Resolving the hot atmospheres of evolved stars with ALMA LBs. Wouter Vlemmings, Chalmers Univ. of Technology w. Theo Khouri, Eamon O Gorman et al.
|
|
- Clara Walsh
- 5 years ago
- Views:
Transcription
1 Resolving the hot atmospheres of evolved stars with ALMA LBs Wouter Vlemmings, Chalmers Univ. of Technology w. Theo Khouri, Eamon O Gorman et al.
2 AGB mass loss
3 (before) dust formation Ballistic motions from pulsations Convection Freytag et al. (2017)
4 Radio/submm stellar surface observations Unique probes of temperature profile through the atmosphere free-free optical depth changes with observing frequency (Reid & Menten 1997) direct probe of temperature within 1-4 R star resolution improvements with ALMA allow resolving structures much less line confusion lines allow for probes of the dynamics Trace e.g. convective motions, shocks, stellar (magnetic) activity within wind acceleration zone chromospheres? e.g. Betelgeuse (O Gorman et al. 2015)
5 W Hya size & dust W Hya Teff L D dm/dt 2500 K 5400 Lsun 98 pc 1.3x10-7 Msun/yr Zhao-Geisler et al R *,1μm~2 AU (20mas) Ohnaka et al. 2016
6 Radio ~7 mm W ~1 ~1.2 cm Reid & Menten 1997, 2007 Matthews et al. 2015
7 W 338 GHz Observed Dec 2015 With 8 km baselines robust weighting: 38x31 mas beam Vlemmings et al. 2017
8 W 338 GHz Observed Dec 2015 With 8 km baselines robust weighting: 38x31 mas beam uniform weighting: 17x24 mas beam (restored with 17 mas circular beam) Vlemmings et al. 2017
9 W 338 GHz Observed Dec 2015 With 8 km baselines robust weighting: 38x31 mas beam uniform weighting: 17x24 mas beam (restored with 17 mas circular beam) Residuals after subtracting best fit disk 56.5 x degrees Vlemmings et al. 2017
10 Hotspots and inhomogenieties Significant structure seen on the stellar disk Average disk temperature ~2500 K, similar to photosphere Unresolved features lower limits on temperature
11 Hotspots and inhomogenieties Significant structure seen on the stellar disk brightest hotspot < 2x3 mas (5 σ) > K! other spots of several K as well as colder spots (larger optical depth) few 100 K below disk temp.
12 Result summary ~7 mm W ~1 μm Chromosphere average T~2500 K non-uniform disk with mottled surface and compact hotspot area filling factor <0.1% up to > K Change of dynamics across the star infall and outflow up to ~20 km/s hot region lower infall ~1.2 cm
13 Model comparison W Hya Freytag et al. (2017)
14 Result Summary II Shock heating non-instantaneous radiation of shock energy Low filling factor chromosphere origin of UV emission? >65% of all AGB stars are UV active (Montez et al. 2017) contribution of magnetic activity? gas mass >> mass lost per year all expelled gas will experience shock heating shock chemistry unavoidable
15 0.4 deltamodel Outlook gaussmodel Offset [arcsec] B ig. 1. example caption Offset [arcsec] East offset [arcsec] ~1500 K A Mira A&B A B Offset [arcsec] Offset [arcsec] ~3000 K To map temperature East offset [arcsec] deltamodel Offset [arcsec] structure we need: multi-band obs resolving power (>4 beams across) continuum sensitivity not very crucial, SNR>100 gaussmodel requires Tb,rms<30 K practically ~1 hr per source self-calibration! Offset [arcsec] East offset [arcsec] -0.4 Vlemmings et al East offset [arcsec] white dwarf companion East offset [arcsec] East offset [arcsec]
16 5 Dec 2015 Outlook II max 345 GHz nr. of stars notes Current ~16 mas ~5 oxygen-rich! x2 ~8 mas ~20 x3 ~5 mas ~100 oxygen-rich dominated optical/nir interferometryy synergy W Hya (scattered) dust polarisation VLT Sphere (Khouri et al. in prep) for >4 beams across briggs (0.5) weighting R Dor VLT Sphere (Khouri et al. in prep) VLTI (Wittkowski et al. 2017)
17 Conclusions ALMA long baselines provide unique capability to characterise the extended atmospheres of evolved stars Only probe of temperature structure together with dynamics! (next talk) (non-thermal processes with full polarisation) Avoid line opacity sources affecting most other wavelengths important synergy with optical/(n)ir observations The required model constraints for the study of dust formation and wind driving (ISM replenishment) Direct probes of astrophysical dust (seed) formation only possible around evolved stars!
