Extra-solar Weather. Ian Dobbs-Dixon. University of Washington, Seattle
|
|
- Kelley Fleming
- 6 years ago
- Views:
Transcription
1 Extra-solar Weather Ian Dobbs-Dixon University of Washington, Seattle
2 Outline Dynamical Modeling Methodologies Hydrodynamic Models Radiative Models Giant Planet Meteorology Thermal inversions Opacity variations Viscous effects Variability Vertical mixing efficiency Eccentric planets
3 Dynamical Methods Completeness Equivalent Barotropic and Shallow Water (2D) Cho et al (2003,2008) Langton and Laughlin (2007,2008) Rauscher et al (2007, 2008) Primitive equations (~3D) Showman et al. (2002, 2005, 2006, 2008, 2009), Menou and Rauscher (2009) Navier-Stokes equation (2D) Burkert et al Full Navier-Stokes equations (3D) Dobbs-Dixon et al (2008,2009) Resolution
4 Radiation Transfer Methods Completeness Relaxation methods (Newtonian heating) Cho et al (2003,2008) Langton and Laughlin (2007,2008) Rauscher et al (2007, 2008), Showman et al. (2002, 2005, 2006, 2008), Menou and Rauscher (2009) 2/3D one temperature flux-limited radiative diffusion Burkert et al. (2007), Dobbs-Dixon and Lin (2008) 3D FLD + decoupled thermal and radiative components Dobbs-Dixon et al (2009) 1D (radial) wavelength-dependent radiative transfer Showman et al. (2009)
5 3D Navier-Stokes, flux limited diffusion and decoupled thermal and radiative components
6 Absorption vs. Emission Opacities (κ * /κ P ) 1/4 T (K)
7 3D Flux-Limited Radiation Diffusion Slowly varying in space/time: F α λ( R) R Freedman et al. (2007) Accurate in the limits { Levermore & Pomraning (1981)
8 P rot =P orb =3.52d, Tstar=6117K
9 Photospheric Velocities
10 Observed Inversion (HD b) Burrows et al (2007)
11 Outer Temperature Structure Hubeny et al. (2003)
12 T-Profile Dichotomy? Fortney et al (2007)
13 HD209458b sub-solar anti-solar
14 Opacity Variations Zahnle et al 2009
15 Opacity Variations Freedman Opc κ Interstellar Opc Dobbs-Dixon and Lin (2007)
16 Opacity Variations Freedman Opc κ ~0 2.5km Interstellar Opc ~0 4.2km Dobbs-Dixon and Lin (2007)
17 10 12 cm 2 /s Viscosity Momentum eq cm 2 /s Add thermal and radiation energy equations ν Radiation determines behavior along streamlines 10 8 cm 2 /s
18 10 12 cm 2 /s Viscosity Momentum eq cm 2 /s Add thermal and radiation energy equations ν Radiation determines behavior along streamlines 10 8 cm 2 /s
19 Variability Grillmair et al 2009 Agol et al 2008 Madhusudhan and Seager 2009
20 Surface and radial shear v φ T (K) -4 km/s +4 km/s
21 Variability To To+0.5d To+1.0d To+1.5d
22 Variability Nick Cowan
23 Vertical Mixing Zahnle et al 2009 Fortney et al (2007)
24 Vertical Mixing K zz = V r,rms H p Spiegel et al (2007)
25 Eccentric Planets
26 Eccentric Planets
27 Eccentric Planets 3.52d
28 e=0.175 Eccentric Planets e=0.350 e=0.525 e=0.7
29 Conclusions Numerical treatment of radiation and dynamics must be included as coupled model Both opacity and dynamically derived temperature inversions play roles in dynamics and spectra. The location of stellar energy deposition governs efficiency of redistribution to the night-side Three jets (one equatorial and two mid-lat.) are common features, with width decreasing with increased planetary rotation Changing viscosity drastically alters streamlines, changing overall thermal structure Dynamically driven variability may cause variations transit spectra, but variation in hemispherically averaged phase curves will be difficult Vertical mixing throughout the atmosphere is significant. Potential for maintaining species aloft Continuing obs. programs, and coupling of dynamical/spectral models will allow tighter constraints on dynamical processes: eccentric planets, multiple (and continuous) observations, lower masses, younger planets, thermal forcing
30
Cloud Formation & Dynamics in Cool Stellar & Planetary Atmospheres
