Enrique Vázquez-Semadeni. Centro de Radioastronomía y Astrofísica, UNAM, México
|
|
- Gladys Ramsey
- 6 years ago
- Views:
Transcription
1 Enrique Vázquez-Semadeni Centro de Radioastronomía y Astrofísica, UNAM, México 1
2 Javier Ballesteros-Paredes Centro de Radioastronomía y Astrofísica, UNAM, México 2
3 Collaborators: Javier Ballesteros-Paredes Pedro Colín Gilberto Gómez Alan Watson Robi Banerjee Ralf Klessen STUDENTS: Manuel Zamora Avilés 3
4 Collaborators: Enrique Vázquez-Semadeni Pedro Colín Gilberto Gómez Alan Watson Robi Banerjee Ralf Klessen STUDENTS: Manuel Zamora Avilés 4
5 I. INTRODUCTION Within the turbulent model of molecular clouds and star formation (SF), there exist two alternative scenarios: Slow star formation (Norman & Silk 1980; Krumholz & McKee 2005; Li & Nakamura 2006; Krumholz & Tan 2007): Clouds are in near virial equilibrium, and last several times their free-fall time. Turbulence supports the clouds. Turbulence is replenished by stellar feedback. Turbulence maintains a low star formation rate (SFR). Rapid star formation (Ballesteros-Paredes et al. 1999; Elmegreen 2000; Klessen et al. 2000; Hartmann et al. 2001; Mac Low & Klessen 2004; VS et al. 2007, ): Clouds form by large-scale compressions and/or instabilities. SF occurs rapidly (at high SFR) and coherently. Stellar feedback disrupts the cloud and terminates SF. 5
6 Defining the star formation efficiency as where then: Slow SF large Δt, small SFR. Rapid SF short Δt, large SFR. 6
7 This work: Numerically investigate effect of massive-star feedback on parent cloud immersed in diffuse (WNM) medium: See Manuel Zamora s poster (this session) for approach to an analytical model. Cloud formed by transonic compression in WNM. Compression triggers phase transition to cold medium (Hennebelle & Pérault 1999). Cloud grows by incorporating material from WNM; Bounded by phase transition front. Able to freely interact with WNM environment. Accrete, return material; Disperse? Subject to ionization heating-like stellar feedback. 7
8 Numerical model: N-body + AMR hydrodynamics code (ART code, by Kravtsov et al. 1997; Kravtsov 2003). 256-pc box. 4 refinement levels. Equivalent resolution pc resolution. Stellar particle formation by density threshold criterion. n SF = 4 x 10 6 cm -3. M part ~ 120 M sun. Cooling function from Koyama & Inutsuka (2002). Vázquez-Semadeni et al
9 Numerical model (cont d): Initial velocity field consisting of oppositely-directed cylindrical streams with velocity 6 km s -1 (Mach # = M s,inf =0.8) in WNM. Superposed initial, low-amplitude turbulent velocity field of Mach # M s,rms to trigger instabilities in compressed layer. Scale: ~ cylinder radius. M s,inf : Mach number of inflow speed w.r.t. warm gas. Converging inflow setup M s,rms M s,rms : Mach number of background turbulence in WNM. M inf M s,inf L box M inf : Mass in colliding cylinders = 2 ρ π R inf 2 L inf R inf n WNM = 1 cm -3 L inflow T WNM = 5000 K c s = 7.4 km s -1 9
10 Four simulations: 10
11 Numerical model (cont d) OB-star ionization-like heating by stellar particles: Deposited in cell containing stellar particle during 10 Myr. Heating rate taken as free parameter, adjusted to achieve realistic HII regions: Density Temperature Velocity 11
12 Run LAF1 (Large-amplitude fluctuations with feedback) 12
13 Global cloud features and evolution: Clouds first appear as atomic, CNM structures (Vázquez- Semadeni et al. 2006). Gravitational contraction sets in globally, bringing column density up to molecular-cloud values (Vázquez-Semadeni et al. 2007, Heitsch & Hartmann 2008). Size and mass of clouds determined by scale of dominant compression mechanism: SA simulations: collapse of massive, pancake-shaped cloud of radius = R cyl. Clouds shaped by colliding inflows. LA simulations: collapse of amorphous, less massive, smaller clouds. Clouds shaped by turbulent fluctuations. 13
14 14
15 20-pc measuring box Central Cloud in run SAF1 (small fluctuation amplitude with feedback). 15
16 20-pc measuring box Cloud 1 in run LAF1 (Large fluctuation amplitude with feedback). 16
17 20-pc measuring box Cloud 2 in run LAF1 (Large fluctuation amplitude with feedback). 17
18 Central Cloud, SA No feedback With feedback M(n>100 cm -3 ) [M sun ] Whole box 10-pc box M star [M sun ] 18