Imaging the complex atmosphere of cool evolved stars Observing stars like the Sun
Imaging the complex atmosphere of cool evolved stars Observing stars like the Sun Keiichi Ohnaka Max Planck Institute for Radio Astronomy Bonn, Germany Graphics: L. Calçada (ESO) Mass-loss in cool evolved
More informationContinuum and Line ALMA band 5: the supergiant VY CMa
Continuum and Line Polarisation @ ALMA band 5: the supergiant VY CMa Wouter Vlemmings, Chalmers Univ. of Technology w. Theo Khouri, Daniel Tafoya, Ivan Marti-Vidal, Liz Humphreys, Anita Richards, Eamon
More informationarxiv: v1 [astro-ph.sr] 9 Oct 2018
Astronomy & Astrophysics manuscript no. Arxiv Version ESO 218 October 1, 218 High-resolution observations of gas and dust around Mira using ALMA and SPHERE/ZIMPOL T. Khouri 1, W. H. T. Vlemmings 1, H.
More informationarxiv: v2 [astro-ph.sr] 18 Apr 2015
Astronomy& Astrophysics manuscript no. Vlemmings_Mira c ESO 215 April 21, 215 Letter to the Editor Resolving the stellar activity of the Mira AB binary with ALMA W. H. T. Vlemmings 1,, S. Ramstedt 2, E.
More informationINTERFEROMETRIC OBSERVATIONS OF EVOLVED STARS
INTERFEROMETRIC OBSERVATIONS OF EVOLVED STARS Iva KAROVICOVA MPIA Heidelberg, Germany M. WITTKOWSKI ESO Garching, Germany D. A. BOBOLTZ Naval Observatory, USA E. FOSSAT Observatoire de la Côte d'azur,
More informationAGB stars and their environment. Michel Guélin (Presenter: Ka Tat Wong) Institut de Radioastronomie Millimétrique (IRAM) Grenoble, France
AGB stars and their environment Michel Guélin (Presenter: Ka Tat Wong) Institut de Radioastronomie Millimétrique (IRAM) Grenoble, France 1. AGB stars and their winds: why, how? 2. New interferometric observations
More informationRecent VLTI results on stellar winds and perspectives with second generation instruments. Xavier Haubois
Recent VLTI results on stellar winds and perspectives with second generation instruments Xavier Haubois Outline - The VLTI and its instruments - Massive stars - HMXBs - AGBs - Planetary Nebulae - Perspectives
More informationDynamical Atmospheres & Winds of AGB Stars A Theorist's View
Dynamical Atmospheres & Winds of AGB Stars A Theorist's View Susanne Höfner Department of Physics & Astronomy Uppsala University Dynamics of atmosphere & wind stellar pulsation & convection induce strong
More informationThe Mira variable S Ori: SiO maser shells related to the photosphere and dust shell at 3 epochs
The Mira variable S Ori: SiO maser shells related to the photosphere and dust shell at 3 epochs Program of coordinated interferometry of oxygen-rich evolved stars at near-infrared, mid-infrared, and radio
More informationWind properties and clumping
Wind properties and clumping Red Supergiants and Asymptotic Giant Branch stars (with no obvious companions) How are clouds formed? What affects their journey to the ISM? Anita Richards, Manchester Assaf,
More informationResolving evolved Sun-like stars' mass loss
Resolving evolved Sun-like stars' mass loss Anita Richards UK ARC, JBCA, Manchester with thanks to Bains, Bartkiewicz, Diamond, Dinh Van Trung, Gray, Lekht, Lim, Mendoza, Murakawa, Rosa-Gonzalez, Szymczak,
More informationSeeing into stars and their clouds
Seeing into stars and their clouds Anita Richards, UK ARC node, JBCA, Manchester with thanks to many collaborators How is matter ejected from old, cool stars? How is it accelerated? Relationships between
More informationIR spectro-interferometry of cool evolved stars
IR spectro-interferometry of cool evolved stars Keiichi Ohnaka Max-Planck-Institut für Radioastronomie Infrared Interferometry Group 1) Mid-IR interferometry of Mira stars 2) Near-IR spectro-interferometry
More informationProbing the Molecular Outflows of the Coldest Known Object in the Universe The Boomerang Nebula. R.Sahai (JPL) W. Vlemmings, L-A Nyman & P.