+ Cloud Formation & Dynamics in Cool Stellar & Planetary Atmospheres Adam J. Burgasser UC San Diego/MIT + Clouds are a universal characteristic of low temperature stars/brown dwarfs (particularly L dwarfs),
More informationarxiv: v1 [astro-ph.ep] 6 Jan 2010
Radiative Hydrodynamic Simulations of HD209458b: Temporal Variability Ian Dobbs-Dixon 1,2, Andrew Cumming 1, D.N.C Lin 3,4 1 Department of Physics, McGill University, Montreal, H3A 2T8 Canada 2 Department
More informationExoplanetary Atmospheres: Temperature Structure of Irradiated Planets. PHY 688, Lecture 23 Mar 20, 2009
Exoplanetary Atmospheres: Temperature Structure of Irradiated Planets PHY 688, Lecture 23 Mar 20, 2009 Outline Review of previous lecture hot Jupiters; transiting planets primary eclipses and atmospheric
More informationExoplanetary Atmospheres: Atmospheric Dynamics of Irradiated Planets. PHY 688, Lecture 24 Mar 23, 2009
Exoplanetary Atmospheres: Atmospheric Dynamics of Irradiated Planets PHY 688, Lecture 24 Mar 23, 2009 Outline Review of previous lecture: atmospheric temperature structure of irradiated planets isothermal
More informationAtmospheric Circulation of Eccentric Extrasolar Giant Planets
Atmospheric Circulation of Eccentric Extrasolar Giant Planets Item Type text; Electronic Dissertation Authors Lewis, Nikole Kae Publisher The University of Arizona. Rights Copyright is held by the author.
More informationhd b greg laughlin jonathan langton ucsc
hd 80606 b greg laughlin jonathan langton ucsc The success of the planet detection programs has enabled the comparative study of populations of planets, as well as the detailed investigation of individual
More informationATMOSPHERIC DYNAMICS OF SHORT-PERIOD EXTRASOLAR GAS GIANT PLANETS. I. DEPENDENCE OF NIGHTSIDE TEMPERATURE ON OPACITY
The Astrophysical Journal, 673:513 525, 2008 January 20 # 2008. The American Astronomical Society. All rights reserved. Printed in U.S.A. ATMOSPHERIC DYNAMICS OF SHORT-PERIOD EXTRASOLAR GAS GIANT PLANETS.
More informationStrong water absorption in the dayside emission spectrum of the planet HD b
1 Strong water absorption in the dayside emission spectrum of the planet HD 189733b Carl J. Grillmair 1, Adam Burrows 2, David Charbonneau 3, Lee Armus 1, John Stauffer 1, Victoria Meadows 4, Jeffrey van
More informationAtmospheric Dynamics of Exoplanets: Status and Opportunities
Atmospheric Dynamics of Exoplanets: Status and Opportunities Adam Showman University of Arizona Collaborators: Jonathan Fortney, Lorenzo Polvani, Yuan Lian, Mark Marley, Nikole Lewis, Daniel Perez-Becker,
More informationMAGNETOHYDRODYNAMIC SIMULATIONS OF THE ATMOSPHERE OF HD209458B
Draft version April 11, 2018 Preprint typeset using L A TEX style emulateapj v. 5/2/11 MAGNETOHYDRODYNAMIC SIMULATIONS OF THE ATMOSPHERE OF HD209458B T.M. Rogers Department of Planetary Sciences, University
More informationON THE SURFACE HEATING OF SYNCHRONOUSLY SPINNING SHORT-PERIOD JOVIAN PLANETS
The Astrophysical Journal, 618:512 523, 2005 January 1 # 2005. The American Astronomical Society. All rights reserved. Printed in U.S.A. ON THE SURFACE HEATING OF SYNCHRONOUSLY SPINNING SHORT-PERIOD JOVIAN
More informationPlanetary Atmospheres. Structure Composition Clouds Photochemistry Meteorology Atmospheric Escape
Planetary Atmospheres Structure Composition Clouds Photochemistry Meteorology Atmospheric Escape Photochemistry We can characterize chemical reactions in the atmosphere in the following way: 1. Photolysis:
More informationAstronomy. Astrophysics. 3D mixing in hot Jupiters atmospheres. I. Application to the day/night cold trap in HD b
A&A 558, A9 (23) DOI:.5/4-636/23232 c ESO 23 Astronomy & Astrophysics 3D mixing in hot Jupiters atmospheres I. Application to the day/night cold trap in HD 29458b Vivien Parmentier,AdamP.Showman 2, and
