Outflows from Clusters of Massive Stars

Slides:



Advertisements
Similar presentations
1 VO Theory Use Cases – Intermediate Scale David De Young Project Scientist US NVO IVOA Theory Interest Group S. Lorenzo del Escorial - 10/05.
Advertisements

arvard.edu/phot o/2007/m51/. Confronting Stellar Feedback Simulations with Observations of Hot Gas in Elliptical Galaxies Q. Daniel Wang,
Methanol maser polarization in W3(OH) Lisa Harvey-Smith Collaborators: Vlemmings, Cohen, Soria-Ruiz Joint Institute for VLBI in Europe.
September 2005 Magnetic field excitation in galaxies.
Chapter 19.
Stellar Birth and Stellar Structure Dense “cold” clouds in the Interstellar Medium, or the ISM 75% hydrogen 25% helium and trace amounts of : carbon, oxygen,
Stellar Structure: TCD 2006: star formation.
Astrophysical Jets Robert Laing (ESO). Galactic black-hole binary system Gamma-ray burst Young stellar object Jets are everywhere.
The spectral resolution of x-ray telescopes has improved many hundred-fold over the past decade, enabling us to detect and resolve emission lines in hot.
Krakow 2010 Galactic magnetic fields: MRI or SN-driven dynamo? Detlef Elstner Oliver Gressel Natali Dziourkevich Alfio Bonanno Günther Rüdiger.
Cosmological MHD Hui Li Collaborators: S. Li, M. Nakamura, S. Diehl, B. Oshea, P. Kronberg, S. Colgate (LANL) H. Xu, M. Norman (UCSD), R. Cen (Princeton)
Estimate* the Total Mechanical Feedback Energy in Massive Clusters Bill Mathews & Fulai Guo University of California, Santa Cruz *~ ±15-20% version 2.
Cosmic Rays Discovery of cosmic rays Local measurements Gamma-ray sky (and radio sky) Origin of cosmic rays.
Stellar Winds and Mass Loss Brian Baptista. Summary Observations of mass loss Mass loss parameters for different types of stars Winds colliding with the.
Quasars and Other Active Galaxies
Star and Planet Formation Sommer term 2007 Henrik Beuther & Sebastian Wolf 16.4 Introduction (H.B. & S.W.) 23.4 Physical processes, heating and cooling.
Zhang Ningxiao.  Emission of Tycho from Radio to γ-ray.  The γ-ray is mainly accelerated from hadronic processes.
Active Galaxy Jets – An exhausting business Diana Worrall University of Bristol.
Superbubble Driven Outflows in Cosmological Galaxy Evolution Ben Keller (McMaster University) James Wadsley, Hugh Couchman CASCA 2015 Paper: astro-ph:
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.
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. Introduction Star-Forming Regions The Formation of Stars Like the Sun Stars of Other Masses Observations of Brown Dwarfs Observations.
Accretion disc dynamos B. von Rekowski, A. Brandenburg, 2004, A&A 420, B. von Rekowski, A. Brandenburg, W. Dobler, A. Shukurov, 2003 A&A 398,
Multidimensional Diffusive Shock Acceleration in Winds from Massive Stars Paul P. Edmon University of Minnesota Collaborators: Tom Jones (U of M), Andrew.
The Origin and Acceleration of Cosmic Rays in Clusters of Galaxies HWANG, Chorng-Yuan 黃崇源 Graduate Institute of Astronomy NCU Taiwan.
Mellinger Lesson 8 Star Formation Toshihiro Handa Dept. of Phys. & Astron., Kagoshima University Kagoshima Univ./ Ehime Univ. Galactic radio astronomy.
Department of Physics and Astronomy Rice University From the Omega facility to the Hubble Space Telescope: Experiments and Observations of Supersonic Fluid.
CARMA Large Area Star-formation SurveY  Completing observations of 5 regions of square arcminutes with 7” angular resolution in the J=1-0 transitions.
The X-ray Universe Sarah Bank Presented July 22, 2004.
A Panoramic HST Infrared View of the Galactic Center Q. D. Wang, H. Dong, D. Calzetti (UMass), A. Cotera (SETI), S. Stolovy, M. Muno, J. Mauerhan, (Caltech/IPAC/JPL),
Rachael Ainsworth Dublin Institute for Advanced Studies YERAC 2011.
Lecture 30: The Milky Way. topics: structure of our Galaxy structure of our Galaxy components of our Galaxy (stars and gas) components of our Galaxy (stars.
Spiral Triggering of Star Formation Ian Bonnell, Clare Dobbs Tom Robitaille, University of St Andrews Jim Pringle IoA, Cambridge.
Quasars and Other Active Galaxies