Probing the Molecular Outflows of the Coldest Known Object in the Universe The Boomerang Nebula R.Sahai (JPL) W. Vlemmings, L-A Nyman & P. Huggins The Extraordinary Deaths of Ordinary Stars Planetary nebulae
More informationVLTI/AMBER studies of the atmospheric structures and fundamental parameters of red giant and supergiant stars
VLTI/AMBER studies of the atmospheric structures and fundamental parameters of red giant and supergiant stars B. Arroyo-Torres, M. Wittkowski and J. M. Marcaide Contributors: P. H. Hauschildt, A. Chiavassa,
More informationRadio/mm/sub-mm Observations of AGB and RSG stars. Hans Olofsson Dept. of Earth and Space Sciences, Chalmers
Radio/mm/sub-mm Observations of AGB and RSG stars Hans Olofsson Dept. of Earth and Space Sciences, Chalmers Outline I will cover the following topics:! The central stars! Chemistry: Spectral scans Source
More informationScience Opportunities in Stellar Physics. Douglas R. Gies CHARA, Georgia State Univ., and the Stellar Physics Working Group
Science Opportunities in Stellar Physics Douglas R. Gies CHARA, Georgia State Univ., gies@chara.gsu.edu and the Stellar Physics Working Group General Themes! Fundamental properties! Interior structure
More informationAbout the angular diameter of red supergiant stars
Mass loss of evolved stars Betlegeuse/PIONIER Antares/PIONIER CE Tau/PIONIER Conclusion About the angular diameter of red supergiant stars Miguel Montargès (IRAM) VLTI Community Days ESO Garching - March
More informationInterferometric Observations of S140-IRS1
Interferometric Observations of S140-IRS1 e-merlin early science workshop April 2014 Luke T. Maud University of Leeds, UK Melvin G. Hoare University of Leeds Star formation scenario Collapse of a core
More informationChallenges for the Study of Hot Cores with ALMA: NGC 6334I
Challenges for the Study of Hot Cores with ALMA: NGC 6334I Crystal Brogan (NRAO/North American ALMA Science Center) Collaborators: Todd Hunter (NRAO) Remy Indebetouw (UVa/NRAO), Ken (Taco) Young (CfA),
More informationThe innermost circumstellar environment of massive young stellar objects revealed by infrared interferometry
The innermost circumstellar environment of massive young stellar objects revealed by infrared interferometry Thomas Preibisch, Stefan Kraus, Keiichi Ohnaka Max Planck Institute for Radio Astronomy, Bonn
More informationThe ALMA SKA Synergy For Star and Stellar Cluster Formation
The ALMA SKA Synergy For Star and Stellar Cluster Formation Gary Fuller Jodrell Bank Centre for Astrophysics & UK ALMA Regional Centre Node University of Manchester What is ALMA? Atacama Large Millimetre/Sub-millimetre
More informationMagnetic fields around evolved stars
Magnetic fields around evolved stars Downloaded from: https://research.chalmers.se, 2019-01-20 00:12 UTC Citation for the original published paper (version of record): Vlemmings, W. (2018) Magnetic fields
More informationAtmospheric Dynamics & Winds of AGB stars: A Theorist's View. Susanne Höfner Department of Physics and Astronomy Uppsala University
Atmospheric Dynamics & Winds of AGB stars: A Theorist's View Susanne Höfner Department of Physics and Astronomy Uppsala University Overview Dynamical atmospheres convection, pulsation, extended structures
More informationE-ELT METIS * AND MATISSE: PROSPECTS FOR AGB-STARS
E-ELT METIS * AND MATISSE: PROSPECTS FOR AGB-STARS J. Hron 1, J. Blommaert 2, L. Decin 2, T. Lebzelter 1, C. Paladini 3,1, H. Van Winckel 2 and the METIS and MATISSE teams (1) Universitätssternwarte Wien,
More informationSpectroscopy of giants and supergiants! Maria Bergemann MPIA Heidelberg"
Spectroscopy of giants and supergiants! Maria Bergemann MPIA Heidelberg" Spectroscopy of (cool) giants and supergiants! Maria Bergemann MPIA Heidelberg" Outline! Motivation why do spectroscopy of giant
More informationLate-Type Stars and Observational Studies Based on SiO and H 2 O Masers Jan., 2018 Kantary Hills Hotel, Chiang Mai, Tailand
Late-Type Stars and Observational Studies Based on SiO and H 2 O Masers 16-19 Jan., 2018 Kantary Hills Hotel, Chiang Mai, Tailand Se-Hyung Cho, KASI, Korea Outlines Basic Introduction Studies of Late-Type
More informationSub-mm maser VLBI: how do stellar winds break free from the star s gravity?