More informationAdam Burrows, Princeton April 7, KITP Public Lecture
Adam Burrows, Princeton April 7, 2010 KITP Public Lecture The Ancient History of Comparative Planetology There are infinite worlds both like and unlike this world of ours...we must believe that in all
More informationOpacity and Optical Depth
Opacity and Optical Depth Absorption dominated intensity change can be written as di λ = κ λ ρ I λ ds with κ λ the absorption coefficient, or opacity The initial intensity I λ 0 of a light beam will be
More informationMagnetic Induction in Hot Jupiter Atmospheres
Magnetic Induction in Hot Jupiter Atmospheres University of Toronto May 12 th, 2010 Outline An Overview of Extra solar Giant Planets Hot Jupiter General Circulation in the Atmosphere Preliminaries: Ionization,
More informationDoppler Signatures of the Atmospheric Circulation on Hot Jupiters
Submitted to ApJ Doppler Signatures of the Atmospheric Circulation on Hot Jupiters Adam P. Showman 1, Jonathan J. Fortney 2, Nikole K. Lewis 1, and Megan Shabram 3 ABSTRACT The meteorology of hot Jupiters
More informationOn the radiative equilibrium of irradiated planetary atmospheres
On the radiative equilibrium of irradiated planetary atmospheres Tristan Guillot To cite this version: Tristan Guillot. On the radiative equilibrium of irradiated planetary atmospheres. Astronomy and Astrophysics
More informationExoplanet Forum: Transit Chapter
Exoplanet Forum: Transit Chapter A condensed version of the Transits Chapter from the Exoplanet Forum Proceedings, made available to the Decadal Survey, Planetary Systems and Star Formation Panel Drake
More informationarxiv: v1 [astro-ph.ep] 9 Oct 2014
Draft version March 24, 219 Preprint typeset using L A TEX style emulateapj v. 12/16/11 THE ATMOSPHERIC CIRCULATION OF THE HOT JUPITER WASP-43B: COMPARING THREE-DIMENSIONAL MODELS TO SPECTROPHOTOMETRIC
More informationDOPPLER SIGNATURES OF THE ATMOSPHERIC CIRCULATION ON HOT JUPITERS
Submitted to ApJ Preprint typeset using L A TEX style emulateapj v. 08/13/06 DOPPLER SIGNATURES OF THE ATMOSPHERIC CIRCULATION ON HOT JUPITERS Adam P. Showman 1, Jonathan J. Fortney 2, Nikole K. Lewis
More informationCharacterization of Transiting Planet Atmospheres
Characterization of Transiting Planet Atmospheres Heather Knutson Division of Geological and Planetary Sciences, Caltech A Bird s-eye View of Exoplanet Atmospheres Limited information available for individual
More informationarxiv: v2 [astro-ph.ep] 9 Sep 2016
Astronomy & Astrophysics manuscript no. the_met_office_um_applied_to_hot_jupiters ESO 2016 September 13, 2016 The UK Met Office GCM with a sophisticated radiation scheme applied to the hot Jupiter HD 209458b
More informationThe atmosphere of Exoplanets AND Their evolutionary properties. I. Baraffe
The atmosphere of Exoplanets AND Their evolutionary properties I. Baraffe I) Properties of cool atmospheres: 1) Atmospheric chemistry 2) Main opacity sources 3) Non solar composition 4) Non equilibrium
More informationNUMERICAL METHODS IN ASTROPHYSICS An Introduction
-1 Series in Astronomy and Astrophysics NUMERICAL METHODS IN ASTROPHYSICS An Introduction Peter Bodenheimer University of California Santa Cruz, USA Gregory P. Laughlin University of California Santa Cruz,
More informationarxiv: v2 [astro-ph.ep] 2 Oct 2018
Exoplanet phase curves: observations and theory Vivien Parmentier and Ian J. M. Crossfield arxiv:1711.07696v2 [astro-ph.ep] 2 Oct 2018 Abstract Phase curves are the best technique to probe the three dimensional
More informationSubstellar Atmospheres II. Dust, Clouds, Meteorology. PHY 688, Lecture 19 Mar 11, 2009
Substellar Atmospheres II. Dust, Clouds, Meteorology PHY 688, Lecture 19 Mar 11, 2009 Outline Review of previous lecture substellar atmospheres: opacity, LTE, chemical species, metallicity Dust, Clouds,
