2018 TIARA Summer School Origins of the Solar System. Observations and Modelling of Debris Disks. J.P. Marshall (ASIAA) Wednesday 18 th July 2018

Size: px
Start display at page:

Download "2018 TIARA Summer School Origins of the Solar System. Observations and Modelling of Debris Disks. J.P. Marshall (ASIAA) Wednesday 18 th July 2018"

Transcription

1 2018 TIARA Summer School Origins of the Solar System Observations and Modelling of Debris Disks J.P. Marshall (ASIAA) Wednesday 18 th July 2018

2

3 [Hogerheijde 1998]

4 Debris disks Tenuous belts of icy and rocky material left over from planet formation processes Observed at far-infrared wavelengths around ~ 15 30% of main sequence A K stars, lower at mid-infrared wavelengths (~ 2%) Detection limits strongly biased by limited instrument sensitivity, age and distance of host stars

5 [Eiroa et al. 2013; Thureau et al. 2014; Montesinos et al. 2016; Sibthorpe et al. 2018]

6 Reprocessing starlight We assume that the dust is in thermal equilibrium with incident starlight emits radiation as a blackbody L = 4πR 2 σt 4 F = L /4πa d 2 a d L d = F = 4πR d2 σt d 4 a d = (T d /278) -2 (L /L ) 0.25

7 Hot dust Asteroid belt Edgeworth-Kuiper belt Halo Comets Exoplanets(?) T [K] R [au] [Su & Rieke 2014]

8 Spectral energy distribution (SED)

9 Dust temperature [Morales et al. 2011]

10 [Wyatt 2018]

11 Architectures of planetary systems

12 Disk structures Resolved imaging of debris disks reveals their radii > R bb Also non-axisymmetric structure, e.g. warps, clumps, brightness asymmetries Indicative of dynamical interaction of dust with planets/ism Different wavelengths probe different dust temperatures and sizes; multi-wavelength imaging vital to break degeneracy

13 Scattered light [Wyatt 2008]

14 Sub-millimetre [Holland et al. 2017]

15 Millimetre

16 Realistic dust models (modified) blackbody models contain no physics. more advanced models, including realistic dust optical properties and size distributions allow physical interpretation and comparison simple disc power law model defined by six parameters: a min, a max, γ, R in, dr, α.

17 log linear

18 Spectral energy distribution (SED) Temperature Inner radius Minimum grain size Grain size distribution [Marshall et al. in prep.]

19 Dust grain size vs stellar luminosity [Pawellek & Krivov 2015]

20 Disc size vs stellar luminosity [Pawellek et al. 2014, Pawellek & Krivov 2015]

21 Size distribution of dust [Macgregor et al. 2016]

22 Dust mass, CO emission [Wyatt 2018]

23 Disk radius vs stellar luminosity [Matra et al. 2018]

24 [Schneider et al. 2014]

25 Mid-infrared spectral features Mid-infrared spectral features from debris dust are rare Absence of features implies absence of small (warm) dust grains in those discs These features are one of the few probes of the composition of larger bodies (i.e. planets!)

26 Mid-infrared spectral features [Beichman et al. 2005]

27 [Lisse et al. 2012]

28 [Johnson et al. 2012]

29 Molecular gas in debris disks One of the more exciting findings of debris disk observations in the recent years Around a dozen stars have been identified with mm-wavelength CO emission but only in young A and early F type stars Evidence of cometary activity around the star Molecular gas offers constraint on the volatile content of planetesimals and disk chemistry

30 Continuum [Marino et al. 2016]

31 [Dent et al. 2016]

32 [Matra et al. 2017]

33 Disks & Exoplanets Planetary companions leave scars on planetesimal disks! Dust trapping in resonances revealed by clumps in mm imaging* Resolved disk structure, but also radial extent vs age reveals influence of companion(s) Disk-planet interactions probe regions of m plt a plt space closed to other detection methods

34 Planet-bearing stars: 28/99 = 28±5% with disks No known planets: 43/203 = 21±3% with disks Debris disk luminosity is correlated with the presence of known planets at >99% significance. [Marshall et al. 2014; Matthews et al. 2014; Meshkat et al. 2017]

35 i = 0 d i = 0 i = 90 d i = 9 0 [Greaves et al. 2014]

36 [Marois et al. 2010; Booth et al. 2016; Wilner et al. 2018] [Jason Wang]

37 [Lagrange et al. 2012] [Jason Wang]

38 Disc-planet interaction [Moor et al. 2015; Vican et al. 2016]

39 Time variability Continuum emission disc brightnesses observed to decay on timescale of years Scattered light dust clumps in disc of AU Mic observe to migrate outward Spectral features time (and depth) variability of circumstellar absorption in Ca II H&K feature seen for several stars

40 Continuum emission [Melis et al. 2012]

41 [Meng et al. 2014]

42 Scattered light [Boccaletti et al. 2018]

43 Spectral features [Kiefer et al. 2014]

44 [Beust et al. 1994]

45 [Kiefer et al. 2014]

46 The Solar system [JPL Minor Planet Center]

47 Questions? Debris discs around mature, sun-like stars are a visible remnant of planet formation The properties and composition of the dust are measured through images, photometry, spectra, and polarisation Spatially resolved imaging and broadband photometry provide complementary details for dust modelling Planets can influence the location and motion of the dust, revealing themselves through indirect measurements But: not every disc structure is real, or requires planets! Combining our knowledge of planets, debris and their host stars leads to a greater understanding of the outcomes of the planet formation process

