior.
Presentation transcript:

Circumstellar Chemistry: The Effects of High Density Shells on the Distribution of Molecules in IRC Joanna Brown

CW Leo: IRC Part of Asymptotic Giant Branch

Why is CW Leo chemically interesting? During helium flashes, convection zones form which bring C & O from the core to the surface. The C & O is then pushed outwards in the star’s wind

Rings around CW Leo From Mauron & Huggins (1999). Astron. Astrophys. 349, 204.

How does the model work? UV light Abundances of molecules Experimental and theoretical rates of reaction Differential rate equations Parent abundances

Effects of density rings on distribution No enhanced density shells Density enhancement of 6 times normal 1/r 2 distribution With shells at positions in agreement with observations Mass loss of 3.0E-5 M  /yr

Observational agreement From Guélin et al. (2000). IAU Symposium, 197, 369. Actual distribution in IRC using 3mm lines

Conclusions Density shells have a significant effect on chemical abundances and need included in the models Peak abundances are aligned in agreement with observations High abundance range is narrower than previous models in agreement with observations

Acknowledgments Dr. Tom Millar for providing such an interesting project and supervising my research Dr. David Cohen for advising on my thesis and this presentation My family for their support

Feedback: Privacy Policy Feedback
Do Not Sell My Personal Information
About project: SlidePlayer Terms of Service

© 2024 SlidePlayer.com Inc. All rights reserved.