More informationProtoplanetary Disks. Ernst Dorfi WS 2012
Protoplanetary Disks Ernst Dorfi WS 2012 Disks and star formation Disks of gas and dust are observed around young stars for about 107 years Disks form because of angular momentum (conservation), collapse
More informationModeling of Jupiter s stratosphere: new radiation code and impacts on the dynamics
Symposium on Planetary Science 2015, 2015/02/16, Tohoku Univ. Modeling of Jupiter s stratosphere: new radiation code and impacts on the dynamics Takeshi Kuroda Tohoku University A.S. Medvedev, J. Sethunadh,
More informationarxiv: v1 [astro-ph.ep] 19 Feb 2010
Draft version October 30, 018 Preprint typeset using L A TEX style emulateapj v. 11/10/09 INFLATING HOT JUPITERS WITH OHMIC DISSIPATION Konstantin Batygin & David J. Stevenson Division of Geological and
More informationAtmospheric Circulation of Hot Jupiters: A Review of Current Understanding
EXTREME SOLAR SYSTEMS ASP Conference Series, Vol. 398, c 2008 D. Fischer, F. A. Rasio, S. E. Thorsett, and A. Wolszczan, eds. Atmospheric Circulation of Hot Jupiters: A Review of Current Understanding
More informationTHE INFLUENCE OF ATMOSPHERIC DYNAMICS ON THE INFRARED SPECTRA AND LIGHT CURVES OF HOT JUPITERS
The Astrophysical Journal, 652:746Y757, 2006 November 20 # 2006. The American Astronomical Society. All rights reserved. Printed in U.S.A. THE INFLUENCE OF ATMOSPHERIC DYNAMICS ON THE INFRARED SPECTRA
More informationarxiv: v2 [astro-ph.ep] 11 Feb 2015
ApJ, in press Preprint typeset using L A TEX style emulateapj v. 5/2/11 THREE-DIMENSIONAL ATMOSPHERIC CIRCULATION OF WARM AND HOT JUPITERS: EFFECTS OF ORBITAL DISTANCE, ROTATION PERIOD, AND NON-SYNCHRONOUS
More informationDOPPLER SIGNATURES OF THE ATMOSPHERIC CIRCULATION ON HOT JUPITERS
ApJ, accepted and published Preprint typeset using L A TEX style emulateapj v. 5/2/11 DOPPLER SIGNATURES OF THE ATMOSPHERIC CIRCULATION ON HOT JUPITERS Adam P. Showman 1, Jonathan J. Fortney 2, Nikole
More informationEART164: PLANETARY ATMOSPHERES
EART164: PLANETARY ATMOSPHERES Francis Nimmo Last Week Radiative Transfer Black body radiation, Planck function, Wien s law Absorption, emission, opacity, optical depth Intensity, flux Radiative diffusion,
More informationVII. Hydrodynamic theory of stellar winds
VII. Hydrodynamic theory of stellar winds observations winds exist everywhere in the HRD hydrodynamic theory needed to describe stellar atmospheres with winds Unified Model Atmospheres: - based on the
More informationarxiv: v1 [astro-ph.ep] 3 Mar 2019
Draft version March 5, 2019 Typeset using L A TEX twocolumn style in AASTeX62 Atmospheres on Nonsynchronized Eccentric-tilted Exoplanets I: Dynamical Regimes Kazumasa Ohno 1 and Xi Zhang 2 1 Department
More information50F-1650, 1 Cyclotron Rd, Berkeley, CA , USA
Irradiated Planets Peter H. Hauschildt 1, Travis Barman 2 and E. Baron 3,4 1 Hamburger Sternwarte, Gojenbergsweg 112, 21029 Hamburg, Germany 2 Lowell Observatory, Hendricks Center for Planetary Studies,
More informationarxiv: v2 [astro-ph.ep] 29 Sep 2014
Draft version April 17, 2018 Preprint typeset using L A TEX style emulateapj v. 5/2/11 THE 4.5 µm FULL-ORBIT PHASE CURVE OF THE HOT JUPITER HD 209458B arxiv:1405.5923v2 [astro-ph.ep] 29 Sep 2014 Robert
More information3D MODELING OF SPECTRA AND LIGHT CURVES OF HOT JUPITERS WITH PHOENIX; A FIRST APPROACH
Revista Mexicana de Astronomía y Astrofísica, 52, 69 82 (2016) 3D MODELING OF SPECTRA AND LIGHT CURVES OF HOT JUPITERS WITH PHOENIX; A FIRST APPROACH Juan J. Jiménez-Torres Hamburger Sternwarte, Gojenbergsweg
More informationExoplanetary Atmospheres
Exoplanetary Atmospheres Nikku Madhusudhan 1,2, Heather Knutson 3, Jonathan J. Fortney 4, Travis Barman 5,6 The study of exoplanetary atmospheres is one of the most exciting and dynamic frontiers in astronomy.