19 M(n>100 cm -3 ) [M sun ] No feedback Cloud 1, LA Whole box 30-pc box 20-pc box 10-pc box With feedback M star [M sun ] 19
20 Cloud 2, LA No feedback With feedback M(n>100 cm -3 ) [M sun ] Whole box 30-pc box 20-pc box 10-pc box M star [M sun ] 20
21 Suggests that, for massive clouds, Total mass (cloud + stars) mainly determined by accretion, consistent with Fuikui et al. (2009). SF inhibited by feedback. i.e, larger dense gas mass in case with feedback due to reduced rate of gas-to-stars conversion. Apparently due to focusing of feedback on gas closest to forming stars next. 21
22 3. SFE is reduced to realistic values SA, Central cloud (10-pc box) No feedback Feedback 22
23 No feedback LA runs With feedback Cloud 1 Cloud 1 stellar mass smaller in the presence of feedback. Cloud 2 Cloud 2 23
24 4. Factor by which SFE is reduced by feedback depends on the cloud mass (at roughly the same size) involved in coherent collapse. Apparently due to short-range effect of feedback vs. longrange nature of gravity. The more extended the infall motions, the less effective the feedback in disrupting them. 24
25 5. SFE correlates with SFR. Average low-mass cloud of Evans et al Orion A cloud 25
26 Caveats: 1. Only one kind of feedback star (~ early B star). Excessive for small clouds, weak for massive ones. May be have non-negligible role in dispersal of small clouds, permanence of large ones. Work in progress: consideration of a range of feedback-star masses. 2. No radiative transfer; just heat dumping. 3. No supernova-like feedback. May give the fatal blow to large clouds. 4. Large ambiguity in masses when one is not restricted to a certain tracer. 26
27 27
28 Conclusions (cont d): 3. Turbulence does not seem to be able to hold up a large cloud: Initial turbulence (from cloud assembly) dissipates quickly. Stellar feedback seems too localized. Supersonic turbulent linewidths are indicative of global contraction. (Hartmann & Burkert 2007; Field et al. 2008; Vázquez- Semadeni et al. 2008; Heitsch et al. 2009). 28
Enrique Vázquez-Semadeni. Centro de Radioastronomía y Astrofísica, UNAM, México
Enrique Vázquez-Semadeni Centro de Radioastronomía y Astrofísica, UNAM, México 1 Collaborators: CRyA UNAM: Abroad: Javier Ballesteros-Paredes Pedro Colín Gilberto Gómez Recent PhDs: Alejandro González
More informationEnrique Vázquez-Semadeni. Instituto de Radioastronomía y Astrofísica, UNAM, México
Enrique Vázquez-Semadeni Instituto de Radioastronomía y Astrofísica, UNAM, México 1 Collaborators: CRyA UNAM: Javier Ballesteros-Paredes Pedro Colín Gilberto Gómez Manuel Zamora-Avilés Abroad: Robi Banerjee
More informationGravity or Turbulence?
Gravity or Turbulence? On the dynamics of Molecular Clouds Javier Ballesteros-Paredes On Sabbatical at Institut für Theoretische Astrophysik, University of Heidelberg Instituto de Radioastronomía y Astrofísica,
More informationMOLECULAR CLOUD EVOLUTION. II. FROM CLOUD FORMATION TO THE EARLY STAGES OF STAR FORMATION IN DECAYING CONDITIONS
The Astrophysical Journal, 657:870 883, 2007 March 10 # 2007. The American Astronomical Society. All rights reserved. Printed in U.S.A. A MOLECULAR CLOUD EVOLUTION. II. FROM CLOUD FORMATION TO THE EARLY
More informationTurbulence, kinematics & galaxy structure in star formation in dwarfs. Mordecai-Mark Mac Low Department of Astrophysics
Turbulence, kinematics & galaxy structure in star formation in dwarfs Mordecai-Mark Mac Low Department of Astrophysics Outline Turbulence inhibits star formation, but slowly Interplay between turbulence
More informationMolecular Cloud Turbulence and Star Formation
Molecular Cloud Turbulence and Star Formation Javier Ballesteros-Paredes1, Ralf Klessen2, MordecaiMark Mac Low3, Enrique Vazquez-Semadeni1 1UNAM Morelia, Mexico, 2AIP, Potsdam, Germany, 3AMNH New York,
More informationGravity or turbulence? II. Evolving column density probability distribution functions in molecular clouds
Mon. Not. R. Astron. Soc. 416, 1436 1442 (2011) doi:10.1111/j.1365-2966.2011.19141.x Gravity or turbulence? II. Evolving column density probability distribution functions in molecular clouds Javier Ballesteros-Paredes,
More informationThe Effects of Radiative Transfer on Low-Mass Star Formation
