Lecture 9: Wind-Blown Bubbles September 21, 2011.

Slides:



Advertisements
Similar presentations
X-Ray Emission from Planetary Nebulae and Their Central Stars: A Status Report Joel Kastner Rochester Institute of Technology w/ help from lots of other.
Advertisements

Thermal X-ray in SNR Patrick Slane Zhang Ningxiao.
Supernova Remnants Shell-type versus Crab-like Phases of shell-type SNR.
Feedback: in the form of outflow. AGN driven outflow.
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.
2009 July 8 Supernova Remants and Pulsar Wind Nebulae in the Chandra Era 1 Modeling the Dynamical and Radiative Evolution of a Pulsar Wind Nebula inside.
X-ray Properties of Five Galactic SNRs arXiv: Thomas G. Pannuti et al.
The Nature and Origin of Molecular Knots in Planetary Nebulae Sarah Eyermann – U. of Missouri Angela Speck – U. of Missouri Margaret Meixner – STScI Peter.
Structure of the Local ISM Jeffrey Linsky (University of Colorado) Seth Redfield (University of Texas) Small Ionized and Neutral Structures in the Diffuse.
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,
Mike Crenshaw (Georgia State University) Steve Kraemer (Catholic University of America) Jack Gabel (University of Colorado) NGC 4151 Mass Outflows from.
Einstein Fellows Symposium 10/27/ Orly Gnat, Caltech In Collaboration with : Amiel Sternberg, Chris McKee.
Oct 17, Non-Equilibrium Ionization Orly Gnat (Caltech) with Amiel Sternberg (Tel-Aviv University) Gnat & Sternberg 2007, ApJS, 168, 213 in Post-Shock.
The Interstellar Medium ( 星際物質 、星際介質 ) Chapter 10.
9/7/04Claus Leitherer: A Far-UV View1 Claus Leitherer (STScI) A Far-Ultraviolet View of Starburst Galaxies Claus Leitherer (STScI)
NASA's Chandra Sees Brightest Supernova Ever N. Smith et al. 2007, astro-ph/ v2.
Hot Gas in Planetary Nebulae You-Hua Chu Robert A. Gruendl Martín A. Guerrero Univ. of Illinois.
Andrea Dupree SAO/CfA New England Space Science Consortium (NESSC) March 1, 2006 Some Stellar Problems of Interest to Solar Physics  Global properties.
Jonathan Slavin Harvard-Smithsonian CfA
IAU Symp 34 IAU Symposium 34: Planetary Nebulae Tatranska Lomnica, Czechoslovakia August 1967 C.R. O’Dell High Resolution, High S/N Spectroscopy of PNe.
Interacting Winds: Theory Overview Stan Owocki Bartol Research Institute University of Delaware with thanks for web slides from: D. Folini, K. Gayley,
X-ray Emission from PNe Martín A. Guerrero You-Hua Chu Robert A. Gruendl Univ. of Illinois APN III, Mt Rainier, 7/30/03.
An X-ray Study of the Bright Supernova Remnant G with XMM-Newton SNRs and PWNe in the Chandra Era Boston, MA – July 8 th, 2009 Daniel Castro,
On the velocity structure in clumpy planetary nebulae Café de grano o soluble: Micro-estructuras en nebulosas planetarias Wolfgang Steffen Alberto López.
Stellar Winds and Mass Loss Brian Baptista. Summary Observations of mass loss Mass loss parameters for different types of stars Winds colliding with the.
The Interstellar Medium Chapter 14. Is There Anything Between the Stars? The answer is yes! And that “stuff” forms some of the most beautiful objects.
6 th IRAM 30m Summer School Star formation near and far A. Fuente Observatorio Astronómico Nacional (OAN, Spain) Photon Dominated Regions I. Physical conditions.
Superbubble Driven Outflows in Cosmological Galaxy Evolution Ben Keller (McMaster University) James Wadsley, Hugh Couchman CASCA 2015 Paper: astro-ph:
The ionization structure of the wind in NGC 5548
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.
STUDYING NEBULAE EJECTED FROM MASSIVE STARS WITH HERSCHEL Chloi Vamvatira-Nakou ARC meeting - 11 February 2010 Centre Spatiale de Liège (CSL) (PhD student.
Radio and X-Ray Properties of Magellanic Cloud Supernova Remnants John R. Dickel Univ. of Illinois with: D. Milne. R. Williams, V. McIntyre, J. Lazendic,