More informationarxiv:astro-ph/ v2 28 Feb 2005
Astronomy & Astrophysics manuscript no. iro article November 14, 2018 (DOI: will be inserted by hand later) A Time-Dependent Radiative Model of HD209458b arxiv:astro-ph/0409468v2 28 Feb 2005 N. Iro, B.
More informationarxiv: v1 [astro-ph.ep] 1 Jun 2017
Draft version June 1, 218 1 Preprint typeset using L Space Telescope Science A TEX style emulateapj v. 1/23/15 Institute, Baltimore, MD 21218, USA; ATMOSPHERIC CIRCULATION AND CLOUD EVOLUTION ON THE HIGHLY
More informationExoplanets Atmospheres. Characterization of planetary atmospheres. Photometry of planetary atmospheres from direct imaging
Photometry of planetary atmospheres from direct imaging Exoplanets Atmospheres Planets and Astrobiology (2016-2017) G. Vladilo Example: planetary system detected with direct imaging HR 8799 b, c, d (Marois
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 informationSIMPLE RADIATIVE TRANSFER
ASTR 511/O Connell Lec 4 1 SIMPLE RADIATIVE TRANSFER The theory of radiative transfer provides the means for determining the emergent EM spectrum of a cosmic source and also for describing the effects
More informationPlanetary Atmospheres
Planetary Atmospheres Structure Composition Clouds Meteorology Photochemistry Atmospheric Escape EAS 4803/8803 - CP 11:1 Structure Generalized Hydrostatic Equilibrium P( z) = P( 0)e z # ( ) " dr / H r
More informationEnergy transport: convection
Outline Introduction: Modern astronomy and the power of quantitative spectroscopy Basic assumptions for classic stellar atmospheres: geometry, hydrostatic equilibrium, conservation of momentum-mass-energy,
More informationThe hottest hot Jupiters may host atmospheric dynamos
The hottest hot Jupiters may host atmospheric dynamos T.M. Rogers Department of Mathematics and Statistics, Newcastle University, UK Planetary Science Institute, Tucson, AZ 85721, USA J.N.McElwaine arxiv:1704.04197v1
More informationH 2 OABUNDANCESINTHEATMOSPHERESOFTHREEHOTJUPITERS
To be published in The Astrophysical Journal Letters on July 24, 2014 Preprint typeset using L A TEX styleemulateapjv.2/16/10 H 2 OABUNDANCESINTHEATMOSPHERESOFTHREEHOTJUPITERS Nikku Madhusudhan 1,NicolasCrouzet
More informationarxiv: v1 [astro-ph.ep] 13 Jul 2012
DRAFT VERSION SEPTEMBER 18, 018 Preprint typeset using LATEX style emulateapj v. 5//11 OHMIC DISSIPATION IN THE INTERIORS OF HOT JUPITERS XU HUANG 1 AND ANDREW CUMMING Draft version September 18, 018 arxiv:107.378v1
More informationarxiv: v1 [astro-ph.ep] 22 Nov 2018
SF2A 18 P. Di Matteo, F. Billebaud, F. Herpin, N. Lagarde, J.-B. Marquette, A. Robin, O. Venot (eds) CONSEQUENCES OF SEMIDIURNAL THERMAL TIDES ON HOT JUPITERS ZONAL MEAN FLOWS P. Auclair-Desrotour 1 and
More informationObservations of Extrasolar Planets During the non-cryogenic Spitzer Space Telescope Mission
Observations of Extrasolar Planets During the non-cryogenic Spitzer Space Telescope Mission Drake Deming, Eric Agol, David Charbonneau, Nicolas Cowan, Heather Knutson and Massimo Marengo NASA s Goddard
More informationarxiv: v2 [astro-ph.ep] 7 Nov 2014
Astronomy & Astrophysics manuscript no. Parmentier24c c ESO 24 November, 24 A non-grey analytical model for irradiated atmospheres. II: Analytical vs. numerical solutions Vivien Parmentier,2,3, Tristan
More informationSearching for Other Worlds: The Methods
Searching for Other Worlds: The Methods John Bally 1 1 Center for Astrophysics and Space Astronomy Department of Astrophysical and Planetary Sciences University of Colorado, Boulder The Search Extra-Solar
More information1. Weather and climate.
