Long term evolution of circumstellar discs: DM Tau and GM Aur Ricardo Hueso (*) & Tristan Guillot Laboratoire Cassini, Observatoire de la Côte d’Azur,

Slides:



Advertisements
Similar presentations
Probing the Conditions for Planet Formation in Inner Protoplanetary Disks James Muzerolle.
Advertisements

Millimeter-Wavelength Observations of Circumstellar Disks and what they can tell us about planets A. Meredith Hughes Miller Fellow, UC Berkeley David Wilner,
3D Vortices in Stratified, Rotating, Shearing Protoplanetary Disks April 8, I PAM Workshop I: Astrophysical Fluid Dynamics Philip Marcus – UC Berkeley.
Disk Structure and Evolution (the so-called model of disk viscosity) Ge/Ay 133.
Proto-Planetary Disk and Planetary Formation
The formation of stars and planets Day 3, Topic 3: Irradiated protoplanetary disks Lecture by: C.P. Dullemond.
Structure and Evolution of Protoplanetary Disks Carsten Dominik University of Amsterdam Radboud University Nijmegen.
Protoplanetary Disks: The Initial Conditions of Planet Formation Eric Mamajek University of Rochester, Dept. of Physics & Astronomy Astrobio 2010 – Santiago.
Planet Formation Topic: Disk thermal structure Lecture by: C.P. Dullemond.
FU Ori and Outburst Mechanisms Zhaohuan Zhu Hubble Fellow, Princeton University Collaborators: Lee Hartmann (Umich), Charles Gammie (UIUC), Nuria Calvet.
Estimate of physical parameters of molecular clouds Observables: T MB (or F ν ), ν, Ω S Unknowns: V, T K, N X, M H 2, n H 2 –V velocity field –T K kinetic.
Star Birth How do stars form? What is the maximum mass of a new star? What is the minimum mass of a new star?
Chapter 7: The Birth and Evolution of Planetary Systems
1 Concluding Panel Al Glassgold Sienny Shang Jonathan Williams David Wilner.
Dust particles and their spectra. Review Ge/Ay 132 Final report Ivan Grudinin.
Disc clearing conventional view: most stars are either rich in circumstellar diagnostics, e.g. Or devoid of same: intermediate states less common ==> RAPID.
“The interaction of a giant planet with a disc with MHD turbulence II: The interaction of the planet with the disc” Papaloizou & Nelson 2003, MNRAS 339.
6. Stars evolve and eventually ‘die’
Jeong-Eun Lee Kyung Hee University University of Texas at Austin.
SELF-SIMILAR SOLUTIONS OF VISCOUS RESISTIVE ACCRETION FLOWS Jamshid Ghanbari Department of Physics, School of Sciences, Ferdowsi University of Mashhad,
DUSTY04 – Paris ALMA and ISM / Star Formation Stéphane GUILLOTEAU Observatoire de Bordeaux.
Planet Formation Topic: Viscous accretion disks Lecture by: C.P. Dullemond.
Ge/Ay133 SED studies of disk “lifetimes” & Long wavelength studies of disks.
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 Influence of Planets on Disk Observations (and the influence of disks on planet observations) Geoff Bryden (JPL) Doug Lin (UCSC) Hal Yorke (JPL)
Ge/Ay133 What effects do 1-10 M Earth cores & Jovian planets have on the surrounding disk? Or, … Migration & Gaps.
The formation of stars and planets Day 3, Topic 2: Viscous accretion disks Continued... Lecture by: C.P. Dullemond.
Ge/Ay133 Disk Structure and Spectral Energy Distributions (SEDs)
Planet Driven Disk Evolution Roman Rafikov IAS. Outline Introduction - Planet-disk interaction - Basics of the density wave theory Density waves as drivers.
Processes in Protoplanetary Disks
Planet Masses and Radii from Physical Principles Günther Wuchterl CoRoT / DLR Thüringer Landessternwarte Tautenburg.
Felipe Garrido Goicovic Supervisor: Jorge Cuadra PhD thesis project January 2014.
Stellar Winds and Mass Loss Brian Baptista. Summary Observations of mass loss Mass loss parameters for different types of stars Winds colliding with the.
Ge/Ay133 What effects do 1-10 M Earth cores have on the surrounding disk? Today = Gaps Wednesday = Migration (included here)
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.
Monte Carlo Radiation Transfer in Protoplanetary Disks: Disk-Planet Interactions Kenneth Wood St Andrews.