: how do stellar winds break free from the star s gravity? a A. Baudry b,c S. Etoka d E.A. Humphreys e C.M.V. Impellizeri f,g H.J. van Langevelde h,i and W. Vlemmings j a Jodrell Bank Centre for Astrophysics,
More informationarxiv:astro-ph/ v1 21 May 2003
Astronomy & Astrophysics manuscript no. 3752 January 17, 2014 (DOI: will be inserted by hand later) VLBI astrometry of circumstellar OH masers; proper motions and parallaxes of four AGB stars W.H.T. Vlemmings
More informationMasers around evolved stars from kinematics to physics
Masers around evolved stars from kinematics to physics Anita Richards UK ARC, JBCA, Manchester with thanks to Al-Muntafki, Bains, Bartkiewicz, Diamond, Elitzur, Etoka, Gray, Humphreys, Murakawa, Rosa-Gonzalez,
More informationMilky Way SKA: the ISM, star formation and stellar evolution with the SKA
Milky Way SKA: the ISM, star formation and stellar evolution with the SKA Mark Thompson, Grazia Umana, Naomi McClure-Griffiths, Laurent Loinard, Gary Fuller, Guillem Anglada, Sergio Molinari, Raymond Oonk
More informationExercise: A Toy Model for Dust-driven Winds
Astrofysikalisk dynamik, VT 00 Exercise: A Toy Model for Dust-driven Winds Susanne Höfner Department of Physics and Astronomy, Uppsala University Cool luminous giants stars, in particular pulsating AGB
More informationLate-Type Stars. Liz Humphreys (ESO)
Late-Type Stars Liz Humphreys (ESO) Markus Wittkowski, Alain Baudry, Eric Blackman, Jason Grunhut, Susanne Hoefner, Franz Kerschbaum, Pierre Kervella, Mikako Matsuura, Iain Mcdonald, Claudia Paladini,
More informationClassical Interferometric Arrays. Andreas Quirrenbach Landessternwarte Heidelberg
Classical Interferometric Arrays Andreas Quirrenbach Landessternwarte Heidelberg The VLT Interferometer Tucson 11/14/2006 Andreas Quirrenbach 2 Optical / Infrared Interferometry Today Access to milliarcsecond-scale
More informationFirst Resolved Images of the Mira AB Symbiotic Binary at Centimeter Wavelengths
First Resolved Images of the Mira AB Symbiotic Binary at Centimeter Wavelengths Lynn D. Matthews 1 and Margarita Karovska 1 ABSTRACT We report the first spatially resolved radio continuum measurements
More informationThe Impact of the Galactic Center Arches Cluster: Radio & X-ray Observations
The Impact of the Galactic Center Arches Cluster: Radio & X-ray Observations Cornelia C. Lang University of Iowa GC region (Sagittarius) is obscured by ~30 visual magnitudes of extinction no optical, UV;
More information2. Stellar atmospheres: Structure
2. Stellar atmospheres: Structure 2.1. Assumptions Plane-parallel geometry Hydrostatic equilibrium, i.e. o no large-scale accelerations comparable to surface gravity o no dynamically significant mass loss
More informationProbing companions of evolved stars
Introduction Spiral-shell Summary Probing companions of evolved stars (ASIAA, EACOA fellow)... migrating to KASI ALMA long baseline workshop @ Kyoto 2017-10-04 Introduction Spiral-shell Summary Evolution
More informationLate-type Stars with Perspective of Radio Observations. Youngjoo Yun 2018 Radio Winter of Ulsan
Late-type Stars with Perspective of Radio Observations Youngjoo Yun 2018 Radio Winter School @University of Ulsan Outline l l l l Introduction to late-type stars with an example Brief description of stellar
More informationOrigins of clumps & asymmetries
Origins of clumps & asymmetries Anita Richards UK ALMA Regional Centre JBCA, University of Manchester with thanks to Assaf, Baudry, Decin, Etoka, Gray, Humphreys, O'Gorman, Vlemmings, Wittkowski & many
More informationATMOSPHERES OF C-RICH AGB STARS OBSERVATIONS AND MODELS
ATMOSPHERES OF C-RICH AGB STARS OBSERVATIONS AND MODELS Gioia Rau University of Vienna - Institute for Astrophysics Blowing in the Wind, 8 August 2016 Collaborators: B. Aringer, K. Eriksson, M. A. T. Groenewegen,
More informationRadio Nebulae around Luminous Blue Variable Stars
Radio Nebulae around Luminous Blue Variable Stars Claudia Agliozzo 1 G. Umana 2 C. Trigilio 2 C. Buemi 2 P. Leto 2 A. Ingallinera 1 A. Noriega-Crespo 3 J. Hora 4 1 University of Catania, Italy 2 INAF-Astrophysical
More informationThe Superbubble Power Problem: Overview and Recent Developments. S. Oey