Lecture 31. Introduction to climate and climate change. Part 1. Objectives: 1. Weather and climate. 2. Earth s radiation budget. 3. Clouds and radiation field. Readings: Turco: p. 320-349; Brimblecombe:
More informationTHEORETICAL SPECTRA AND LIGHT CURVES OF CLOSE-IN EXTRASOLAR GIANT PLANETS AND COMPARISON WITH DATA
The Astrophysical Journal, 678:1436Y1457, 2008 May 10 # 2008. The American Astronomical Society. All rights reserved. Printed in U.S.A. A THEORETICAL SPECTRA AND LIGHT CURVES OF CLOSE-IN EXTRASOLAR GIANT
More informationWP the Mass-Radius relationship for gas giants
WP 115 100 the Mass-Radius relationship for gas giants Tristan Guillot, Mathieu Havel Observatoire de la Côte d'azur, CNRS UMR 6202 Objectives: Understand the expected impact of PLATO photometry on the
More informationRadiative transfer in planetary atmospheres
Chapter 9 Radiative transfer in planetary atmospheres Warning: This chapter is just a very rough introduction to planetary atmospheres. Since the discovery of planets around other stars than the sun, the
More informationRadiative Heat Balances in Jupiter s Stratosphere: Development of a Radiation Code for the Implementation to a GCM
Radiative Heat Balances in Jupiter s Stratosphere: Development of a Radiation Code for the Implementation to a GCM T. Kuroda Tohoku University A.S. Medvedev, P. Hartogh Max Planck Institute for Solar System
More informationCollisions and transport phenomena
Collisions and transport phenomena Collisions in partly and fully ionized plasmas Typical collision parameters Conductivity and transport coefficients Conductivity tensor Formation of the ionosphere and
More informationPlanetary Upper Atmospheres Under Strong XUV radiation
Planetary Upper Atmospheres Under Strong XUV radiation Feng Tian Laboratory for Atmosphere and Space Physics University of Colorado at Boulder March 4 th, 2010 Outline Early Solar XUV radiation was strong.
More informationProbing the extreme planetary atmosphere of WASP-12b
Probing the extreme planetary atmosphere of WASP-12b Mark Swain, Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA Pieter Deroo, Jet Propulsion
More informationLimb Darkening. Limb Darkening. Limb Darkening. Limb Darkening. Empirical Limb Darkening. Betelgeuse. At centre see hotter gas than at edges
Limb Darkening Sun Betelgeuse Limb Darkening Stars are both redder and dimmer at the edges Sun Limb Darkening Betelgeuse Limb Darkening Can also be understood in terms of temperature within the solar photosphere.
More informationRadiative Transfer Plane-Parallel Frequency-Dependent
4 Radiative Transfer Plane-Parallel Frequency-Dependent variables I ν J ν H ν K ν in astronomy 4. Basic Equations After Fukue, J. 2, PASJ, 63, in press We here assume the followings: i) The disk is steady
More informationEquatorial Superrotation on Tidally Locked Exoplanets
Equatorial Superrotation on Tidally Locked Exoplanets Adam P. Showman University of Arizona Lorenzo M. Polvani Columbia University Synopsis Most 3D atmospheric circulation models of tidally locked exoplanets
More informationEvolution of protoplanetary discs
Evolution of protoplanetary discs and why it is important for planet formation Bertram Bitsch Lund Observatory April 2015 Bertram Bitsch (Lund) Evolution of protoplanetary discs April 2015 1 / 41 Observations
More informationImperial College London
Solar Influence on Stratosphere-Troposphere Dynamical Coupling Isla Simpson, Joanna D. Haigh, Space and Atmospheric Physics, Imperial College London Mike Blackburn, Department of Meteorology, University
More informationThermal structure of an exoplanet atmosphere from phase-resolved emission spectroscopy
Thermal structure of an exoplanet atmosphere from phase-resolved emission spectroscopy Kevin B. Stevenson 1,13, Jean-Michel Désert 2, Michael R. Line 3, Jacob L. Bean 1, Jonathan J. Fortney 3, Adam P.