Multiwavelength Continuum Survey of Protostellar Disks in Ophiuchus Left: Submillimeter Array (SMA) aperture synthesis images of 870 μm (350 GHz) continuum.
Goal: To understand how stars form. Objectives: 1)To learn about the properties for the initial gas cloud for 1 star. 2)To understand the collapse and.
Collaborators : Valentine Wakelam (supervisor)
The study on Li abundances of solar-like stars Li Tanda Beijing Nomal University
6. GROWTH OF PLNETS: AN OVERVIEW 6.1. Observational Constraints a. The planets’ masses and radii and the age of the Solar System M E R E Neptune.
Alpha Disc Model in Accretion Disks Hongyu Gong Xiamen University.
Surface abundances of Am stars as a constraint on rotational mixing Olivier Richard 1,2, Suzanne Talon 2, Georges Michaud 2 1 GRAAL UMR5024, Université.
1 S. Davis, April 2004 A Beta-Viscosity Model for the Evolving Solar Nebula Sanford S Davis Workshop on Modeling the Structure, Chemistry, and Appearance.
Renaissance: Formation of the first light sources in the Universe after the Dark Ages Justin Vandenbroucke, UC Berkeley Physics 290H, February 12, 2008.
Time-Dependent Phenomena in Protoplanetary Disks
A Submillimeter View of Protoplanetary Disks Sean Andrews University of Hawaii Institute for Astronomy Jonathan Williams & Rita Mann, UH IfA David Wilner,
Infall rates from observations Joseph Mottram 1. Why is infall relevant? Infall must happen for star formation to proceed The rate of infall on envelope.
A-Ran Lyo KASI (Korea Astronomy and Space Science Institute) Nagayoshi Ohashi, Charlie Qi, David J. Wilner, and Yu-Nung Su Transitional disk system of.
The Early Stages of Star Formation Leo Blitz UC Berkeley Space, Time and Life – August 26, 2002.
Spiral Triggering of Star Formation Ian Bonnell, Clare Dobbs Tom Robitaille, University of St Andrews Jim Pringle IoA, Cambridge.
野口正史 (東北大学).  Numerical simulation Disk galaxy evolution driven by massive clumps  Analytical model building Hubble sequence.
The University of Western Ontario Shantanu Basu and Eduard Vorobyov Cores to Disks to Protostars: The Effect of the Core Envelope on Accretion and Disk.
Physics 778 – Star formation: Protostellar disks Ralph Pudritz.
Planetesimal dynamics in self-gravitating discs Giuseppe Lodato IoA - Cambridge.
Star forming regions in Orion. What supports Cloud Cores from collapsing under their own gravity? Thermal Energy (gas pressure) Magnetic Fields Rotation.
How Different was the Universe at z=1? Centre de Physique Théorique, Marseille Université de Provence Christian Marinoni.
AS 4002 Star Formation & Plasma Astrophysics Steady thin discs Suppose changes in external conditions are slower than t visc ~R 2 /. Set ∂/∂t=0 and integrate.
Evolved Protoplanetary Disks: The Multiwavelength Picture Aurora Sicilia-Aguilar Th. Henning, J. Bouwman, A. Juhász, V. Roccatagliata, C. Dullemond, L.
Processes in Protoplanetary Disks Phil Armitage Colorado.
Massive planets in FU Orionis objects Giuseppe Lodato Institute of Astronomy, Cambridge In collaboration with Cathie Clarke (IoA)
MOLECULAR HYDROGEN IN THE CIRCUMSTELLAR ENVIRONMENT OF HERBIG Ae/Be STARS Claire MARTIN 1 M. Deleuil 1, J-C. Bouret 1, J. Le Bourlot 2, T. Simon 3, C.
Day/night cold trap of TiO in hot Jupiters atmospheres Vivien Parmentier 1, Adam Showman 2, Tristan Guillot 1 1 Observatoire de la Côte d'Azur, Nice, France.
Matteo Cantiello Astronomical Institute Utrecht Binary star progenitors of long GRBs M. Cantiello, S.-C. Yoon, N. Langer, and M. Livio A&A 465, L29-L33.
Star and Planet Formation
Making Our Solar System: Planetary Formation and Evolution
Pre-Main-Sequence of A stars
Disk Structure and Evolution (the so-called a model of disk viscosity)
Can Giant Planet Form by Direct Gravitational Instability?
Mayer et al Viability of Giant Planet Formation by Direct Gravitational Instability Roman Rafikov (CITA)
Presentation transcript:

Long term evolution of circumstellar discs: DM Tau and GM Aur Ricardo Hueso (*) & Tristan Guillot Laboratoire Cassini, Observatoire de la Côte d’Azur, Nice, France (*) Now at: E.T.S. Ing. Ind. y Telecom. UPV, Bilbao, Spain Circumstellar disks & protoplanets, Nice, February 2003

Initial questions: Are models of star & disk formation able to compare with observations and give constraints on relevant disk physics? Numerous Parameterizations. How to set up values for the most relevant parameters? Circumstellar disks & protoplanets, Nice, February 2003 Is it viscous evolution the most important factor determining disk properties on the long term? Different models of turbulence a prescription, b prescription, Shear, convection, MRI, surface MRI, waves Statistics about protoplanetary disks begin to be available. Life-span, disk masses, star accretion rates with time … This work: Make simple models of disk formation & evolution and compare with available observations. Set up model parameters and test turbulence prescriptions.

Models of Disk Formation and Evolution Circumstellar disks & protoplanets, Nice, February 2003 PAREMETERS - T cloud - w cloud - M cloud - a, b Several long term simulations of DM Tau and GM Aur Compare with observations Fast 1D models Including gravitational collapse of rotating isothermal spheres: + Additional equations for disk properties + Simplified radiative transfer + Photoevaporation (Long term simulations) Viscous evolution + source terms

Two “models” of turbulence: a and b Non-Linear shear instability  n b = b ( d W/ dR ) R 3 Non-Linear shear instability  n b = b ( d W/ dR ) R 3 Not easy to study in numerical experiments!! Intensity from experiments in rotating tanks. b ~ 2 x Not easy to study in numerical experiments!! Intensity from experiments in rotating tanks. b ~ 2 x HCsCs Mixing-Length  n a = a c s H ~ r 3/4 Mixing-Length  n a = a c s H ~ r 3/4 Only a parameterization! Models of MRI a ~ Used also when considering others kind of mechanisms for the turbulence Only a parameterization! Models of MRI a ~ Used also when considering others kind of mechanisms for the turbulence  n a ~ r 3/4 n b ~ r ½  Are finally both parameterizations so different when applied?  n a ~ r 3/4 n b ~ r ½  Are finally both parameterizations so different when applied? Circumstellar disks & protoplanets, Nice, February 2003

Observational characteristics of DM Tau and GM Aur Guilloteau & Dutrey, 1998 Simon, Guilloteau & Dutrey, 2001 CO Maps of disk emission: Temperature and S retrievals Dust Maps of diffused light: S Retrievals Kitamura et al Spectral Energy Dist. (IR) Signatures of Star accretion Rate Hartmann et al Circumstellar disks & protoplanets, Nice, February 2003

Comparing model with DM Tau a = w cd = s -1 T cd = 10 K M 0 = 0.3 M  PAREMETERS Circumstellar disks & protoplanets, Nice, February 2003

Comparing model with DM Tau a = w cd = s -1 T cd = 10 K M 0 = 0.3 M  PAREMETERS Circumstellar disks & protoplanets, Nice, February 2003

Comparing model with DM Tau a = w cd = s -1 T cd = 10 K M 0 = 0.3 M  PAREMETERS n a =a c s H n b =b ( d W/ dR ) R 3 n a =a c s H n b =b ( d W/ dR ) R 3 Explore parameter space. Test parameterizations of turbulence Explore parameter space. Test parameterizations of turbulence Circumstellar disks & protoplanets, Nice, February 2003

Constraining model parameters: All Models Circumstellar disks & protoplanets, Nice, February 2003 Selecting models

All Models CO + Star age & mass Circumstellar disks & protoplanets, Nice, February 2003 Constraining model parameters: Selecting models

All Models CO + Star age & mass CO + Dust Circumstellar disks & protoplanets, Nice, February 2003 Constraining model parameters: Selecting models

All Models CO + Star age & mass CO + Dust CO + Dust + Accretion Rate Circumstellar disks & protoplanets, Nice, February 2003 Constraining model parameters: Selecting models

All Models CO + Star age & mass CO + Dust CO + Dust + Accretion Rate Circumstellar disks & protoplanets, Nice, February 2003 Constraining model parameters: Selecting models

Set of model parameters fitting the observational constraints: Circumstellar disks & protoplanets, Nice, February 2003 Practically a standard accretion disk.

Set of model parameters fitting the observational constraints: More mass is needed Less Turbulence Greater Temperature (15 K) (Faster early formation) Less dispersion with Temperature Circumstellar disks & protoplanets, Nice, February 2003

a vs. b : DM Tau & GM Aur b models behave globally like a models b models show bigger dispersion in turbulence  They have n almost unchanged in time while a models evolve from high turbulence to less turbulent stages. Circumstellar disks & protoplanets, Nice, February 2003 Knowing the data for the disk within an order of 5 doesn’t improve these plots. Iincertitudes come also from the assumed star age and its mass.

Conclusions Circumstellar disks & protoplanets, Nice, February 2003 Models of purely viscous discs are able to explain presently observed characteristics of circumstellar disks like DM Tau and GM Aur. We can obtain valuable information about the relevant parameters governing disk formation and evolution. Large incertitudes on the determination of physical properties. Results depends on assumptions such as CO depletion or dust abundance. Incertitudes give rise to one-two orders of magnitude indetermination of disk viscosity. Alpha an Beta parameterizations of turbulence work equally well (or bad) to fit the observations. GM Aur requires 10 times less turbulence than DM Tau. Consequence of a more massive disk combined with a lower accretion rate. Why? Simply more massive system, older, or... A procative posibility. Can this reduced “accretion” be interpreted in terms of an internal gap in GM Aur? SED of GM Aur seems to suggest a gap!