The Impact of Dust on a Stellar Wind-Blown Bubbles Ed Churchwell & John Everett University of Wisconsin Oct. 12-15, 2008Lowell Observatory Flagstaff, AZ.

Slides:



Advertisements
Similar presentations
arvard.edu/phot o/2007/m51/. Confronting Stellar Feedback Simulations with Observations of Hot Gas in Elliptical Galaxies Q. Daniel Wang,
Advertisements

Spitzer IRS Spectroscopy of IRAS-Discovered Debris Disks Christine H. Chen (NOAO) IRS Disks Team astro-ph/
Masers and Massive Star Formation Claire Chandler Overview: –Some fundamental questions in massive star formation –Clues from masers –Review of three regions:
H 2 Formation in the Perseus Molecular Cloud: Observations Meet Theory.
Luminous Infrared Galaxies with the Submillimeter Array: Probing the Extremes of Star Formation Chris Wilson (McMaster), Glen Petitpas, Alison Peck, Melanie.
X Y i M82 Blue: Chandra Red: Spitzer Green & Orange: Hubble Face-on i = 0 Edge-on i = 90 Absorption-line probes of the prevalence and properties of outflows.
New Developments in Starburst Modelling: 30 Doradus and NGC 604 as Benchmarks Rafael Martínez-Galarza Leiden Observatory Brent Groves (Leiden/MPIA) Bernhard.
Studying circumstellar envelopes with ALMA
Herschel study of the dust content of Cassiopeia A Ref: arxiv: v1 Oliver Krause PPT.
The Size, Structure & Ionization of the Broad-Line Region in NGC 3227 and NGC 4051 Nick Devereux (ERAU) Emily Heaton (ERAU) May 22 nd, 2013 Naples, Italy.
Multi-band Infrared Mapping of the Galactic Nuclear Region Q. D. Wang (PI), H. Dong, D. Calzetti (Umass), Cotera (SETI), S. Stolovy, M. Muno, J. Mauerhan,
Eddington limited starbursts in the central 10pc of AGN Richard Davies, Reinhard Genzel, Linda Tacconi, Francisco Mueller Sánchez, Susanne Friedrich Max.
Portrait of a Forming Massive Protocluster: NGC6334 I(N) Todd Hunter (NRAO/North American ALMA Science Center) Collaborators: Crystal Brogan (NRAO) Ken.
3-D Simulations of Magnetized Super Bubbles J. M. Stil N. D. Wityk R. Ouyed A. R. Taylor Department of Physics and Astronomy, The University of Calgary,
The Interstellar Medium Astronomy 315 Professor Lee Carkner Lecture 19.
Stars science questions Origin of the Elements Mass Loss, Enrichment High Mass Stars Binary Stars.
Millimeter Spectroscopy Joanna Brown. Why millimeter wavelengths? >1000 interstellar & circumstellar molecular lines Useful for objects at all different.
The Interstellar Medium ( 星際物質 、星際介質 ) Chapter 10.
Constraining TW Hydra Disk Properties Chunhua Qi Harvard-Smithsonian Center for Astrophysics Collaborators : D.J. Wilner, P.T.P. Ho, T.L. Bourke, N. Calvet.
The Interstellar Medium Astronomy 315 Professor Lee Carkner Lecture 19.
Injection of Small Bodies into the ISM by Planetary Nebulae. Bob O’Dell University of Chicago 18 April 2007.
STAR FORMATION STUDIES with the CORNELL-CALTECH ATACAMA TELESCOPE Star Formation/ISM Working Group Paul F. Goldsmith (Cornell) & Neal. J. Evans II (Univ.
A Submillimeter study of the Magellanic Clouds Tetsuhiro Minamidani (Nagoya University) & NANTEN team ASTE team Mopra – ATNF team.
Clicker Question: The HR diagram is a plot of stellar A: mass vs diameter. B: luminosity vs temperature C: mass vs luminosity D: temperature vs diameter.
Jonathan Slavin Harvard-Smithsonian CfA
A Herschel Galactic Plane Survey of [NII] Emission: Preliminary Results Paul F. Goldsmith Umut Yildiz William D. Langer Jorge L. Pineda Jet Propulsion.
Building the Hertzsprung-Russell (H-R) Diagram Use the worksheets passed out in class.
The 511 keV Annihilation Emission From The Galactic Center Department of Physics National Tsing Hua University G.T. Chen 2007/1/2.
ASTR112 The Galaxy Lecture 6 Prof. John Hearnshaw 10. Galactic spiral structure 11. The galactic nucleus and central bulge 11.1 Infrared observations Galactic.
Stellar Winds and Mass Loss Brian Baptista. Summary Observations of mass loss Mass loss parameters for different types of stars Winds colliding with the.
Zhang Ningxiao.  Emission of Tycho from Radio to γ-ray.  The γ-ray is mainly accelerated from hadronic processes.
TURBULENCE AND HEATING OF MOLECULAR CLOUDS IN THE GALACTIC CENTER: Natalie Butterfield (UIowa) Cornelia Lang (UIowa) Betsy Mills (NRAO) Dominic Ludovici.
Astrophysics from Space Lecture 8: Dusty starburst galaxies Prof. Dr. M. Baes (UGent) Prof. Dr. C. Waelkens (KUL) Academic year