More information3D MODELING OF GJ1214B S ATMOSPHERE: FORMATION OF INHOMOGENEOUS HIGH CLOUDS AND OBSERVATIONAL IMPLICATIONS
Draft version October 7, Preprint typeset using L A TEX style emulateapj v. // D MODELING OF GJB S ATMOSPHERE: FORMATION OF INHOMOGENEOUS HIGH CLOUDS AND OBSERVATIONAL IMPLICATIONS B. Charnay,,, V. Meadows,,
More informationarxiv: v2 [astro-ph.ep] 21 May 2010
Day-side z band emission and eccentricity of WASP-12b 1 Mercedes López-Morales 2,4, Jeffrey L. Coughlin 3,5, David K. Sing 6, Adam Burrows 7, Dániel Apai 8, Justin C. Rogers 4,9, David S. Spiegel 7 & Elisabeth
More informationScience with Transiting Planets TIARA Winter School on Exoplanets 2008
Science with Transiting Planets TIARA Winter School on Exoplanets 2008 Eric Agol University of Thanks to Josh Winn for slides 1 Venusian transit 2004 August 6, 2004 from Slovenia (Lajovic et al.) 2 History
More information2. Meridional atmospheric structure; heat and water transport. Recall that the most primitive equilibrium climate model can be written
2. Meridional atmospheric structure; heat and water transport The equator-to-pole temperature difference DT was stronger during the last glacial maximum, with polar temperatures down by at least twice
More informationno eddies eddies Figure 3. Simulated surface winds. Surface winds no eddies u, v m/s φ0 =12 φ0 =0
References Held, Isaac M., and Hou, A. Y., 1980: Nonlinear axially symmetric circulations in a nearly inviscid atmosphere. J. Atmos. Sci. 37, 515-533. Held, Isaac M., and Suarez, M. J., 1994: A proposal
More informationBrown dwarfs and hot young planets
Brown dwarfs and hot young planets D. Saumon Los Alamos National Laboratory Images: Cassini; Marois et al. (2008) 2009 Sagan Exoplanet Summer Workshop, 21 July 2009 LA-UR-09-04365 Brown dwarfs and hot
More informationMA3D1 Fluid Dynamics Support Class 5 - Shear Flows and Blunt Bodies
MA3D1 Fluid Dynamics Support Class 5 - Shear Flows and Blunt Bodies 13th February 2015 Jorge Lindley email: J.V.M.Lindley@warwick.ac.uk 1 2D Flows - Shear flows Example 1. Flow over an inclined plane A
More informationAtmospheres and evaporation of extrasolar planets
Atmospheres and evaporation of extrasolar planets Alain Lecavelier des Etangs Institut d Astrophysique de Paris Une planète s évapore ESLAB ESTEC 29 mai 2007 Absorption spectroscopy during transits Light
More informationPlanetary interiors: What they can(not) tell us about formation
Planetary interiors: What they can(not) tell us about formation Methods and constraints Jérémy Leconte Timeline Formation ( 1-10 Myr) Mass Radius Orbital Parameters Stellar Parameters... Evolution ( 1-10
More information3. FORMS OF GOVERNING EQUATIONS IN CFD
3. FORMS OF GOVERNING EQUATIONS IN CFD 3.1. Governing and model equations in CFD Fluid flows are governed by the Navier-Stokes equations (N-S), which simpler, inviscid, form is the Euler equations. For
More informationSubstellar Atmospheres. PHY 688, Lecture 18 Mar 9, 2009
Substellar Atmospheres PHY 688, Lecture 18 Mar 9, 2009 Outline Review of previous lecture the Kepler mission launched successfully results P < 1 month planets by September 09 giant planet interiors comparison
More informationPlanetary Atmospheres
Planetary Atmospheres Structure Composition Clouds Meteorology Photochemistry Atmospheric Escape EAS 4803/8803 - CP 17:1 Structure Generalized Hydrostatic Equilibrium P( z) = P( 0)e z # ( ) " dr / H r
More informationRadiation from planets
Chapter 4 Radiation from planets We consider first basic, mostly photometric radiation parameters for solar system planets which can be easily compared with existing or future observations of extra-solar
More informationExo-Cartography (Mapping the Climate and Oceans of Exoplanets)
Exo-Cartography (Mapping the Climate and Oceans of Exoplanets) Nick Cowan CIERA Postdoctoral Fellow Northwestern University May 17, 2011 What I Won t Talk About Pallé et al. (2009) May 17, 2011 Nick Cowan's
More informationarxiv: v2 [astro-ph.ep] 18 Feb 2016
Submitted to The Astrophysical Journal Preprint typeset using L A TEX style emulateapj v. /2/11 ATMOSPHERIC CIRCULATION OF HOT JUPITERS: DAYSIDE-NIGHTSIDE TEMPERATURE DIFFERENCES Thaddeus D. Komacek 1