The Superbubble Power Problem: Overview and Recent Developments S. Oey It has been known for decades that superbubbles generated by massive star winds and supernovae are smaller than expected based on
More informationImaging of Stellar Surfaces
DOI: 10.18727/0722-6691/5080 Report on the ESO Workshop Imaging of Stellar Surfaces held at ESO Headquarters, Garching, Germany, 5 9 March 2018 Markus Wittkowski 1 Liz Humphreys 1 1 ESO There have recently
More informationNear-Infrared Imaging Observations of the Orion A-W Star Forming Region
Chin. J. Astron. Astrophys. Vol. 2 (2002), No. 3, 260 265 ( http: /www.chjaa.org or http: /chjaa.bao.ac.cn ) Chinese Journal of Astronomy and Astrophysics Near-Infrared Imaging Observations of the Orion
More informationGalaxy Ecosystems Adam Leroy (OSU), Eric Murphy (NRAO/IPAC) on behalf of ngvla Working Group 2
Next Generation Very Large Array Working Group 2 HI in M74: Walter+ 08 CO in M51: Schinnerer+ 13 Continuum in M82: Marvil & Owen Galaxy Ecosystems Adam Leroy (OSU), Eric Murphy (NRAO/IPAC) on behalf of
More informationFrom AGB Stars to Planetary Nebula. Cats Eye Planetary Nebula: HST
From AGB Stars to Planetary Nebula Cats Eye Planetary Nebula: HST AGB Stars NOAO H -> He in convective region Dredge Up Prialnik AGB stars pulsing Schwarzchild & Harm (1967) The 9th Cycle Schwarzchild
More informationTh. Henning, J. Bouwman, J. Rodmann MPI for Astronomy (MPIA), Heidelberg. Grain Growth in Protoplanetary Disks From Infrared to Millimetre Wavelengths
Th. Henning, J. Bouwman, J. Rodmann MPI for Astronomy (MPIA), Heidelberg Grain Growth in Protoplanetary Disks From Infrared to Millimetre Wavelengths Cumber01.ppt 30.5.2001 Motivation From molecular cloud
More informationSTUDYING COMPACT RADIO SOURCES ASSOCIATED WITH UCHII REGIONS
STUDYING COMPACT RADIO SOURCES ASSOCIATED WITH UCHII REGIONS Josep Maria Masqué Saumell Departamento de Astronomía Universidad de Guanajuato Collaborators: Universidad de Guanajuato: Miguel Angel Trinidad,
More informationTHE LAST SURVEY OF THE OLD WSRT: TOOLS AND RESULTS FOR THE FUTURE HI ABSORPTION SURVEYS
F. Maccagni; R. Morganti; T. Oosterloo; K. Geréb; N. Maddox, J. Allison THE LAST SURVEY OF THE OLD WSRT: TOOLS AND RESULTS FOR THE FUTURE HI ABSORPTION SURVEYS A SURVEY BEFORE THE BLIND SURVEYS During
More informationThe Physics of the Interstellar Medium
The Physics of the Interstellar Medium Ulrike Heiter Contact: 471 5970 ulrike@astro.uu.se www.astro.uu.se Matter between stars Average distance between stars in solar neighbourhood: 1 pc = 3 x 1013 km,
More informationFrom the VLT to ALMA and to the E-ELT
From the VLT to ALMA and to the E-ELT Mission Develop and operate world-class observing facilities for astronomical research Organize collaborations in astronomy Intergovernmental treaty-level organization
More informationarxiv: v1 [astro-ph.sr] 12 Apr 2018
Astronomy & Astrophysics manuscript no. 32929 c ESO 218 September 26, 218 Letter to the Editor Rotation of the asymptotic giant branch star R Doradus W. H. T. Vlemmings 1,, T. Khouri 1, E. De Beck 1, H.
More informationTransition Disk Chemistry in the Eye of ALMA
COURTESY NASA/JPL-CALTECH Spectroscopy2011 January 16, 2011 Transition Disk Chemistry in the Eye of ALMA Ilse Cleeves Univ. of Michigan ADVISOR: Edwin Bergin Outline I. Transition Disks: Introduction II.
More informationAn Introduction to Stellar Radio Astronomy. Manuel Güdel University of Vienna
An Introduction to Stellar Radio Astronomy Manuel Güdel University of Vienna Outline 1. Thermal bremsstrahlung stellar photospheres 2a. Gyromagnetic emission 2b. Coherent radiation in plasma stellar coronae
More informationWhat does the Sun tell us about circular polarization on stars? Stephen White
What does the Sun tell us about circular polarization on stars? Stephen White The Radio Sun at 4.6 GHz Combination of: optically thick upper chromosphere, optically thick coronal gyroresonance where B>500
More informationNEW MEASUREMENTS OF THE RADIO PHOTOSPHERE OF MIRA BASED ON DATA FROM THE JVLA AND ALMA
2015. The American Astronomical Society. All rights reserved. doi:10.1088/0004-637x/808/1/36 NEW MEASUREMENTS OF THE RADIO PHOTOSPHERE OF MIRA BASED ON DATA FROM THE JVLA AND ALMA L. D. Matthews 1, M.