48 Literature Wyatt, M.C., 2008, Annual Reviews of Astronomy and Astrophysics Krivov, A.V., 2010, Research in Astronomy and Astrophysics Matthews, B., et al., 2014, in proceedings of Protostars & Planets V

49 Dust mass Planetesimal strength Radial width Mass Semi-major axis Exoplanets Continuum emission Radial extent Dynamics Eccentricity Temperature Mid-infrared features Self-stirring Size distribution Composition Debris Disks Minimum grain size Dust shape Albedo Optical depth Comets Gas Scattered light Stellar wind Star Age Inclination Spectral lines Time variability Temperature Mass

Detectability of extrasolar debris. Mark Wyatt Institute of Astronomy, University of Cambridge

Detectability of extrasolar debris. Mark Wyatt Institute of Astronomy, University of Cambridge Detectability of extrasolar debris Mark Wyatt Institute of Astronomy, University of Cambridge Why image extrasolar debris? Emission spectrum shows dust thermal emission, used to infer radius of parent

More information

Debris discs, exoasteroids and exocomets. Mark Wyatt Institute of Astronomy, University of Cambridge

Debris discs, exoasteroids and exocomets. Mark Wyatt Institute of Astronomy, University of Cambridge Debris discs, exoasteroids and exocomets Mark Wyatt Institute of Astronomy, University of Cambridge The Solar System s outer and inner debris belts Outer debris: Kuiper belt Inner debris: Asteroid belt

More information

Debris Disks from Spitzer to Herschel and Beyond. G. H. Rieke, K. Y. L. Su, et al. Steward Observatory The University of Arizona

Debris Disks from Spitzer to Herschel and Beyond. G. H. Rieke, K. Y. L. Su, et al. Steward Observatory The University of Arizona Debris Disks from Spitzer to Herschel and Beyond G. H. Rieke, K. Y. L. Su, et al. Steward Observatory The University of Arizona Our neighborhood debris disk There was a huge amount of collisional activity

More information

Debris disk structure arising from planetary perturbations

Debris disk structure arising from planetary perturbations Debris disk structure arising from planetary perturbations Mark Wyatt Institute of Astronomy, Cambridge Debris disk structure arising from planetary perturbations Disk dynamical theory and the observables

More information

How inner planetary systems relate to inner and outer debris belts. Mark Wyatt Institute of Astronomy, University of Cambridge

How inner planetary systems relate to inner and outer debris belts. Mark Wyatt Institute of Astronomy, University of Cambridge How inner planetary systems relate to inner and outer debris belts Mark Wyatt Institute of Astronomy, University of Cambridge The Solar System s outer and inner debris belts Outer debris: Kuiper belt Inner

More information

Placing Our Solar System in Context: [A 12 step program to learn to accept disk evolution]

Placing Our Solar System in Context: [A 12 step program to learn to accept disk evolution] Placing Our Solar System in Context: [A 12 step program to learn to accept disk evolution] Michael R. Meyer Steward Observatory, The University of Arizona Dana Backman, SOFIA/SETI Institute Alycia Weinberger,

More information

IRS SPECTRA OF SOLAR-TYPE STARS: A SEARCH FOR ASTEROID BELT ANALOGS

IRS SPECTRA OF SOLAR-TYPE STARS: A SEARCH FOR ASTEROID BELT ANALOGS IRS SPECTRA OF SOLAR-TYPE STARS: A SEARCH FOR ASTEROID BELT ANALOGS Debris disks Around Stars In our Solar System, dust is generated by collisions between larger bodies in the asteroid and Kuiper belts,

More information

Kuiper Belt Dynamics and Interactions

Kuiper Belt Dynamics and Interactions Kuiper Belt Dynamics and Interactions Minor Planet Center Ruth Murray-Clay Harvard-Smithsonian Center for Astrophysics Kuiper belt µm ejected by radiation pressure larger grains migrate in via PR drag

More information

The Fomalhaut Debris Disk

The Fomalhaut Debris Disk The Fomalhaut Debris Disk IRAS 12 micron http://ssc.spitzer.caltech.edu/documents/compendium/foma lhaut/ Fomalhaut is a bright A3 V star 7.7 pc away IRAS discovered an IR excess indicating a circumstellar

More information

Mid-IR and Far-IR Spectroscopic Measurements & Variability. Kate Su (University of Arizona)

Mid-IR and Far-IR Spectroscopic Measurements & Variability. Kate Su (University of Arizona) Mid-IR and Far-IR Spectroscopic Measurements & Variability Kate Su (University of Arizona) Five Zones of Debris Dust edge-on view of the Fomalhaut planetary system distance, r 1500 K very hot dust 500

More information

Debris dust tell us much about planetesimals and planets and sheds light to formation and evolution of planetary systems. KALAS et al.