More informationEvolution Beyond the Red Giants
Evolution Beyond the Red Giants Interior Changes Sub-giant star 1 Post-Helium Burning What happens when there is a new core of non-burning C and O? 1. The core must contract, which increases the pressure
More informationThe diversity of exoplanet bulk compositions: Modelling structure and evolution of (exo)planets! I. Baraffe (University of Exeter)
The diversity of exoplanet bulk compositions: Modelling structure and evolution of (exo)planets I. Baraffe (University of Exeter) The fact: Huge diversity of bulk compositions according to the massradius
More informationExtrasolar Transiting Planets: Detection and False Positive Rejection
4 Harvard-Smithsonian Center for Astrophysics Extrasolar Transiting Planets: Detection and False Positive Rejection Willie Torres Harvard-Smithsonian Center for Astrophysics Young Planetary Systems Workshop
More informationADVECTION OF POTENTIAL TEMPERATURE IN THE ATMOSPHERE OF IRRADIATED EXOPLANETS: A ROBUST MECHANISM TO EXPLAIN RADIUS INFLATION
Draft version October 15, 218 Preprint typeset using L A TEX style AASTeX6 v. 1. ADVECTION OF POTENTIAL TEMPERATURE IN THE ATMOSPHERE OF IRRADIATED EXOPLANETS: A ROBUST MECHANISM TO EXPLAIN RADIUS INFLATION
More informationTransit Spectroscopy Jacob Bean
Transit Spectroscopy Jacob Bean University of Chicago Some recent reviews: Exoplanetary Atmospheres Chemistry, Forma6on Condi6ons, and Habitability Madhusudhan+ 2016 Observa6ons of Exoplanet Atmospheres
More informationDifferential Rotation and Emerging Flux in Solar Convective Dynamo Simulations
Differential Rotation and Emerging Flux in Solar Convective Dynamo Simulations Yuhong Fan (HAO/NCAR), Fang Fang (LASP/CU) GTP workshop August 17, 2016 The High Altitude Observatory (HAO) at the National
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 informationResearch paper assignment
Research paper assignment Review of research that interests you, more focused than discussions in class Include references and figures Final format should be PDF (try LaTeX!) Concise! < 5000 words Steps:
More informationTurbulence models and excitation of solar oscillation modes
Center for Turbulence Research Annual Research Briefs Turbulence models and excitation of solar oscillation modes By L. Jacoutot, A. Wray, A. G. Kosovichev AND N. N. Mansour. Motivation and objectives
More informationarxiv: v1 [astro-ph.ep] 13 Jan 2010
Accepted for publication in The Astrophysical Journal Thermal Emission and Tidal Heating of the Heavy and Eccentric Planet XO-3b arxiv:1001.2319v1 [astro-ph.ep] 13 Jan 2010 Pavel Machalek 1,2, Tom Greene
More informationStars AS4023: Stellar Atmospheres (13) Stellar Structure & Interiors (11)
Stars AS4023: Stellar Atmospheres (13) Stellar Structure & Interiors (11) Kenneth Wood, Room 316 kw25@st-andrews.ac.uk http://www-star.st-and.ac.uk/~kw25 What is a Stellar Atmosphere? Transition from dense
More informationCarbon- rich Exoplanets
Carbon- rich Exoplanets Nikku Madhusudhan Princeton University Exploring Strange New Worlds: From Giant Planets to Super Earths Flagstaff, AZ. May 04, 2011 Overview 1. WASP-12b and the need for a second
More informationSolar surface rotation
Stellar rotation Solar surface rotation Solar nearsurface rotation Surface Doppler Schou et al. (1998; ApJ 505, 390) Rotational splitting Inferred solar internal rotation Near solidbody rotation of interior
More informationAccretion disks. AGN-7:HR-2007 p. 1. AGN-7:HR-2007 p. 2
Accretion disks AGN-7:HR-2007 p. 1 AGN-7:HR-2007 p. 2 1 Quantitative overview Gas orbits in nearly circular fashion Each gas element has a small inward motion due to viscous torques, resulting in an outward
More informationThe Planetary Circulation System
12 The Planetary Circulation System Learning Goals After studying this chapter, students should be able to: 1. describe and account for the global patterns of pressure, wind patterns and ocean currents
More informationDirect imaging of extra-solar planets
Chapter 6 Direct imaging of extra-solar planets Direct imaging for extra-solar planets means that emission from the planet can be spatially resolved from the emission of the bright central star The two
More information