More informationCan we do this science with SKA1-mid?
Can we do this science with SKA1-mid? Let s start with the baseline design SKA1-mid expected to go up to 3.05 GHz Proposed array configuration: 133 dishes in ~1km core, +64 dishes out to 4 km, +57 antennas
More informationTHE SPHERE VIEW OF BETELGEUSE
Title : will be set by the publisher Editors : will be set by the publisher EAS Publications Series, Vol.?, 2013 THE SPHERE VIEW OF BETELGEUSE O. Chesneau 1, H.-M. Schmid 2, M. Carbillet 3, A. Chiavassa
More informationDiscovery of Terahertz Water Masers with SOFIA/GREAT
Discovery of Terahertz Water Masers with SOFIA/GREAT 1 Outline Motivation for studying water masers Physics of maser amplification Discovery of Terahertz masers with SOFIA 2 Water masers First detection
More informationThe shock-heated atmosphere of an asymptotic giant branch star resolved by ALMA
The shock-heated atmosphere of an asymptotic giant branch star resolved by ALMA Authors: Wouter Vlemmings 1,*, Theo Khouri 1, Eamon O Gorman 2, Elvire De Beck 1, Elizabeth Humphreys 3, Boy Lankhaar 1,
More informationE-ELT/HIRES Disk-Star Interactions at the epoch of planet formation
E-ELT/HIRES Disk-Star Interactions at the epoch of planet formation Leonardo Testi (ESO/INAF-Arcetri) B. Nisini (INAF-Monteporzio), J. Alcalaʼ (INAF-Capodimonte) From Cores to Planetary Systems Core (Hernandez
More informationInterstellar Medium and Star Birth
Interstellar Medium and Star Birth Interstellar dust Lagoon nebula: dust + gas Interstellar Dust Extinction and scattering responsible for localized patches of darkness (dark clouds), as well as widespread
More informationPayne-Scott workshop on Hyper Compact HII regions Sydney, September 8, 2010
Payne-Scott workshop on Hyper Compact HII regions Sydney, September 8, 2010 Aim Review the characteristics of regions of ionized gas within young massive star forming regions. Will focus the discussion
More informationZooming into high-mass star-forming regions
Zooming into high-mass star-forming regions Henrik Beuther SMA ATCA PdBI VLA Important questions - What are the characteristics of accretion disks/large toroid in high-mass star formation? - Can we constrain
More informationEnergy Sources of the Far IR Emission of M33
Energy Sources of the Far IR Emission of M33 Hinz, Reike et al., ApJ 154: S259 265 (2004). Presented by James Ledoux 24 µm 70 µm 160 µm Slide 1 M33 Properties Distance 840kpc = 2.7 Mlyr (1'' ~ 4 pc) Also
More informationStellar Winds: Mechanisms and Dynamics
Astrofysikalisk dynamik, VT 010 Stellar Winds: Mechanisms and Dynamics Lecture Notes Susanne Höfner Department of Physics and Astronomy Uppsala University 1 Most stars have a stellar wind, i.e. and outflow
More informationThe formation of super-stellar clusters
The formation of super-stellar clusters François Boulanger Institut d Astrophysique Spatiale Cynthia Herrera, Edith Falgarone, Pierre Guillard, Nicole Nesvadba, Guillaume Pineau des Forets Outline How
More informationSetting the Stage for Planet Formation: Grain Growth in Circumstellar Disks
Setting the Stage for Planet Formation: Grain Growth in Circumstellar Disks Leonardo Testi (European Southern Observatory) Disk Evolution From Grains to Pebbles Do we understand what we observe? Wish List
More information10x Effective area JVLA, ALMA 10x Resolution w. 50% to few km + 50% to 300km Frequency range: 1 50, GHz
10x Effective area JVLA, ALMA 10x Resolution w. 50% to few km + 50% to 300km Frequency range: 1 50, 70 115 GHz JVLA: Good 3mm site, elev. ~ 2200m Residual phase rms after calibration 90% coherence 550km
More informationet al. 1996; Hansen 2005; Kalirai et al ML is a free parameter with a huge astrophysical impact
Rood 1973; Fusi Pecci & Renzini 1975,1976; Renzini 1977; Castellani & Tornambe 1981; Peterson 1982; Castellani & Castellani 1993; Fusi Pecci et al. 1993; D Cruz et al. 1996; Hansen 2005; Kalirai et al.