Debris dust tell us much about planetesimals and planets and sheds light to formation and evolution of planetary systems. KALAS et al. Debris dust tell us much about planetesimals and planets and sheds light to formation and evolution of planetary systems KALAS et al. 2008 THE STAR Spectral type: F8 Distance : 17.4 pc Age : ~ 2 Gyr A

More information

Are planets and debris correlated? Herschel imaging of 61 Vir

Are planets and debris correlated? Herschel imaging of 61 Vir Are planets and debris correlated? Herschel imaging of 61 Vir Mark Wyatt Institute of Astronomy, University of Cambridge + Grant Kennedy, Amaya Moro-Martin, Jean-Francois Lestrade, Geoff Bryden, Bruce

More information

Debris Disks and the Evolution of Planetary Systems. Christine Chen September 1, 2009

Debris Disks and the Evolution of Planetary Systems. Christine Chen September 1, 2009 Debris Disks and the Evolution of Planetary Systems Christine Chen September 1, 2009 Why Study Circumstellar Disks? How common is the architecture of our solar system (terrestrial planets, asteroid belt,

More information

Kate Su (University of Arizona)

Kate Su (University of Arizona) Debris Disks with Spitzer and beyond Kate Su (University of Arizona) Collaborators: G. Rieke, K. Misselt, P. Smith J. Sierchio, P. Espinoza (U of A), K. Stapelfeldt, F. Morales, G. Bryden (Caltech/JPL),

More information

Science Olympiad Astronomy C Division Event National Exam

Science Olympiad Astronomy C Division Event National Exam Science Olympiad Astronomy C Division Event National Exam University of Nebraska-Lincoln May 15-16, 2015 Team Number: Team Name: Instructions: 1) Please turn in all materials at the end of the event. 2)

More information

Who was here? How can you tell? This is called indirect evidence!

Who was here? How can you tell? This is called indirect evidence! 1 Who was here? How can you tell? This is called indirect evidence! 2 How does a planetary system form? The one we can study in the most detail is our solar system. If we want to know whether the solar

More information

Hot Dust Around Young Stars and Evolved Stars

Hot Dust Around Young Stars and Evolved Stars Hot Dust Around Young Stars and Evolved Stars Kate Su Steward Observatory University of Arizona Dust Zones Revealed by Great Observatories edge-on view of nearby planetary debris disks distance, r, increases

More information

other Galactic science Jane Greaves St Andrews

other Galactic science Jane Greaves St Andrews other Galactic science Jane Greaves St Andrews JCMT examples Sgr A*: massive black hole Evolved stars: dust and molecules Shell stars: violent mass-loss Shaping PNe: breaking spherical symmetry Pulsars:

More information

Observations of exozodiacal disks. Jean-Charles Augereau LAOG, Grenoble, France. ISSI team: Exozodiacal dust diks and Darwin. Cambridge, August 2009

Observations of exozodiacal disks. Jean-Charles Augereau LAOG, Grenoble, France. ISSI team: Exozodiacal dust diks and Darwin. Cambridge, August 2009 + Olivier Absil Emmanuel Di Folco Hervé Beust Rémy Reche Alexander Krivov Philippe Thébault Torsten Loehne Vincent Coudé du Foresto Bertrand Menesson Pierre Kervella ISSI team: Exozodiacal dust diks and

More information

Debris Disks and the Formation and Evolution of Planetary Systems. Christine Chen October 14, 2010

Debris Disks and the Formation and Evolution of Planetary Systems. Christine Chen October 14, 2010 Debris Disks and the Formation and Evolution of Planetary Systems Christine Chen October 14, 2010 1 Outline Dust Debris in our Solar System The Discovery of Dust Debris Around Other Stars The Connection

More information

Optical Properties and Thermal Modeling of Dust Grains in Circumstellar Environments

Optical Properties and Thermal Modeling of Dust Grains in Circumstellar Environments Optical Properties and Thermal Modeling of Dust Grains in Circumstellar Environments Justin Bracks Consortium for Undergraduate Research Los Angeles Community College Los Angeles, USA Justinbracks@gmail.com

More information

WFIRST Preparatory Science (WPS) Project: The Circumstellar Environments of Exoplanet Host Stars (NNH14ZDA001N-WPS; PI: Christine Chen)

WFIRST Preparatory Science (WPS) Project: The Circumstellar Environments of Exoplanet Host Stars (NNH14ZDA001N-WPS; PI: Christine Chen) Permission to use these WFIRST CGI simulated data products and information within this document is granted under the condition that credit is given to: Charles Poteet (STScI), Christine Chen (STScI), Maxime

More information

Origins of Stars and Planets in the VLT Era

Origins of Stars and Planets in the VLT Era Origins of Stars and Planets in the VLT Era Michael R. Meyer Institute for Astronomy, ETH-Zurich From Circumstellar Disks to Planets 5 November 2009, ESO/MPE Garching Planet Formation = Saving the Solids

More information

Debris Disks: A Brief Observational History Thomas Oberst April 19, 2006 A671

Debris Disks: A Brief Observational History Thomas Oberst April 19, 2006 A671 Debris Disks: A Brief Observational History Thomas Oberst A671 Debris Disk; Artist s rendition (T. Pyle (SSC), JPL-Caltech, & NASA http://www.spitz er.caltech.edu/m edia/happenings /20051214/) Debris Disks

More information

Astronomy 405 Solar System and ISM

Astronomy 405 Solar System and ISM Astronomy 405 Solar System and ISM Lecture 14 Comets February 15, 2013 Dynamics of Comet Tails Gas (ion) tails - interact with the solar wind - point away from the Sun. Dust tails - pushed by radiation