The Effects of Radiative Transfer on Low-Mass Star Formation Stella Offner NSF Fellow, ITC Dense Cores in Dark Clouds Oct 23 2009 Collaborators: Chris McKee (UC Berkeley), Richard Klein (UC Berkeley; LLNL),
More informationModelling star formation in galaxy formation simulations
Modelling star formation in galaxy formation simulations Vadim Semenov (U.Chicago) Andrey Kravtsov University of Chicago Carving through the codes Davos, Switzerland 16 February, 2017 Nick Gnedin (Fermilab)
More informationFrom Filaments to Stars: a Theoretical Perspective
From Filaments to Stars: a Theoretical Perspective NRAO Filaments. Oct. 10-11, 2014 Ralph E. Pudritz Origins Institute, McMaster U. Collaborators McMaster: Mikhail Klassen, Corey Howard, (Ph.D.s) Helen
More informationarxiv:astro-ph/ v1 26 Sep 2003
Star Formation at High Angular Resolution ASP Conference Series, Vol. S-221, 2003 M.G. Burton, R. Jayawardhana & T.L. Bourke The Turbulent Star Formation Model. Outline and Tests arxiv:astro-ph/0309717v1
More informationThe nature of the velocity field in molecular clouds I. The non-magnetic case
Mon. Not. R. Astron. Soc. 390, 769 780 (2008) doi:10.1111/j.1365-2966.2008.13778.x The nature of the velocity field in molecular clouds I. The non-magnetic case Enrique Vázquez-Semadeni, 1 Ricardo F. González,
More informationThe Formation of Star Clusters
The Formation of Star Clusters Orion Nebula Cluster (JHK) - McCaughrean Jonathan Tan University of Florida & KITP In collaboration with: Brent Buckalew (ERAU), Michael Butler (UF u-grad), Jayce Dowell
More informationarxiv: v1 [astro-ph.ga] 25 Apr 2012
Mon. Not. R. Astron. Soc. 000, 000 000 (0000) Printed 26 April 2012 (MN LATEX style file v2.2) arxiv:1204.5570v1 [astro-ph.ga] 25 Apr 2012 How long does it take to form a molecular cloud? Paul C. Clark
More informationShocks, cooling and the origin of star formation rates in spiral galaxies
MNRAS 430, 1790 1800 (2013) doi:10.1093/mnras/stt004 Shocks, cooling and the origin of star formation rates in spiral galaxies Ian A. Bonnell, 1 Clare L. Dobbs 2 and Rowan J. Smith 3 1 Scottish Universities
More informationThe Fragmentation of expanding shells. Kazunari Iwasaki (Nagoya Univ.) Collaborate with S. Inutsuka (Nagoya Univ.) T. Tsuribe (Osaka Univ.
.... The Fragmentation of expanding shells Kazunari Iwasaki (Nagoya Univ.) Collaborate with S. Inutsuka (Nagoya Univ.) T. Tsuribe (Osaka Univ.) 1 / 23 Outline Introduction Three Dimensional SPH Simulations
More informationGalaxy Simulators Star Formation for Dummies ^
Galaxy Simulators Star Formation for Dummies ^ Mark Krumholz UC Santa Cruz HIPACC Summer School August 6, 2010 The Challenge of Star Formation ~10 pc ~10 pc ~10 pc Like stars, star formation involves impossibly
More informationFrédérique Motte and Nicola Schneider (AIM Paris-Saclay, Obs. Bordeaux) Coordinated by Frédérique Motte, Annie Zavagno, and Sylvain Bontemps
Cloud structure and high-mass star formation in HOBYS, the Herschel imaging survey of OB Young Stellar objects Frédérique Motte and Nicola Schneider (AIM Paris-Saclay, Obs. Bordeaux) http://hobys-herschel.cea.fr
More informationTidal forces as a regulator of star formation in Taurus
Mon. Not. R. Astron. Soc. 000, 1 5 (2006) Printed 13 March 2009 (MN LATEX style file v2.2) Tidal forces as a regulator of star formation in Taurus Javier Ballesteros-Paredes 1, Gilberto C. Gómez 1, Laurent
More informationAn overview of star formation
An overview of star formation Paul Clark ITA: Ralf Klessen Robi Banerjee Simon Glover Ian Bonnell Clare Dobbs Jim Dale Why study star formation? Stars chemically the enrich the Universe, so star formation
More informationARE THERE PHASES IN THE ISM?
The Role of Disk-Halo Interaction in Galaxy Evolution: Outflow vs Infall? Editor EAS Publications Series, Vol.?, 2009 ARE THERE PHASES IN THE ISM? Enrique Vázquez-Semadeni 1 Abstract. The interstellar
More informationCollapse of Massive Cloud Cores
Collapse of Massive Cloud Cores Robi Banerjee ITA, University of Heidelberg Based on 3D MHD, AMR* Simulations * Adaptive Mesh Refinement Collapse of Hydrostatic Cores Cloud formation by TI Slowly rotating
More informationSFEs in clusters. Final value of the SFE. For an isolated clump SFE exp. (t exp. = SFE(t exp. M ( cluster. t ) exp M clump. (t) M gas,i.