More informationarxiv: v1 [astro-ph.sr] 27 Sep 2018
Why Galaxies Care About AGB Stars: A Continuing Challenge through Cosmic Time Proceedings IAU Symposium No. 343, 2018 c 2018 International Astronomical Union F. Kerschbaum, H. Olofsson & M. Groenewegen,
More informationAstro2010 Science White Paper: Tracing the Mass Buildup of Supermassive Black Holes and their Host Galaxies
Astro2010 Science White Paper: Tracing the Mass Buildup of Supermassive Black Holes and their Host Galaxies Anton M. Koekemoer (STScI) Dan Batcheldor (RIT) Marc Postman (STScI) Rachel Somerville (STScI)
More informationSolar Astrophysics with ALMA. Sujin Kim KASI/EA-ARC
Solar Astrophysics with ALMA Sujin Kim KASI/EA-ARC Contents 1. The Sun 2. ALMA science targets 3. ALMA capabilities for solar observation 4. Recent science results with ALMA 5. Summary 2 1. The Sun Dynamic
More informationOrianne ROOS CEA-Saclay Collaborators : F. Bournaud, J. Gabor, S. Juneau
Orianne ROOS CEA-Saclay Collaborators : F. Bournaud, J. Gabor, S. Juneau Bachelor of Physics, Master of Astrophysics Université de Strasbourg PhD, Université Paris-Diderot Observatoire de Strasbourg Les
More informationNew ALMA Long Baseline Observations of the Transitional Disk around TW Hya
New ALMA Long Baseline Observations of the Transitional Disk around TW Hya Takashi Tsukagoshi (Ibaraki University, Japan) H. Nomura, T. Muto, R. Kawabe, D. Ishimoto, K. D. Kanagawa, S. Okuzumi, S. Ida,
More informationNear -IR interferometry:
Near -IR interferometry: spectrally dispersed JHK-band IOTA / GI2T interferograms, advantages of NIR, and aims Gerd Weigelt Max-Planck Institute for Radioastronomy, Bonn Plan Interferometry with spectrally
More informationLifecycle of Dust in Galaxies
Lifecycle of Dust in Galaxies Karl Gordon Space Telescope Science Institute 3700 San Martin Drive Baltimore, MD 21218 Email: kgordon@stsci.edu Phone: 410-338-5031 co-authors: Margaret Meixner (Space Telescope
More informationStar formation history in high redshift radio galaxies
Cygnus A Star formation history in high redshift radio galaxies Collaborators: B. Rocca-Volmerange (IAP), C. De Breuck (ESO), J. Vernet (ESO), N. Seymour (CASS), D. Stern (JPL), M. Lehnert (IAP), P. Barthel
More informationMethanol masers and their environment at high resolution
Mon. Not. R. Astron. Soc. 300, 1131 1157 (1998) Methanol masers and their environment at high resolution C. J. Phillips, 1 R. P. Norris, 2 S. P. Ellingsen 1 and P. M. McCulloch 1 1 Department of Physics,
More informationThe role of magnetic fields during massive star formation
The role of magnetic fields during massive star formation Wouter Vlemmings Chalmers University of Technology / Onsala Space Observatory / Nordic ALMA Regional Center with: Gabriele Surcis, Kalle Torstensson,
More informationRadio Probes of Extrasolar Space Weather
Radio Probes of Extrasolar Space Weather Rachel Osten Space Telescope Science Institute Radio Stars: from khz to THz Haystack Observatory November 2, 2017 Star s magnetic field helps to set the environment
More informationVLTI/AMBER studies of the atmospheric structure and fundamental parameters of red giant and supergiant stars
**Volume Title** ASP Conference Series, Vol. **Volume Number** **Author** c **Copyright Year** Astronomical Society of the Pacific VLTI/AMBER studies of the atmospheric structure and fundamental parameters
More informationExploring the powering source of the TeV X-ray binary LS 5039
Exploring the powering source of the TeV X-ray binary LS 5039 Javier Moldón Marc Ribó Josep Maria Paredes Josep Martí (Univ. Jaén) Maria Massi (MPIfR) 9th European VLBI Network Symposium Bologna, Italy
More informationMass loss from stars
Mass loss from stars Can significantly affect a star s evolution, since the mass is such a critical parameter (e.g., L ~ M 4 ) Material ejected into interstellar medium (ISM) may be nuclear-processed:
More informationGalaxies of Many Colours: Star Formation Across Cosmic Time. z=0, t= /-0.037x10 9 years (Now)
Galaxies of Many Colours: Star Formation Across Cosmic Time z=0, t=13.798+/-0.037x10 9 years (Now) And if you want to study the initial conditions for star formation the colour is black Dense Gas SDC335:
More informationProbing the embedded phase of star formation with JWST spectroscopy
Probing the embedded phase of star formation with JWST spectroscopy NIRSPEC Spitzer NGC 1333 Low mass Herschel Cygnus X High mass Jorgensen et al. Gutermuth et al. 10 10 Motte, Henneman et al. E.F. van
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 informationUnraveling the Envelope and Disk: The ALMA Perspective
Unraveling the Envelope and Disk: The ALMA Perspective Leslie Looney (UIUC) Lee Mundy (UMd), Hsin-Fang Chiang (UIUC), Kostas Tassis (UChicago), Woojin Kwon (UIUC) The Early Disk Disks are probable generic
More informationSunbathing around low-mass protostars: new insights from hydrides
Sunbathing around low-mass protostars: new insights from hydrides Agata Karska (N. Copernicus Univ., Toruń, Poland) L. Kristensen, M. Kaufman & WISH, DIGIT, WILL teams (Univ. of Copenhagen, San Jose St.