More information

Direct imaging of extra-solar planets

Direct 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

Circumstellar disks The MIDI view. Sebastian Wolf Kiel University, Germany

Circumstellar disks The MIDI view. Sebastian Wolf Kiel University, Germany Circumstellar disks The MIDI view Sebastian Wolf Kiel University, Germany MPIA MIDI SG concluding meeting May 5, 2014 Overview Circumstellar disks: Potential of IR long-baseline interferometry MIDI: Exemplary

More information

Millimeter Emission Structure in the AU Mic Debris Disk

Millimeter Emission Structure in the AU Mic Debris Disk Millimeter Emission Structure in the AU Mic Debris Disk Meredith MacGregor Harvard University Wilner, D.J., Rosenfeld, K.A., Andrews, S.M., Ma7hews, B., Hughes, A.M., Booth, M., Chiang, E., Graham, J.R.,

More information

Modeling interactions between a debris disc and planet: which initial conditions?

Modeling interactions between a debris disc and planet: which initial conditions? Modeling interactions between a debris disc and planet: which initial conditions? Elodie Thilliez @ET_astro Supervisors : Prof Sarah Maddison (Swinburne) Prof Jarrod Hurley (Swinburne) Crédit : NASA/JPL-Caltech

More information

Spitzer Space Telescope Imaging of Spatially- Resolved Debris Disks. Karl Stapelfeldt Jet Propulsion Laboratory MSC d2p: Mar

Spitzer Space Telescope Imaging of Spatially- Resolved Debris Disks. Karl Stapelfeldt Jet Propulsion Laboratory MSC d2p: Mar Spitzer Space Telescope Imaging of Spatially- Resolved Debris Disks Karl Stapelfeldt Jet Propulsion Laboratory MSC d2p: Mar 9 2005 1 In collaboration with Jet Propulsion Laboratory: Michael Werner, Chas

More information

Extrasolar Planets. Properties Pearson Education Inc., publishing as Pearson Addison-Wesley

Extrasolar Planets. Properties Pearson Education Inc., publishing as Pearson Addison-Wesley Extrasolar Planets Properties 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley Finding extrasolar planets is hard quick recap Planet Detection Direct: pictures or spectra of the planets

More information

Exozodiacal discs with infrared interferometry

Exozodiacal discs with infrared interferometry Exozodiacal discs with infrared interferometry First results and perspectives * (post-doc at LAOG, Grenoble) and E. Di Folco (Obs. Geneva), J.C. Augereau (LAOG), V. Coudé du Foresto (Obs. Paris), A. Mérand

More information

Molecular gas in young debris disks

Molecular gas in young debris disks Molecular gas in young debris disks Attila Moór1, Péter Ábrahám1, Ágnes Kóspál1, Michel Curé2, Attila Juhász3 et al. 1 - Konkoly Observatory, Budapest, Hungary 2 Universidad Valparaíso, Chile 3 - Institute

More information

Analysis of the Herschel DEBRIS Sun-like star sample

Analysis of the Herschel DEBRIS Sun-like star sample Advance Access publication 2017 December 11 doi:10.1093/mnras/stx3188 Analysis of the Herschel DEBRIS Sun-like star sample B. Sibthorpe, 1,2 G. M. Kennedy, 3 M. C. Wyatt, 4 J.-F. Lestrade, 5 J. S. Greaves,

More information

Formation and Evolution of Planetary Systems

Formation and Evolution of Planetary Systems Formation and Evolution of Planetary Systems Meyer, Hillenbrand et al., Formation and Evolution of Planetary Systems (FEPS): First Results from a Spitzer Legacy Science Program ApJ S 154: 422 427 (2004).

More information

Lecture Outlines. Chapter 15. Astronomy Today 7th Edition Chaisson/McMillan Pearson Education, Inc.

Lecture Outlines. Chapter 15. Astronomy Today 7th Edition Chaisson/McMillan Pearson Education, Inc. Lecture Outlines Chapter 15 Astronomy Today 7th Edition Chaisson/McMillan Chapter 15 The Formation of Planetary Systems Units of Chapter 15 15.1 Modeling Planet Formation 15.2 Terrestrial and Jovian Planets

More information

Investigations of the Formation and Evolution of Planetary Systems

Investigations of the Formation and Evolution of Planetary Systems Investigations of the Formation and Evolution of Planetary Systems Alwyn Wootten, Bryan Butler, Antonio Hales, Stuartt Corder, 1 Robert Brown 2 & David Wilner 3 Abstract. Stars and planets are the fundamental

More information

A White Paper for the Astro2010 Decadal Survey Submitted to the Planetary and Star Formation Panel

A White Paper for the Astro2010 Decadal Survey Submitted to the Planetary and Star Formation Panel Debris Disks: Signposts to planetary systems Prospects for the next decade A White Paper for the Astro2010 Decadal Survey Submitted to the Planetary and Star Formation Panel Wayne Holland, UK ATC, Royal

More information

Transneptunian objects. Minor bodies in the outer Solar System. Transneptunian objects

Transneptunian objects. Minor bodies in the outer Solar System. Transneptunian objects Transneptunian objects Minor bodies in the outer Solar System Planets and Astrobiology (2016-2017) G. Vladilo Around 1980 it was proposed that the hypothetical disk of small bodies beyond Neptune (called

More information

EXOPLANET LECTURE PLANET FORMATION. Dr. Judit Szulagyi - ETH Fellow

EXOPLANET LECTURE PLANET FORMATION. Dr. Judit Szulagyi - ETH Fellow EXOPLANET LECTURE PLANET FORMATION Dr. Judit Szulagyi - ETH Fellow (judits@ethz.ch) I. YOUNG STELLAR OBJECTS AND THEIR DISKS (YSOs) Star Formation Young stars born in 10 4 10 6 M Sun Giant Molecular Clouds.