SFEs in clusters SFE(t) Final value of the SFE M cluster (t) M gas,i + M gas,acc (t) SFE exp = SFE(t exp ) M cluster (t exp ) M gas,i + M gas,acc ( t ) exp For an isolated clump SFE exp M ( cluster t )
More informationSAM GEEN (ITA/ZAH HEIDELBERG)
SAM GEEN (ITA/ZAH HEIDELBERG) WITH PATRICK HENNEBELLE JUAN SOLER AND RALF KLESSEN Credit: Lost Valley Observatory Star formation is self regulating HII HII regions, regions, supernovae supernovae Molecular
More informationImpact of magnetic fields on molecular cloud formation and evolution
MNRAS 51, 33 3353 (15) doi:1.193/mnras/stv1 Impact of magnetic fields on molecular cloud formation and evolution Bastian Körtgen and Robi Banerjee Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg
More informationThe dependence of star cluster formation on initial conditions. Matthew Bate University of Exeter
The dependence of star cluster formation on initial conditions Matthew Bate University of Exeter Stellar properties do not greatly depend on initial conditions constellation Little evidence for variation
More informationTHE FORMATION OF MASSIVE STARS. η Carina (NASA, ESA, N. Smith)
THE FORMATION OF MASSIVE STARS η Carina (NASA, ESA, N. Smith) THE FORMATION OF MASSIVE STARS Christopher F. McKee Institute for Astronomy November 2, 2011 with Andrew Cunningham Edith Falgarone Richard
More informationTheoretical ideas About Galaxy Wide Star Formation! Star Formation Efficiency!
Theoretical ideas About Galaxy Wide Star Formation Theoretical predictions are that galaxy formation is most efficient near a mass of 10 12 M based on analyses of supernova feedback and gas cooling times
More information! what determines the initial mass function of stars (IMF)? dn /dm
! what determines the initial mass function of stars (IMF)? dn /dm M ! what determines the initial mass function of stars (IMF)?! What determines the total mass of stars that can form in the cloud? dn
More informationThe Magic Scale of Galaxy Formation: SNe & Hot CGM --> Compaction & BHs
The Magic Scale of Galaxy Formation: SNe & Hot CGM --> Compaction & BHs Avishai Dekel The Hebrew University of Jerusalem & UCSC Silk 75, December 2017 A Characteristic Mass for Galaxy Formation Efficiency
More informationMolecular Cloud Support, Turbulence, and Star Formation in the Magnetic Field Paradigm
Molecular Cloud Support, Turbulence, and Star Formation in the Magnetic Field Paradigm Shantanu Basu The University of Western Ontario Collaborators: Glenn Ciolek (RPI), Takahiro Kudoh (NAOJ), Wolf Dapp,
More informationMassive Star Formation with RT-MHD Simulations
Massive Star Formation with RT-MHD Simulations Robi Banerjee Hamburg University Collaborators: Thomas Peters (Zurich), Daniel Seifried (Hamburg), Philipp Girichidis (MPA), Roberto Galvan-Madrid (UNAM,
More informationFundamental Issues in Star Formation
Fundamental Issues in Star Formation - Formation and statistical properties of dense molecular cloud cores (mass function of cores, scaling relations, gravitational boundedness, rotational properties)
More informationarxiv:astro-ph/ v1 17 May 2006
Draft version February 5, 2008 Preprint typeset using L A TEX style emulateapj v. 02/09/03 THE BIRTH OF MOLECULAR CLOUDS: FORMATION OF ATOMIC PRECURSORS IN COLLIDING FLOWS Fabian Heitsch 1,2,3, Adrianne
More informationTurbulence simulations with ENZO and FLASH3
Turbulence simulations with ENZO and FLASH3... not yet Adaptive-mesh simulations with FLASH Christoph Federrath Institute for Theoretical Astrophysics Heidelberg Collaborators: Ralf Klessen, Robi Banerjee,
More informationSvitlana Zhukovska Max Planck Institute for Astrophysics
Unveiling dust properties across galactic environments with dust evolution models Svitlana Zhukovska Max Planck Institute for Astrophysics Clare Dobbs (Uni Exeter), Ed Jenkins (Princeton Uni) Ralf Klessen
More informationStar Cluster Formation
Star Cluster Formation HST Colin Hill Princeton Astrophysics 4 December 2012 Trapezium VLT Outline Star Clusters: Background + Observations The Life of a Cluster - Fragmentation - Feedback Effects - Mass
More informationRevista Mexicana de Astronomía y Astrofísica ISSN: Instituto de Astronomía México
Revista Mexicana de Astronomía y Astrofísica ISSN: 0185-1101 rmaa@astroscu.unam.mx Instituto de Astronomía México Klessen, Ralf S. Star Formation from Gravoturbulent Fragmentation Revista Mexicana de Astronomía
More informationCollapse of magnetized dense cores. Is there a fragmentation crisis?