Feedback Observations and Simulations of Elliptical Galaxies –Daniel Wang, Shikui Tang, Yu Lu, Houjun Mo (UMASS) –Mordecai Mac-Low (AMNH) –Ryan Joung (Princeton)
1 Carlo Nipoti Dipartimento di Astronomia Università di Bologna Thermal evaporation, AGN feedback and quenched star formation in massive galaxies Chandra.
Philamentary Structure and Velocity Gradients in the Orion A Cloud
A Pulsar Wind Nebula Origin for Luminous TeV Source HESS J Joseph Gelfand (NYUAD / CCPP) Eric Gotthelf, Jules Halpern (Columbia University), Dean.
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.
Contra Viento y …Contra Viento y … Un homenaje a Eduardo Delgado Donate, Estallidos 2007.
Evolution of Newly Formed Dust in Population III Supernova Remnants and Its Impact on the Elemental Composition of Population II.5 Stars Takaya Nozawa.
Cornelia C. Lang University of Iowa collaborators:
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)
Stellar NurseriesStages of Star Birth. The interstellar medium The space between the stars is not empty.
ASTR112 The Galaxy Lecture 12 Prof. John Hearnshaw 16. Evolution of the Galaxy 16.1 Star formation 16.2 Exchange of material between stars and ISM 16.3.
Gamma-ray Bursts from Synchrotron Self-Compton Emission Juri Poutanen University of Oulu, Finland Boris Stern AstroSpace Center, Lebedev Phys. Inst., Moscow,
High energy Astrophysics Mat Page Mullard Space Science Lab, UCL 7. Supernova Remnants.
The Physics of Galaxy Formation. Daniel Ceverino (NMSU/Hebrew U.) Anatoly Klypin, Chris Churchill, Glenn Kacprzak (NMSU) Socorro, 2008.
From Cloud to Cluster: A Tale of Orion Steven Stahler Eric Huff.
Arman Khalatyan AIP 2006 GROUP meeting at AIP. Outline What is AGN? –Scales The model –Multiphase ISM in SPH SFR –BH model Self regulated accretion ?!
Qualifying Exam Jonathan Carroll-Nellenback Physics & Astronomy University of Rochester Turbulence in Molecular Clouds.
Cooling, AGN Feedback and Star Formation in Simulated Cool-Core Galaxy Clusters Yuan Li University of Michigan Collaborators: Greg L. Bryan (Columbia)
Reionization of the Universe MinGyu Kim
Towards Realistic Modeling of Massive Star Clusters Oleg Gnedin (University of Michigan) graduate student Hui Li.
Modeling Astrophysical Turbulence
On the origin of Microturbulence in hot stars
Star and Planet Formation. I. The Big Questions
Winds Driven by Massive Star Clusters
Lecture 6 Summary and Perspectives
Fermi Bubble Z.G.,Xiong.
Stellar Winds of Massive Stars Lamers & Cassinelli (1999)
X-ray and Radio Connections
Edison Liang, Koichi Noguchi Orestes Hastings, Rice University
Feedback from Massive Stellar Clusters in Starbursts (Poster 7)
Why only a small fraction of quasars are radio loud?
Hideki Maki Department of Physics, Rikkyo University
The Interstellar Medium
Supernova Nucleosynthesis and Extremely Metal-Poor Stars
Cornelia C. Lang University of Iowa collaborators:
Borislav Nedelchev et al. 2019
Presentation transcript:

Outflows from Clusters of Massive Stars Summary of presentations: Gayley: Thermal vs NT, uniform vs clumpy Beuther: jet mechanism? High vs low mass? Silich: Radiative cooling of winds important Townsley: diffuse vs stellar xray emission Lang: xraydio sources in the GC Arches cluster Law: embedded sources vs external illumination

Outflows from Clusters of Massive Stars 3 types of massive outflows tracing cluster life: Jets from young massive stars Stellar winds from adult O and WR stars SN ejecta with swept up ISM material Focusing on the winds as Xraydio sources: Do CWs always result in both radio and xray? What is the degree of feedback between the two? How does acceleration efficiency affect this? How important is the partitioning of energy (ions vs electrons)?

What’s Important? Investigate roles of: Star formation (single or low mass coalesence, mixture of temperatures) Turbulence (source and dissipation of) Metallicity (effect on winds and cooling) ISM (density, composition, magnetic fields) Magnetic fields (orientation, strength) Radiative cooling (affects scales) Tripod of observation, theory, and simulation seems out of whack: what should the latter two explore?