More information

summary of last lecture

summary of last lecture radiation specific intensity flux density bolometric flux summary of last lecture Js 1 m 2 Hz 1 sr 1 Js 1 m 2 Hz 1 Js 1 m 2 blackbody radiation Planck function(s) Wien s Law λ max T = 2898 µm K Js 1 m

More information

Chapter 19 The Origin of the Solar System

Chapter 19 The Origin of the Solar System Chapter 19 The Origin of the Solar System Early Hypotheses catastrophic hypotheses, e.g., passing star hypothesis: Star passing closely to the the sun tore material out of the sun, from which planets could

More information

while the Planck mean opacity is defined by

while the Planck mean opacity is defined by PtII Astrophysics Lent, 2016 Physics of Astrophysics Example sheet 4 Radiation physics and feedback 1. Show that the recombination timescale for an ionised plasma of number density n is t rec 1/αn where

More information

Pluto, the Kuiper Belt, and Trans- Neptunian Objects

Pluto, the Kuiper Belt, and Trans- Neptunian Objects Pluto, the Kuiper Belt, and Trans- Neptunian Objects 1 What about Pluto? Pluto used to be considered a planet Pluto is one of a large number of Trans-Neptunian Objects, not even the largest one! Discovery

More information

Importance of the study of extrasolar planets. Exoplanets Introduction. Importance of the study of extrasolar planets

Importance of the study of extrasolar planets. Exoplanets Introduction. Importance of the study of extrasolar planets Importance of the study of extrasolar planets Exoplanets Introduction Planets and Astrobiology (2017-2018) G. Vladilo Technological and scientific spin-offs Exoplanet observations are driving huge technological

More information

Planet formation in protoplanetary disks. Dmitry Semenov Max Planck Institute for Astronomy Heidelberg, Germany

Planet formation in protoplanetary disks. Dmitry Semenov Max Planck Institute for Astronomy Heidelberg, Germany Planet formation in protoplanetary disks Dmitry Semenov Max Planck Institute for Astronomy Heidelberg, Germany Suggested literature "Protoplanetary Dust" (2010), eds. D. Apai & D. Lauretta, CUP "Protostars

More information

AST 105 The Important Things

AST 105 The Important Things AST 105 The Important Things I. Science A process not a litany of facts Non-dogmatic Knowing Why or How a process occurs is more important than remembering facts. Our understanding may start out wrong,

More information

arxiv: v1 [astro-ph] 8 Jul 2008

arxiv: v1 [astro-ph] 8 Jul 2008 Dynamics of small bodies in planetary systems Mark C. Wyatt arxiv:0807.1272v1 [astro-ph] 8 Jul 2008 Institute of Astronomy, University of Cambridge, Cambridge CB3 0HA, UK wyatt@ast.cam.ac.uk The number

More information

On the direct imaging of Exoplanets. Sebastian Perez Stellar Coffee - December 2008

On the direct imaging of Exoplanets. Sebastian Perez Stellar Coffee - December 2008 On the direct imaging of Exoplanets Sebastian Perez Stellar Coffee - December 2008 Outline Exoplanets overview Direct Imaging: - Observing strategy - Angular differential imaging HR8799 Fomalhaut beta

More information

DETAILED MODEL OF THE EXOZODIACAL DISK OF FOMALHAUT AND ITS ORIGIN

DETAILED MODEL OF THE EXOZODIACAL DISK OF FOMALHAUT AND ITS ORIGIN EXOZODI project http://ipag.osug.fr/~augereau/site/ ANR_EXOZODI.html IAU Symposium 299 EXPLORING THE FORMATION AND EVOLUTION OF PLANETARY SYSTEMS Victoria, Canada 2013, June 6 DETAILED MODEL OF THE EXOZODIACAL

More information

Young Solar-like Systems

Young Solar-like Systems Young Solar-like Systems FIG.2. Panels(a),(b),and(c)show 2.9,1.3,and 0.87 mm ALMA continuum images of other panels, as well as an inset with an enlarged view of the inner 300 mas centered on the (f) show

More information

Stellar Astronomy Sample Questions for Exam 3

Stellar Astronomy Sample Questions for Exam 3 Stellar Astronomy Sample Questions for Exam 3 Chapter 7 1. A protostar is formed by a) the rapid expansion of gas from an exploding star. b) the gravitational collapse of a rotating interstellar cloud.