Collapse of magnetized dense cores Is there a fragmentation crisis? Patrick Hennebelle (ENS-Observatoire de Paris) Collaborators: Benoît Commerçon, Andréa Ciardi, Sébastien Fromang, Romain Teyssier, Philippe
More informationHow do protostars get their mass?
How do protostars get their mass? Phil Myers Harvard-Smithsonian Center for Astrophysics Origin of Stellar Masses Tenerife, Spain October 18, 2010 Introduction How does nature make a star? a star of particular
More informationBimodal regime in young massive clusters leading to formation of subsequent stellar generations
Bimodal regime in young massive clusters leading to formation of subsequent stellar generations Richard Wünsch J. Palouš, G. Tenorio-Tagle, C. Muñoz-Tuñón, S. Ehlerová Astronomical institute, Czech Academy
More informationSTAR FORMATION RATES observational overview. Ulrike Kuchner
STAR FORMATION RATES observational overview Ulrike Kuchner Remember, remember.. Outline! measurements of SFRs: - techniques to see what the SF rate is - importance of massive stars and HII regions - the
More informationViolent Disk Instability at z=1-4 Outflows; Clump Evolution; Compact Spheroids
Violent Disk Instability at z=1-4 Outflows; Clump Evolution; Compact Spheroids Avishai Dekel The Hebrew University of Jerusalem Santa Cruz, August 2013 stars 5 kpc Outline 1. Inflows and Outflows 2. Evolution
More informationarxiv: v3 [astro-ph.sr] 30 Nov 2016
Draft version November 12, 2018 Preprint typeset using A TEX style emulateapj v. 5/2/11 OSCIATING FIAMENTS: I - OSCIATION AND GEOMETRICA FRAGMENTATION Matthias Gritschneder 1, Stefan Heigl 1, Andreas Burkert
More informationIonization Feedback in Massive Star Formation
Ionization Feedback in Massive Star Formation Thomas Peters Institut für Theoretische Astrophysik Zentrum für Astronomie der Universität Heidelberg Ralf Klessen, Robi Banerjee (ITA, Heidelberg) Mordecai-Mark
More informationProperties of the thinnest cold HI clouds in the diffuse ISM
Properties of the thinnest cold HI clouds in the diffuse ISM Main Points: Very low-n(hi) & small CNM clouds are common in the ISM. Suggest existence of large WNM envelopes, contributing up to 95-99% of
More informationThe Competitive Accretion Debate
The Competitive Accretion Debate 1,2 Paul C. Clark 2 Ralf S. Klessen 3 Ian A. Bonnell 3 Rowan J. Smith 1 KITP 2 University of Heidelberg 3 University of St Andrews What is CA and how does it work? Theory
More informationDirect Evidence for Two Fluid Effects in Molecular Clouds. Dinshaw Balsara & David Tilley University of Notre Dame
Direct Evidence for Two Fluid Effects in Molecular Clouds Dinshaw Balsara & David Tilley University of Notre Dame 1 Outline Introduction earliest stages of star formation Theoretical background Magnetically
More information(Numerical) study of the collapse and of the fragmentation of prestellar dense core
(Numerical) study of the collapse and of the fragmentation of prestellar dense core Benoît Commerçon Supervisors: E. Audit, G. Chabrier and P. Hennebelle Collaborator: R. Teyssier (3D - AMR) CEA/DSM/IRFU/SAp
More informationThe Role of Magnetic Field in Star Formation in the Disk of Milky Way Galaxy Shu-ichiro Inutsuka (Nagoya University)
Role of Magnetic Field in Star Formation & Galactic Structure (Dec 20 22, 2017) The Role of Magnetic Field in Star Formation in the Disk of Milky Way Galaxy Shu-ichiro Inutsuka (Nagoya University) Main
More informationMotivation Q: WHY IS STAR FORMATION SO INEFFICIENT? Ṁ M gas / dyn. Log SFR. Kennicutt Log. gas / dyn
Motivation Q: WHY IS STAR FORMATION SO INEFFICIENT? Ṁ 0.017 M gas / dyn Log SFR Kennicutt 1998 Log gas / dyn Motivation Q: WHY IS STAR FORMATION SO INEFFICIENT? Moster 2009 No Feedback 10% of baryons Log(
More informationGiant molecular clouds: what are they made from, and how do they get there?
Mon. Not. R. Astron. Soc. 425, 2157 2168 (2012) doi:10.1111/j.1365-2966.2012.21558.x Giant molecular clouds: what are they made from, and how do they get there? C. L. Dobbs, 1,2,3 J. E. Pringle 4 and A.
More informationOn the structure of molecular clouds
Mon. Not. R. Astron. Soc. 427, 2562 2571 (2012) doi:10.1111/j.1365-2966.2012.22130.x On the structure of molecular clouds Javier Ballesteros-Paredes, 1 Paola D Alessio 1 and Lee Hartmann 2 1 Centro de
More informationSFEs in clusters. Final value of the SFE. For an isolated clump SFE exp. (t exp. = SFE(t exp. M ( cluster. t ) exp M clump. (t) M gas,i.