More informationScience Prospects with the wsma
Science Prospects with the wsma SMA: the key mm interferometry facility the SMA has genuinely transformed fields, from planet formation to the high-redshift universe 700 publications; 21000 citations (>1
More informationExoplanets Direct imaging. Direct method of exoplanet detection. Direct imaging: observational challenges
Black body flux (in units 10-26 W m -2 Hz -1 ) of some Solar System bodies as seen from 10 pc. A putative hot Jupiter is also shown. The planets have two peaks in their spectra. The short-wavelength peak
More informationNuclear Star Formation, The Torus, & Gas Inflow in Seyfert Galaxies
Nuclear Star Formation, The Torus, & Gas Inflow in Seyfert Galaxies Richard Davies 1, H. Engel 1, M. Schartmann 1, G. Orban de Xivry 1, E. Sani 2, E. Hicks 3, A. Sternberg 4, R. Genzel 1, L. Tacconi 1,
More informationTime resolved X-ray spectral analysis during optical dips and accretion bursts in stars with disks of NGC2264 from Chandra/ACIS-I and CoRoT data
X-Ray Universe - 2017 Time resolved X-ray spectral analysis during optical dips and accretion bursts in stars with disks of NGC2264 from Chandra/ACIS-I and CoRoT data Time resolved X-ray spectral analysis
More informationRevision: Sun, Stars (and Planets) See web slides of Dr Clements for Planets revision. Juliet Pickering Office: Huxley 706
Revision: Sun, Stars (and Planets) See web slides of Dr Clements for Planets revision Juliet Pickering Office: Huxley 706 Office hour (Pickering): Thursday 22nd May 12-11 pm Outline overview of first part
More informationThe Most Detailed Picture Yet of a Massive Star in Formation
The Most Detailed Picture Yet of a Massive Star in Formation L. Greenhill (CfA/Kavli Inst./Berkeley) How do high-mass stars (M *»1 M ) form? What lies < 200 AU from high-mass YSOs? Do magnetic fields drive
More informationBinary Stars (continued) ASTR 2120 Sarazin. γ Caeli - Binary Star System
Binary Stars (continued) ASTR 2120 Sarazin γ Caeli - Binary Star System Visual Binaries: Types of Binary Stars Spectroscopic Binaries: Eclipsing Binaries: Periodic changes in brightness, stars block one
More informationThe physics of stars. A star begins simply as a roughly spherical ball of (mostly) hydrogen gas, responding only to gravity and it s own pressure.
Lecture 4 Stars The physics of stars A star begins simply as a roughly spherical ball of (mostly) hydrogen gas, responding only to gravity and it s own pressure. X-ray ultraviolet infrared radio To understand
More informationPulsar Wind Nebulae: A Multiwavelength Perspective
Pulsar Wind Nebulae: Collaborators: J. D. Gelfand T. Temim D. Castro S. M. LaMassa B. M. Gaensler J. P. Hughes S. Park D. J. Helfand O. C. de Jager A. Lemiere S. P. Reynolds S. Funk Y. Uchiyama A Multiwavelength
More informationarxiv:astro-ph/ v1 10 Sep 2004
The scientific promise of the SKA SKA Workshop Oxford, 2003 Kramer & Rawlings Late stages of stellar evolution with the Square Kilometer Array arxiv:astro-ph/0409242v1 10 Sep 2004 Albert A. Zijlstra UMIST,
More information