More information

The Ecology of Stars

The Ecology of Stars The Ecology of Stars We have been considering stars as individuals; what they are doing and what will happen to them Now we want to look at their surroundings And their births 1 Interstellar Matter Space

More information

Exoplanets Atmospheres. Characterization of planetary atmospheres. Photometry of planetary atmospheres from direct imaging

Exoplanets 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 information

Jessica Donaldson (Carnegie DTM) Aki Roberge (NASA GSFC)

Jessica Donaldson (Carnegie DTM) Aki Roberge (NASA GSFC) Jessica Donaldson (Carnegie DTM) Aki Roberge (NASA GSFC) Gas evolution in disks 10 100 M Jupiter few M Lunar (dust) Total Mass 10 100 M Jupiter? Gas Mass Star Time (Myr) formation 1 5 10 ~ 1 Gyr Planetary

More information

Setting the Stage for Planet Formation: Grain Growth in Circumstellar Disks

Setting 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 information

Astronomy 421. Lecture 8: Binary stars

Astronomy 421. Lecture 8: Binary stars Astronomy 421 Lecture 8: Binary stars 1 Key concepts: Binary types How to use binaries to determine stellar parameters The mass-luminosity relation 2 Binary stars So far, we ve looked at the basic physics

More information

Foundations of Astrophysics

Foundations of Astrophysics Foundations of Astrophysics Barbara Ryden The Ohio State University Bradley M. Peterson The Ohio State University Preface xi 1 Early Astronomy 1 1.1 The Celestial Sphere 1 1.2 Coordinate Systems on a Sphere

More information

Recent advances in understanding planet formation

Recent advances in understanding planet formation Credit: ALMA (ESO/NAOJ/NRAO) Recent advances in understanding planet formation Misato Fukagawa Chile observatory (Mitaka), NAOJ Contents of this talk 1. Introduction: Exoplanets, what we want to know from

More information

Planetary system dynamics Part III Mathematics / Part III Astrophysics

Planetary system dynamics Part III Mathematics / Part III Astrophysics Planetary system dynamics Part III Mathematics / Part III Astrophysics Lecturer: Prof. Mark Wyatt (Dr. Amy Bonsor on 9,11 Oct) Schedule: Michaelmas 2017 Mon, Wed, Fri at 10am MR11, 24 lectures, start Fri

More information

Other planetary systems

Other planetary systems Exoplanets are faint! Other planetary systems Planets are seen only by reflected light at optical wavelengths At the distance of another star the faint light of a planet is lost in the glare of the star

More information

Astro Week 1. (a) Show that the transit duration for a non-central transit (see Figures) is: R R. b = a cos i

Astro Week 1. (a) Show that the transit duration for a non-central transit (see Figures) is: R R. b = a cos i Astro-286 - Week 1 1. Radial Velocity (10 pt) What is the expected amplitude of velocity oscillations of 1 M star that is orbited by a Jupiter mass planet (m J = 0.001 M ) at 1 AU separation? What is the

More information

The architecture of planetary systems revealed by debris disk imaging

The architecture of planetary systems revealed by debris disk imaging The architecture of planetary systems revealed by debris disk imaging Paul Kalas University of California at Berkeley Collaborators: James Graham, Mark Clampin, Brenda Matthews, Mike Fitzgerald, Geoff

More information

Data from: The Extrasolar Planet Encyclopaedia.

Data from: The Extrasolar Planet Encyclopaedia. Data from: The Extrasolar Planet Encyclopaedia http://exoplanet.eu/ 2009->10 Status of Exoplanet Searches Direct Detection: 5->9 planets detected Sensitive to large planets in large orbits around faint

More information

1 Solar System Debris and Formation

1 Solar System Debris and Formation 1 Solar System Debris and Formation Chapters 14 and 15 of your textbook Exercises: Do all Review and Discussion and all Conceptual Self-Test 1.1 Solar System Debris Asteroids small rocky bodies Most under

More information

Non-axisymmetric structure in million-year-old discs around intermediate-mass stars

Non-axisymmetric structure in million-year-old discs around intermediate-mass stars Non-axisymmetric structure in million-year-old discs around intermediate-mass stars Misato Fukagawa (NAOJ) C. A. Grady, J. P. Wisniewski, Y. Ohta, M. Momose, Y. Matura, T. Kotani, Y. Okamoto, J. Hashimoto,

More information

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.

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. 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 information

Astro 201 Radiative Processes Solution Set 1. by Roger O Brient and Eugene Chiang

Astro 201 Radiative Processes Solution Set 1. by Roger O Brient and Eugene Chiang Astro 21 Radiative Processes Solution Set 1 by Roger O Brient and Eugene Chiang Readings: Rybicki & Lightman Chapter 1 except the last section 1.8. Problem 1. Blackbody Flux Derive the blackbody flux formula

More information

Exoplanet Science with SPHEREx s All-Sky Spectro-photometric Survey in the Near-Infrared. A White Paper in support of the Exoplanet Science Strategy

Exoplanet Science with SPHEREx s All-Sky Spectro-photometric Survey in the Near-Infrared. A White Paper in support of the Exoplanet Science Strategy Exoplanet Science with SPHEREx s All-Sky Spectro-photometric Survey in the Near-Infrared A White Paper in support of the Exoplanet Science Strategy March 9, 2018 Daniel J. Stevens (stevens.725@osu.edu,

More information

What is it like? When did it form? How did it form. The Solar System. Fall, 2005 Astronomy 110 1

What is it like? When did it form? How did it form. The Solar System. Fall, 2005 Astronomy 110 1 What is it like? When did it form? How did it form The Solar System Fall, 2005 Astronomy 110 1 Fall, 2005 Astronomy 110 2 The planets all orbit the sun in the same direction. The Sun spins in the same

More information

Lecture Outlines. Chapter 15. Astronomy Today 8th Edition Chaisson/McMillan Pearson Education, Inc.