SFEs in clusters SFE(t) Final value of the SFE M cluster (t) M gas,i + M gas,acc (t) SFE exp = SFE(t exp ) M cluster (t exp ) M gas,i + M gas,acc ( t ) exp For an isolated clump SFE exp M ( cluster t )
More informationSAM GEEN (ITA, HEIDELBERG)
Episode IV: THE RETURN TO SAM GEEN (ITA, HEIDELBERG) WITH PATRICK HENNEBELLE PASCAL TREMBLIN AND JOAKIM ROSDAHL UV FEEDBACK IN CLOUDS HII HII regions, regions, supernovae, supernovae, Molecular Molecular
More informationMagnetic fields in the early phase of massive star formation
Magnetic fields in the early phase of massive star formation FLASH workshop in Hamburg 16.2.2012 Daniel Seifried Hamburger Sternwarte, University of Hamburg (Robi Banerjee, Ralf Klessen, Ralph Pudritz,
More informationFrédérique Motte (AIM Paris-Saclay)
Clusters of high-mass protostars: From extreme clouds to minibursts of star formation Frédérique Motte (AIM Paris-Saclay) Special thanks to S. Bontemps, T. Csengeri, P. Didelon, M. Hennemann, T. Hill,
More informationSubgrid Scale Physics in Galaxy Simulations
CRC 963 Astrophysical Turbulence and Flow Instabilities with thanks to Harald Braun, Jan Frederic Engels, Jens Niemeyer, IAG Ann Almgren and John Bell, LBNL Christoph Federrath, Monash University yt-project.org
More informationThe Initial Mass Function Elisa Chisari
The Initial Mass Function AST 541 Dec 4 2012 Outline The form of the IMF Summary of observations Ingredients of a complete model A Press Schechter model Numerical simulations Conclusions The form of the
More informationGrowing massive black holes via super-critical accretion on to stellar-mass seeds
Growing massive black holes via super-critical accretion on to stellar-mass seeds Alessandro Lupi IAP (Paris) DARK ERC-2010 AdG_20100224 in collaboration with: F. Haardt, M. Dotti, M. Colpi, D. Fiacconi,
More informationNir Mandelker, H.U.J.I.
Compressive vs Solenoidal Turbulence and Non-Linear VDI Nir Mandelker, H.U.J.I. IAU Symposium 319, August 11 2015 Collaborators: Avishai Dekel, Shigeki Inoue, Daniel Ceverino, Frederic Bournaud, Joel Primack
More informationThe Janus Face of Turbulent Pressure
CRC 963 Astrophysical Turbulence and Flow Instabilities with thanks to Christoph Federrath, Monash University Patrick Hennebelle, CEA/Saclay Alexei Kritsuk, UCSD yt-project.org Seminar über Astrophysik,
More informationMassive Star Formation in the LMC Resolved at Clump Scales
Massive Star Formation in the LMC Resolved at Clump Scales N44 NT80 N159 Rosie Chen (MPIfR) R. Indebetouw, A. Hughes, C. Henkel, R. Güsten, K. Menten, Z. Zhang, G. Li, J. Urquhart, M. Requena Torres, L.
More information18. Stellar Birth. Initiation of Star Formation. The Orion Nebula: A Close-Up View. Interstellar Gas & Dust in Our Galaxy
18. Stellar Birth Star observations & theories aid understanding Interstellar gas & dust in our galaxy Protostars form in cold, dark nebulae Protostars evolve into main-sequence stars Protostars both gain
More informationSink particle accretion test
Sink particle accretion test David A. Hubber & Stefanie Walch 1 Objectives Simulate spherically-symmetric Bondi accretion onto a sink particle for an isothermal gas. Calculate the accretion rate onto a
More informationPhysics and chemistry of the interstellar medium. Lecturers: Simon Glover, Rowan Smith Tutor: Raquel Chicharro
Physics and chemistry of the interstellar medium Lecturers: Simon Glover, Rowan Smith Tutor: Raquel Chicharro This course consists of three components: Lectures Exercises Seminar [Wed., 2-4] [Thu., 4-5]
More informationThe structure of the thermally bistable and turbulent atomic gas in the local interstellar medium
The structure of the thermally bistable and turbulent atomic gas in the local interstellar medium E. Saury, M.-A. Miville-Deschênes, P. Hennebelle, E. Audit, W. Schmidt To cite this version: E. Saury,
More information!"#$%&'(#)*'+*,+ %#--./&+0&'-&+1*"&-+ 0*2'+(*+! #"#1(&".9.'$+:"*(*1;<(&"-+
!"#$%&'(#)*'+*,+ %#--./&+0&'-&+1*"&-+ 0*2'+(*+!3444+567+ 18#"#1(&".9.'$+:"*(*1;
More informationSuperbubble Feedback in Galaxy Formation
Superbubble Feedback in Galaxy Formation Ben Keller (McMaster University) James Wadsley, Samantha Benincasa, Hugh Couchman Paper: astro-ph/1405.2625 (Accepted MNRAS) Keller, Wadsley, Benincasa & Couchman