Henize 2-10 IC 342 M 83 NGC 253 NGC 6946 COMPARISON OF GAS AND DUST COOLING RATES IN NEARBY GALAXIES E.Bayet : LRA-LERMA-ENS (Paris) IC 10 Antennae.
Fate of comets This “Sun-grazing” comet was observed by the SOHO spacecraft a few hours before it passed just 50,000 km above the Sun's surface. The comet.
Chapter 4: Formation of stars. Insterstellar dust and gas Viewing a galaxy edge-on, you see a dark lane where starlight is being absorbed by dust. An.
The overall systematic trends in the kinematics of massive star forming regions Observations of HC 3 N* in hot cores Víctor M. Rivilla 41st Young European.
Dust Envelopes around Oxygen-rich AGB stars Kyung-Won Suh Dept. of Astronomy & Space Science Chungbuk National University, Korea
Note that the following lectures include animations and PowerPoint effects such as fly-ins and transitions that require you to be in PowerPoint's Slide.
VLASS – Galactic Science Life cycle of star formation in our Galaxy as a proxy for understanding the Local Universe legacy science Infrared GLIMPSE survey.
Detecting Cool Dust in SNRs in LMC and SMC with ALMA Takaya Nozawa (Kavli IPMU) and Masaomi Tanaka (NAOJ) 2012/6/11 Targets ・ SN 1987A: our proposal for.
Direct Physical Diagnostics of Triggered Star Formation Rachel Friesen NRAO Postdoctoral Fellow North American ALMA Science Center C. Brogan, R. Indebetouw,
Science with continuum data ALMA continuum observations: Physical, chemical properties and evolution of dust, SFR, SED, circumstellar discs, accretion.
Studying Young Stellar Objects with the EVLA
The reliability of [CII] as a SFR indicator Ilse De Looze, Suzanne Madden, Vianney Lebouteiller, Diane Cormier, Frédéric Galliano, Aurély Rémy, Maarten.
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.
Determining the Scale Height of FeIII in the Milky Way by Matt Miller UW REU Summer 2009 Advisor: Dr. Bart Wakker.
CLUSTERS OF GALAXIES The Physics of the IGM: Cooling Flows.
Feedback Observations and Simulations of Elliptical Galaxies –Daniel Wang, Shikui Tang, Yu Lu, Houjun Mo (UMASS) –Mordecai Mac-Low (AMNH) –Ryan Joung (Princeton)
Introduction KU-4/2007 The ISM K.D.Kuntz The Henry A. Rowland Department of Physics and Astronomy The Johns Hopkins University (Diffuse Emission in Galaxies)
Chapter 11 The Interstellar Medium
Probing the Birth of Super Star Clusters Kelsey Johnson University of Virginia Hubble Symposium, 2005.
Formation of Dust in Supernovae and Its Ejection into the ISM Takaya Nozawa (IPMU, Univ. of Tokyo) Collaborators; T. Kozasa (Hokkaido Univ.), N. Tominaga.
Recontres de Moriond XXV La Thuile, March 2005 Recontres de Moriond XXV La Thuile, March 2005 Theoretical SEDs in Starbursts: SFRs in both the UV and IR.
Evolution of Newly Formed Dust in Population III Supernova Remnants and Its Impact on the Elemental Composition of Population II.5 Stars Takaya Nozawa.
The Chemistry of PPN T. J. Millar, School of Physics and Astronomy, University of Manchester.
1 Radio – FIR Spectral Energy Distribution of Young Starbursts Hiroyuki Hirashita 1 and L. K. Hunt 2 ( 1 University of Tsukuba, Japan; 2 Firenze, Italy)
Formation and evolution of dust in Type IIb SN: Application to Cas A Takaya Nozawa (IPMU, Univ. of Tokyo) Collaborators; T. Kozasa (Hokkaido Univ.), N.
SOFIA and the ISM of Galaxies Xander Tielens & Jessie Dotson Presented by Eric Becklin.
Properties of the NLR from Spatially Resolved Spectroscopy Nicola Bennert University of California Riverside Collaborators: Bruno Jungwiert, Stefanie Komossa,
KASI Galaxy Evolution Journal Club A Massive Protocluster of Galaxies at a Redshift of z ~ P. L. Capak et al. 2011, Nature, in press (arXive: )
Imaging Dust in Starburst Outflows with GALEX Charles Hoopes Tim Heckman Dave Strickland and the GALEX Science Team March 7, 2005 Galactic Flows: The Galaxy/IGM.
The Ionization Toward The High-Mass Star-Forming Region NGC 6334 I Jorge L. Morales Ortiz 1,2 (Ph.D. Student) C. Ceccarelli 2, D. Lis 3, L. Olmi 1,4, R.
“Globular” Clusters: M15: A globular cluster containing about 1 million (old) stars. distance = 10,000 pc radius  25 pc “turn-off age”  12 billion years.
By: Mike Malatesta Introduction to Open Clusters.
ALMA observations of Molecules in Supernova 1987A
Shohei Ishiki (Hokkaido University),
Consensus and issues on dust formation in supernovae
The Interstellar Medium
Presentation transcript:

The Impact of Dust on a Stellar Wind-Blown Bubbles Ed Churchwell & John Everett University of Wisconsin Oct , 2008Lowell Observatory Flagstaff, AZ

Outline N49-A Stellar Wind-Blown Bubble Dust observed within this wind-blown bubble –MIR/Radio Image –24µm/70µm brightness ratios Modelling the dust: –Dust properties in wind shocks? –How long does dust survive? Importance of grains on bubble properties Summary

N49 4.5(B), 8.0(G), 24(R) µm Image

N49 IR/Radio Image

Image of Wind-Blown Bubbles a la Weaver et al. 1977

Dust models approximately fit the data: 24/70µm Brightness Distributions

Dust Model Properties As a first approximation, we model N49 as a static, uniform- temperature, dusty bubble using Cloudy (Ferland, 1998) and Cloudy_3D (Morisset, 2004). Key parameters for the models are:

Can Dust Survive in the Bubble? Dust Properties in Wind-Blown Bubbles Grain Temperatures Sputtering Timescales Grain Residence times Average Grain Charge Dust Cooling Fraction

Grain Temperatures: Little Sublimation Graphites slightly warmer than the silicates at same radius and grain size Larger grains cooler than smaller grains at same radius and grain size Decrease in temp with radius only ~20-30%

Sputtering: Very Long Timescales Grains not significantly sputtered in hot, post-shocked wind bubble (Sputtering timescales about same for graphite & silicates.)‏

Wind Drag: Driving Small Grains Out Grains with radii < 0.05 µm are driven out of the wind-blown bubble in less than ~10 5 years. This shows that the advection of dust due to wind drag is the most important process for dust longevity.

Grain Charge: Grains Help With Cooling High stellar luminosity & low density drives grains to have significant positive charges over most of parameter space.

Dust Cooling Fraction Dust dominates the cooling until Compton cooling becomes important at large luminosities and small densities.

Issues 24µm emission => Dust exists within HII regions Dust residence timescales are small relative to the age of bubbles =>Why are grains in HII regions? –Need a continuous source of grains Perhaps from embedded neutral condensations? Entrainment of neutral condensations from the PDR of the HII region?

Diagram of a Dusty Wind-Blown Bubble

What can ALMA Contribute? High spatial resolution, sensitive, mm-submm images of bubbles will be important to determine: –the extent of warm dust in HII regions for comparison with cm and 24 µm emission. Probably different dust components dominate at each wavelength. –the total luminosity of the central star(s)‏ –the location of the ionizing stars and measure their mass loss rates High resolution molecular line probes will provide: –the kinematics and structure of associated PDR regions –constrain chemical models of PDRs –temperature and density structure of PDRs Radio recomb lines will: –provide density structure of H+ gas –locate and define the structure of shocks and ionization fronts in HII regions –determine bubble expansion velocities which will Verify that they are what we think they are Provide distance estimates independent of a Galactic rotation model –determine kinematic distances –internal velocity structure of bubbles

Summary Dust Impacts on wind-blown HII regions –Dust is strongly positively charged –Dust dominates cooling –Temperatures lower than in absence of dust –Radii smaller for age and ambient density than expected in absence of dust => age estimates not simply related to size and ambient ISM density –Ionization structure => looks like a cooler central star than the actual star –MIR-FIR brightness much greater than in absence of dust –Theoretically only grains of size ≥ 0.2µm survive long enough to play an important role, however we seem to see grains of all sizes –Kinematic impacts due to dust? Relative dust drift velocities are fairly large

Comparison:[NeII], [NeIII], PAH(11.3µm)‏