Lecture Outlines. Chapter 15. Astronomy Today 8th Edition Chaisson/McMillan Pearson Education, Inc. Lecture Outlines Chapter 15 Astronomy Today 8th Edition Chaisson/McMillan Chapter 15 Exoplanets Units of Chapter 15 15.1 Modeling Planet Formation 15.2 Solar System Regularities and Irregularities 15.3

More information

Star formation : circumstellar environment around Young Stellar Objects

Star formation : circumstellar environment around Young Stellar Objects Bull. Astr. Soc. India (2005) 33, 327 331 Star formation : circumstellar environment around Young Stellar Objects Manoj Puravankara Inter-University Centre for Astronomy and Astrophysics, Pune - 411007,

More information

Beta Pictoris : Disk, comets, planet

Beta Pictoris : Disk, comets, planet Beta Pictoris : Disk, comets, planet Hervé Beust Institut de Planétologie et d Astrophysique de Grenoble (IPAG) 1 Outline of the talk 1. The star 2. The dust disk Clues for the presence of planets 3. The

More information

MEASURING THE STRUCTURE AND COMPOSITION OF CIRCUMSTELLAR DEBRIS DISKS

MEASURING THE STRUCTURE AND COMPOSITION OF CIRCUMSTELLAR DEBRIS DISKS MEASURING THE STRUCTURE AND COMPOSITION OF CIRCUMSTELLAR DEBRIS DISKS by Nicholas Paul Ballering Copyright c Nicholas Paul Ballering 2016 A Dissertation Submitted to the Faculty of the DEPARTMENT OF ASTRONOMY

More information

DEPARTMENT OF PHYSICS AND ASTRONOMY. Planets around white dwarfs Matt Burleigh

DEPARTMENT OF PHYSICS AND ASTRONOMY. Planets around white dwarfs Matt Burleigh DEPARTMENT OF PHYSICS AND ASTRONOMY Planets around white dwarfs Matt Burleigh Contents Original motivation DODO - results from our direct imaging survey Where do we go next? The role for E-ELT Direct imaging

More information

Observing Habitable Environments Light & Radiation

Observing Habitable Environments Light & Radiation Homework 1 Due Thurs 1/14 Observing Habitable Environments Light & Radiation Given what we know about the origin of life on Earth, how would you recognize life on another world? Would this require a physical

More information

The 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 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 information

Problem Set 4 is due Thursday. Problem Set 5 will be out today or tomorrow. Launch Latest from MASCOT

Problem Set 4 is due Thursday. Problem Set 5 will be out today or tomorrow. Launch Latest from MASCOT 1 Problem Set 4 is due Thursday. Problem Set 5 will be out today or tomorrow. Launch Latest from MASCOT 3 Continuous Spectra: Thermal Radiation The equations below quantitatively summarize the light-emitting

More information

Extrasolar Planets. Methods of detection Characterization Theoretical ideas Future prospects

Extrasolar Planets. Methods of detection Characterization Theoretical ideas Future prospects Extrasolar Planets Methods of detection Characterization Theoretical ideas Future prospects Methods of detection Methods of detection Methods of detection Pulsar timing Planetary motion around pulsar

More information

International Olympiad on Astronomy and Astrophysics (IOAA)

International Olympiad on Astronomy and Astrophysics (IOAA) Syllabus of International Olympiad on Astronomy and Astrophysics (IOAA) General Notes 1. Extensive contents in basic astronomical concepts are required in theoretical and practical problems. 2. Basic concepts

More information

Extrasolar planets Detection and habitability

Extrasolar planets Detection and habitability Extrasolar planets Detection and habitability October 23rd 2014 Detecting exoplanets Primary methods : Direct imaging Transit Radial velocity Direct imaging Planets are much fainter than their host star

More information

Astronomy 111 Exam Review Problems (Real exam will be Tuesday Oct 25, 2016)

Astronomy 111 Exam Review Problems (Real exam will be Tuesday Oct 25, 2016) Astronomy 111 Exam Review Problems (Real exam will be Tuesday Oct 25, 2016) Actual Exam rules: you may consult only one page of formulas and constants and a calculator while taking this test. You may not

More information

Payne-Scott workshop on Hyper Compact HII regions Sydney, September 8, 2010

Payne-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 information

Vega s hot dust from icy planetesimals scattered inwards by an outward-migrating planetary system

Vega s hot dust from icy planetesimals scattered inwards by an outward-migrating planetary system Advance Access publication 2014 April 25 doi:10.1093/mnrasl/slu048 Vega s hot dust from icy planetesimals scattered inwards by an outward-migrating planetary system Sean N. Raymond 1,2,3 and Amy Bonsor

More information

The Infrared Universe as Seen by Spitzer and Beyond. February 20, 2007

The Infrared Universe as Seen by Spitzer and Beyond. February 20, 2007 The Infrared Universe as Seen by Spitzer and Beyond The Holly Berry Cluster [NOT the Halle Berry cluster] in Serpens February 20, 2007 Presented to the Herschel Open Time Key Project Workshop Michael Werner,

More information

What Have We Found? 1978 planets in 1488 systems as of 11/15/15 (http://exoplanet.eu/ ) 1642 planets candidates (http://exoplanets.