Star Formation in our Galaxy Dr Andrew Walsh (James Cook University, Australia) Lecture 1 – Introduction to Star Formation Throughout the Galaxy Lecture.
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.
Molecular Survival in Planetary Nebulae: Seeding the Chemistry of Diffuse Clouds? Jessica L. Dodd Lindsay Zack Nick Woolf Emily Tenenbaum Lucy M. Ziurys.
VLASS – Galactic Science Life cycle of star formation in our Galaxy as a proxy for understanding the Local Universe legacy science Infrared GLIMPSE survey.
Qingkang Li Department of Astronomy Beijing Normal University The Third Workshop of SONG, April, 2010 Disks of Be Stars & Their Pulsations &
Hot gas in galaxy pairs Olga Melnyk. It is known that the dark matter is concentrated in individual haloes of galaxies and is located in the volume of.
Hee-Won Lee ARCSEC and Dept. of Astronomy Sejong University 2010 August 26.
The Milky Way II AST 112. Interstellar Medium The space between stars is not empty! – Filled with the Interstellar Medium (ISM) Star formation is not.
Interstellar Matter and Star Formation in the Magellanic Clouds François Boulanger (IAS) Collaborators: Caroline Bot (SSC), Emilie Habart (IAS), Monica.
The INTERSTELLAR MEDIUM
The Effect of Escaping Galactic Radiation on the Ionization of High-Velocity Clouds Andrew Fox, UW-Madison STScI, 8 th March 2005.
The Interstellar Medium and Star Formation Material between the stars – gas and dust.
Mike Crenshaw (Georgia State University) Steve Kraemer (Catholic University of America) Mass Outflows from AGN in Emission and Absorption NGC 4151.
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.
Warm Absorbers: Are They Disk Outflows? Daniel Proga UNLV.
Hydrodynamical Interpretation of Basic Nebular Structures
Chapter 11 The Interstellar Medium
Radio Galaxies part 4. Apart from the radio the thin accretion disk around the AGN produces optical, UV, X-ray radiation The optical spectrum emitted.
Expected Gamma-Ray Emission of SN 1987A in the Large Magellanic Cloud (d = 50 kpc) E.G.Berezhko 1, L.T. Ksenofontov 1, and H.J.Völk 2 1 Yu.G.Shafer Institute.
ASTR112 The Galaxy Lecture 9 Prof. John Hearnshaw 12. The interstellar medium: gas 12.3 H I clouds (and IS absorption lines) 12.4 Dense molecular clouds.
Cornelia C. Lang University of Iowa collaborators:
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.
Lecture 10: Bubbles and PNe September 26, III. Conduction Layer - Probe the thermal conduction layer High ions produced by thermal collisions O.
High energy Astrophysics Mat Page Mullard Space Science Lab, UCL 7. Supernova Remnants.
Star Formation The stuff between the stars Nebulae Giant molecular clouds Collapse of clouds Protostars Reading
The Physics of Galaxy Formation. Daniel Ceverino (NMSU/Hebrew U.) Anatoly Klypin, Chris Churchill, Glenn Kacprzak (NMSU) Socorro, 2008.
Takashi Hosokawa ( NAOJ ) Daejeon, Korea Shu-ichiro Inutsuka (Kyoto) Hosokawa & Inutsuka, astro-ph/ also see, Hosokawa & Inutsuka,
Where and How Are Massive Stars Formed in Isolation? You-Hua Chu (U of Illinois) In collaboration with: R. Gruendl, R. Chen*, M. Gelman, M. Johnson (Illinois)
1 Instituto Argentino de Radioastronomía, Argentina 2 Facultad de Ciencias Astronómicas y Geofísicas, UNLP, La Plata, Argentina 3 Departamento de Astronomía,
CSI in SNRs You-Hua Chu Inst of Astron and Astroph
The Interstellar Medium and Star Formation
The Interstellar Medium and Star Formation
Galactic Astronomy 銀河物理学特論 I Lecture 1-6: Multi-wavelength properties of galaxies Seminar: Draine et al. 2007, ApJ, 663, 866 Lecture: 2011/11/14.
The Interstellar Medium
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.
From Massive Stars to SNe
Cornelia C. Lang University of Iowa collaborators:
Presentation transcript:

Lecture 9: Wind-Blown Bubbles September 21, 2011

Interstellar & Circumstellar Bubbles fast wind slow wind fast wind km/s km/s km/s M  /yr M  /yr M  /yr    interstellar circumstellar circumstellar bubble nebula bubble O star  LBV  WR (60 M  ) O star  RSG  WR (35 M  ) Low-mass   RG, AGB  planetary neb.

Interstellar Bubble Castor, McCray, Weaver 1975, ApJL Weaver et al. 1977, ApJ

Schematic Bubble Structure Weaver et al. 1977

Variations of Bubble Models Superbubble Model - intermittent SNe averaged over time ~ stellar wind - blown out of galactic plane (Mac Low & McCray 1998) - blown in magnetized medium (Tomisaka 1992) - hot interior enriched with O and Fe (Silich et al. 2001) Circumstellar Bubble Model - ambient medium with density  r -2 - wind velocity and mass loss rate are functions of time - hydrodynamic model (Garcia-Segura et al. 1996) - radiative hydrodynamic model (Freyer et al. 2006) - mass -loading by evaporation/ablation (Pittard et al. 2001) Planetary Nebula model - similar to circumstellar bubbles - stellar radiation is a strong function of time - Schoenberner, Steffen, Warmuth 2006

I. Dense Swept-up Shell - Why aren’t there more interstellar bubbles?

Copyright © by Russell Croman The Bubble Nebula

N11B - Home of LH10

Naze, et al. 2001, AJ, 122, 921 Bubble Size ~ 15 pc Exp Vel ~ km/s Ionized shell (H II) - sound vel ~ 10 km/s - no strong shocks - no large density jump - no limb-brightening Neutral shell (H I) - sound vel ~ 1 km/s - large density jump - limb-brightening - frequently seen

I. Dense Swept-up Shell - Why aren’t there more interstellar bubbles? - clumpy / inhomogeneous ambient ISM Orion Nebula N44F

I. Dense Swept-up Shell - Why aren’t there more interstellar bubbles? - clumpy / inhomogeneous ambient ISM - clumpy circumstellar bubble RCW58 O  RSG  WR LBV Garcia-Segura, Langer, Mac Low 1996 RSG wind Inside an Interstellar Bubble

I. Dense Swept-up Shell - Why aren’t there more interstellar bubbles? - clumpy / inhomogeneous ambient ISM - clumpy circumstellar bubble - observed bubble dynamics does not match that expected from bubble models; e.g., observed kinetic energy is too low Superbubbles - Oey 1996; Kim et al Interstellar Bubbles - Naze et al. 2002

I. Dense Swept-up Shell - Why aren’t there more interstellar bubbles? - clumpy / inhomogeneous ambient ISM - clumpy circumstellar bubble - observed bubble dynamics does not match that expected from bubble models; e.g., observed kinetic energy is too low There are problems. Remember the clumps.

II. Hot Bubble Interior - X-ray emission from bubble interior

Circumstellar Bubble NGC 6888

Chandra X-ray Image of NGC 6888 R: H  G: [O III] B: X-ray Gruendl, Guerrero, Chu 2011, unpublished

S a WR Circumstellar Bubble Red: H  Green: [O III] Blue: X-ray

S a Detailed Look at Its Shell HD * R: H  G: [O III] B: X-ray Chu et al. 2003, ApJ, 599, 1189

[O III] [N II] HH HH X-ray emission starts here  RSG wind

II. Hot Bubble Interior - X-ray emission from bubble interior - Why aren’t more bubbles detected in X-rays? NGC 6888 (Chandra) S 308 (XMM) 1  10 6 K2-3  10 6 K

II. Hot Bubble Interior - X-ray emission from bubble interior - Why aren’t more bubbles detected in X-rays? If T ~ 1  10 6 K, interstellar absorption killls the others. If T ~ 2-3  10 6 K, RCW58 and NGC may be detectable, but are not.

Hot Gas in the Orion Nebula T ~ 2  10 6 K Lx ~ 5.5  erg/s

Hot Gas in the Omega Superbubble Two young superbubbles are detected in X-rays by Chandra: Omega and (Rosette) ROSAT - Dunne et al. 2003, ApJ, 590, 306 Chandra - Townsley et al. 2003, ApJ, 593, 874

X-ray Observations of Bubbles Detection of hot gas associated with fast winds - 10 PNe, 2 WR bubbles, 2 superbubbles* Properties of the hot gas: T e [10 6 K ] N e [cm -3 ] L X [erg/s] PN 1-3   WR 1-2   M17 7  Orion 2   (* Townsley et al. 2003; Guedel et al. 2007)

II. Hot Bubble Interior - X-ray emission from bubble interior is soft - ISM absorbs soft X-ray emission - X-ray emission depends on: wind properties concentration of massive stars clumpy structure of the ambient medium magnetic fields

III. Conduction Layer - Probe the thermal conduction layer High ions produced by thermal collisions O VI N V C IV Si IV

UV Probes of the 10 5 K Gas C IV N V O VI  Å )  1548, , , 1037 Obs. HST STIS HST STIS FUSE I.P. (eV) T (K) 1.0    10 5 T eff (K) >35,000 >75,000 >125,000

Interface of the WR Bubble S308 C IV Boroson et al. 1997, ApJ, 478, 638 N V S II

S ideal for conduction study HD * R: H  G: [O III] B: X-ray Boroson et al. (1997) detected N V absorption from the conduction layer. HST STIS observation of N V and C VI emission was scheduled, but STIS died. FUSE observations of O VI were awarded, and it died, too. Spitzer can observe Ne V, but it ran out cryogen.

FUSE Observations of NGC 6543 Gruendl, Chu, Guerrero 2004, ApJL

III. Conduction Layer - Probe the thermal conduction layer High ions produced by thermal collisions - NGC 6543: given the boundary conditions of hot interior and warm shell, thermal conduction appears to be consistent, but does not explain the low X-ray luminosity.

Pressure-driven bubble with heat conduction at interface Bubble dynamics does not match L x (obs) / L x (expected) = to  Adjust fast wind - wind velocity - mass loss rate  Reduce heat conduction Dynamically mix nebular material (mass-loading)  

What Next? Swept-up Shell Reasonably well understood Interface (conduction) layer Spatially-resolved high-dispersion UV spectra are needed Hot interior Spatially-resolved high-resolution X-ray spectra are needed