More informationGalaxy Evolution & Black-Hole Growth (review)
Galaxy Evolution & Black-Hole Growth (review) Avishai Dekel The Hebrew University of Jerusalem & UCSC Delivered by Fangzhou Jiang Dali, China, November 2018 See also Claude-Andre s talk and Joel s talk
More informationUnstable Disks: Gas and Stars via an analytic model
Unstable Disks: Gas and Stars via an analytic model Marcello Cacciato in collaboration with Avishai Dekel Minerva Fellow @ HUJI Theoretical studies and hydrodynamical cosmological simulations have shown
More informationGalaxy Formation: Overview
Galaxy Formation: Overview Houjun Mo March 30, 2004 The basic picture Formation of dark matter halos. Gas cooling in dark matter halos Star formation in cold gas Evolution of the stellar populaion Metal
More informationSPH simulations of star/planet formation triggered by cloud-cloud collisions
Exoplanets: Detection, Formation and Dynamics Proceedings IAU Symposium No. 249, 2008 Y.-S. Sun, S. Ferraz-Mello & J.-L. Zhou, eds. c 2008 International Astronomical Union DOI: 00.0000/X000000000000000X
More informationarxiv: v2 [astro-ph] 3 Sep 2008
TWO-FLUID MHD SIMULATIONS OF CONVERGING HI FLOWS IN THE INTERSTELLAR MEDIUM. I: METHODOLOGY AND BASIC RESULTS Tsuyoshi Inoue 1,2, and Shu-ichiro Inutsuka 1,3 arxiv:0801.0486v2 [astro-ph] 3 Sep 2008 ABSTRACT
More informationarxiv: v1 [astro-ph] 29 Oct 2008
STAR FORMATION TRIGGERED BY SNR 1 STAR FORMATION TRIGGERED BY SNR IMPACT INTO MAGNETIZED NEUTRAL CLOUDS M. R. M. Leão, 1,5 E. M. de Gouveia Dal Pino, 1,6 D. Falceta-Gonçalves, 2,3,7 C. Melioli, 4,8 F.
More informationFeedback flows of gas, energy and momentum in and out of galaxies
Feedback flows of gas, energy and momentum in and out of galaxies Matthijs H.D. van der Wiel March 10 th 2005 a part of the course Formation and Evolution of Galaxies Feedback accretion outflow Feedback
More informationChapter 11 The Formation and Structure of Stars
Chapter 11 The Formation and Structure of Stars Guidepost The last chapter introduced you to the gas and dust between the stars that are raw material for new stars. Here you will begin putting together
More informationTwo Phase Formation of Massive Galaxies
Two Phase Formation of Massive Galaxies Focus: High Resolution Cosmological Zoom Simulation of Massive Galaxies ApJ.L.,658,710 (2007) ApJ.,697, 38 (2009) ApJ.L.,699,L178 (2009) ApJ.,725,2312 (2010) ApJ.,744,63(2012)
More informationFrom Massive Cores to Massive Stars
From Massive Cores to Massive Stars Mark Krumholz Princeton University / UC Santa Cruz Collaborators: Richard Klein, Christopher McKee (UC Berkeley) Kaitlin Kratter, Christopher Matzner (U. Toronto) Jonathan
More informationOrigin of Bi-modality
Origin of Bi-modality and Downsizing Avishai Dekel HU Jerusalem Galaxies and Structures Through Cosmic Times Venice, March 2006 Summary Q: z
More informationASTR 610 Theory of Galaxy Formation Lecture 16: Star Formation
ASTR 610 Theory of Galaxy Formation Lecture 16: Star Formation Frank van den Bosch Yale University, spring 2017 Star Formation In this lecture we discuss the formation of stars. After describing the structure
More informationThe link between solenoidal turbulence and slow star formation in G
The Multi-Messenger Astrophysics of the Galactic Centre Proceedings IAU Symposium No. 322, 2016 R. M. Crocker, S. N. Longmore & G. V. Bicknell, eds. c 2016 International Astronomical Union DOI: 00.0000/X000000000000000X
More informationThe Birth Of Stars. How do stars form from the interstellar medium Where does star formation take place How do we induce star formation
Goals: The Birth Of Stars How do stars form from the interstellar medium Where does star formation take place How do we induce star formation Interstellar Medium Gas and dust between stars is the interstellar
More informationGas Cloud Collisions and Stellar Cluster Formation
Gas Cloud Collisions and Stellar Cluster Formation J. Klapp 1, G. Arreaga-Garcia 2 1 Instituto Nacional de Investigaciones Nucleares, Km 36.5 Carretera México-Toluca, Ocoyoacac, 52750 Estado de México,
More informationUnbound star-forming molecular clouds