What Have We Found? 1978 planets in 1488 systems as of 11/15/15 (http://exoplanet.eu/ ) 1642 planets candidates (http://exoplanets. Exoplanets. II What Have We Found? 1978 planets in 1488 systems as of 11/15/15 (http://exoplanet.eu/ ) 1642 planets + 3787 candidates (http://exoplanets.org) Detected by radial velocity/astrometry: 621

More information

Olivier Absil. University of Liège

Olivier Absil. University of Liège Olivier Absil University of Liège Seminar at MPIfR Bonn July 15 th, 2011 We all live in a debris disk! 2 nd generation dust (asteroids, comets) Dust is luminous (much more than planets) Dust is expected

More information

Revealing the evolution of disks at au from high-resolution IR spectroscopy

Revealing the evolution of disks at au from high-resolution IR spectroscopy Protoplanetary seen through the eyes of new-generation high-resolution instruments - Rome, June 6, 08 Revealing the evolution of at 0.0-0 au from high-resolution IR spectroscopy VLT IR interferometry (not

More information

Introduction to Astronomy. Lecture 7: Observing Stars Star Birth, Stellar Interiors, and Stellar Evolution

Introduction to Astronomy. Lecture 7: Observing Stars Star Birth, Stellar Interiors, and Stellar Evolution Introduction to Astronomy Lecture 7: Observing Stars Star Birth, Stellar Interiors, and Stellar Evolution 1 Stars What are they? Massive gas bodies in space Generates light by fusion Defined by fusion

More information

Astronomy 111 Review Problems Solutions

Astronomy 111 Review Problems Solutions Astronomy 111 Review Problems Solutions Problem 1: Venus has an equatorial radius of 6052 km. Its semi-major axis is 0.72 AU. The Sun has a radius of cm. a) During a Venus transit (such as occurred June

More information

AST111, Lecture 1b. Measurements of bodies in the solar system (overview continued) Orbital elements

AST111, Lecture 1b. Measurements of bodies in the solar system (overview continued) Orbital elements AST111, Lecture 1b Measurements of bodies in the solar system (overview continued) Orbital elements Planetary properties (continued): Measuring Mass The orbital period of a moon about a planet depends

More information

Do two-temperature debris discs have multiple belts?

Do two-temperature debris discs have multiple belts? doi:10.1093/mnras/stu1665 Do two-temperature debris discs have multiple belts? G. M. Kennedy andm.c.wyatt Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK Accepted

More information

Wed. Aug. 30, 2017 Reading:

Wed. Aug. 30, 2017 Reading: Wed. Aug. 30, 2017 Reading: Reading for Fri.: Wood Ch. 1 (solar system overview) Reading for Wed. Wed. Wood Ch. 6 & 8 (Asteroids & Meteorites, Solar Nebula) Reading for Fri. Sept. 8. Rozel et al. (link

More information

Planets: Name Distance from Sun Satellites Year Day Mercury 0.4AU yr 60 days Venus yr 243 days* Earth 1 1 yr 1 day Mars 1.

Planets: Name Distance from Sun Satellites Year Day Mercury 0.4AU yr 60 days Venus yr 243 days* Earth 1 1 yr 1 day Mars 1. The Solar System (Ch. 6 in text) We will skip from Ch. 6 to Ch. 15, only a survey of the solar system, the discovery of extrasolar planets (in more detail than the textbook), and the formation of planetary

More information

CIRCUMSTELLAR DISKS AND OUTER PLANET FORMATION

CIRCUMSTELLAR DISKS AND OUTER PLANET FORMATION CIRCUMSTELLAR DISKS AND OUTER PLANET FORMATION A. LECAVELIER DES ETANGS Institut d Astrophysique de Paris 98 Bld Arago, F-75014 Paris, France Abstract. The dust disk around β Pictoris must be produced

More information

Stars, Galaxies & the Universe Lecture Outline

Stars, Galaxies & the Universe Lecture Outline Stars, Galaxies & the Universe Lecture Outline A galaxy is a collection of 100 billion stars! Our Milky Way Galaxy (1)Components - HII regions, Dust Nebulae, Atomic Gas (2) Shape & Size (3) Rotation of

More information

Example: model a star using a two layer model: Radiation starts from the inner layer as blackbody radiation at temperature T in. T out.

Example: model a star using a two layer model: Radiation starts from the inner layer as blackbody radiation at temperature T in. T out. Next, consider an optically thick source: Already shown that in the interior, radiation will be described by the Planck function. Radiation escaping from the source will be modified because the temperature

More information

USAAAO First Round 2015

USAAAO First Round 2015 USAAAO First Round 2015 This round consists of 30 multiple-choice problems to be completed in 75 minutes. You may only use a scientific calculator and a table of constants during the test. The top 50%

More information

aka Light Properties of Light are simultaneously

aka Light Properties of Light are simultaneously Today Interaction of Light with Matter Thermal Radiation Kirchhoff s Laws aka Light Properties of Light are simultaneously wave-like AND particle-like Sometimes it behaves like ripples on a pond (waves).

More information

An Unbiased Near-infrared Interferometric Survey for Hot Exozodiacal Dust

An Unbiased Near-infrared Interferometric Survey for Hot Exozodiacal Dust Astronomical Science An Unbiased Near-infrared Interferometric Survey for Hot Exozodiacal Dust Steve Ertel 1,2,3 Jean-Charles Augereau 2,3 Olivier Absil 4 Denis Defrère 5 Jean-Baptiste Le Bouquin 2,3 Lindsay

More information