Advance Access publication 2014 January 30 doi:10.1093/mnras/stu004 Unbound star-forming molecular clouds Rachel L. Ward, James Wadsley and Alison Sills Department of Physics and Astronomy, McMaster University,
More informationTheory of star formation
Theory of star formation Monday 8th 17.15 18.00 Molecular clouds and star formation: Introduction Tuesday 9th 13.15 14.00 Molecular clouds: structure, physics, and chemistry 16.00 16.45 Cloud cores: statistics
More informationSpiral Density waves initiate star formation
Spiral Density waves initiate star formation A molecular cloud passing through the Sagittarius spiral arm Spiral arm Gas outflows from super supernova or O/B star winds Initiation of star formation Supernova
More informationThe Early Evolution of low mass stars and Brown Dwarfs. I. Baraffe University of Exeter
The Early Evolution of low mass stars and Brown Dwarfs I. Baraffe University of Exeter 1. Some observational/theoretical facts Spread in the HRD Lithium depletion Evidence for episodic accretion - Embedded
More informationarxiv: v1 [astro-ph.ga] 24 Jun 2009
Numerical Star-Formation Studies A Status Report arxiv:0906.4452v1 [astro-ph.ga] 24 Jun 2009 Ralf S. Klessen Zentrum für Astronomie der Universität Heidelberg, Institut für Theoretische Astrophysik, Albert-Ueberle-Str.
More informationarxiv: v3 [astro-ph.ga] 28 Nov 2017
Astronomy & Astrophysics manuscript no. chira217 c ESO 217 November 29, 217 arxiv:1711.1417v3 [astro-ph.ga] 28 Nov 217 On the fragmentation of filaments in a molecular cloud simulation R.-A. Chira 1,2,
More informationAccretion Mechanisms
Massive Protostars Accretion Mechanism Debate Protostellar Evolution: - Radiative stability - Deuterium shell burning - Contraction and Hydrogen Ignition Stahler & Palla (2004): Section 11.4 Accretion
More informationTHE FORMATION OF MASSIVE STARS. η Carina (NASA, ESA, N. Smith)
THE FORMATION OF MASSIVE STARS η Carina (NASA, ESA, N. Smith) THE FORMATION OF MASSIVE STARS Christopher F. McKee HIPACC, UCSC August 8, 2013 with Andrew Cunningham Richard Klein Mark Krumholz Andrew Myers
More informationAstronomy 1 Fall 2016
Astronomy 1 Fall 2016 Lecture11; November 1, 2016 Previously on Astro-1 Introduction to stars Measuring distances Inverse square law: luminosity vs brightness Colors and spectral types, the H-R diagram
More informationOutflows from young stellar objects and their impact on star formation
Outflows from young stellar objects and their impact on star formation Robi Banerjee 1, @ 1 : Hamburg Sternewarte, University of Hamburg Gojenbergsweg 112 21209 Hamburg - Germany Jets and outflows are
More informationOrigin and Evolution of Disk Galaxy Scaling Relations
Origin and Evolution of Disk Galaxy Scaling Relations Aaron A. Dutton (CITA National Fellow, University of Victoria) Collaborators: Frank C. van den Bosch (Utah), Avishai Dekel (HU Jerusalem), + DEEP2
More informationMulti-Physics of Feedback in Massive Star Formation
Multi-Physics of Feedback in Massive Star Formation Rolf Kuiper1,2 H. W. Yorke3, N. J. Turner3, T. Hosokawa4 1 - Institute of Astronomy and Astrophysics, University of Tübingen, Germany 2 - Emmy Noether
More informationThe Origin of the Initial Mass Function
The Origin of the Initial Mass Function Ian A. Bonnell University of St Andrews Richard B. Larson Yale University Hans Zinnecker Astrophysikalisches Institut Potsdam Bonnell et al.: Origin of the Initial
More informationarxiv:astro-ph/ v1 17 Mar 2006
The Origin of the Initial Mass Function Ian A. Bonnell University of St Andrews Richard B. Larson Yale University Hans Zinnecker Astrophysikalisches Institut Potsdam arxiv:astro-ph/0603447v1 17 Mar 2006
More informationCooling, dynamics and fragmentation of massive gas clouds: clues to the masses and radii of galaxies and clusters
of massive gas and radii of M. Rees, J. Ostriker 1977 March 5, 2009 Talk contents: The global picture The relevant theory Implications of the theory Conclusions The global picture Galaxies and have characteristic
More informationLecture 23 Internal Structure of Molecular Clouds
Lecture 23 Internal Structure of Molecular Clouds 1. Location of the Molecular Gas 2. The Atomic Hydrogen Content 3. Formation of Clouds 4. Clouds, Clumps and Cores 5. Observing Molecular Cloud Cores References
More information