Recent advances in understanding planet formation

Size: px
Start display at page:

Download "Recent advances in understanding planet formation"

Transcription

1 Credit: ALMA (ESO/NAOJ/NRAO) Recent advances in understanding planet formation Misato Fukagawa Chile observatory (Mitaka), NAOJ

2 Contents of this talk 1. Introduction: Exoplanets, what we want to know from observations of protoplanetary disks 2. Recent observations Dust mass and its evolution available time/material for planet formation Grain growth necessary step toward planet formation Azimuthal asymmetry sign of ongoing formation Multiple, symmetric gaps in HL Tau 3. What will come, what we want to have near future Chemical study is not included in this review.

3 Planets are common

4 Diversity

5 2 Jupiter-mass at 13 AU in direct imaging We ve started to detect planets like in our Solar-system 0.99 Jupiter-mass at 4.8 AU around a star with ~6000 K NASA Ames/JPL-CalTech/R. Hurt

6 Questions How did the solar system (in particular, our Earth) form? How do planets form in the Milky way? What is the key to form Solar-system-like planetary systems?

7 1. Formation 2. Migration Interaction with a disk Interaction with other planets Diversity? Credit: NAOJ

8 Giant planet formation Standard senario: Core accretion Takes ~10 million years (~1 Myr at the fastest) Dust (micron) -> planetesimals (~km) Gas accretion Credit: Rikanenpyo

9 Disks provide initial condition of formation and control early orbital evolution of planets Surface density distribution (disk mass) Planet mass and location Chemical evolution of disk material Planet composition Disk gas lifetime, dissipation mechanisms Orbital evolution (migration) of planets What we want to know: Physical and chemical structure (r, z), T(r, z), X(r, z) X-ray, UV, optical accretion radial drift mixing

10 Key things for protoplanetary disk 1. High angular resolution observations Distance to the nearest star-forming regions ~ 140 pc Want to spatially resolve ~5 AU (Jupiter s orbit) ~30 milliarcsec is required. (ALMA, adaptive optics in optical on 8m class telescopes) 2. Longer wavelengths Mid-plane (where planets form) has very high density. Most region is optically thick if < submillimeter. Large grains are bright at longer wavelengths.

11 Protoplanetary disks frequently observed 0.1 Myr Age: 1 10 million years Optically thick, gaseous 1. Planet will form Initial condition 2. Formation has just completed Dynamical interaction between disk and planets Young planets 1 Myr 10 Myr 100 Myr NAOJ

12 Dust mass and its evolution in protoplanetary disks amount and lifetime of ingredients of planets

13 Disk (mm-dust) mass from dust continuum M disk ~ F d 2 B (T d ) M disk M star 1 solar mass Careful analysis of SMA 1.3 mm 1% of the star Dust mass is roughly proportional to the stellar mass. There is a significant scatter. Jupiter Andrews et al. (2013)

14 Disk (mm-dust) mass evolution ALMA, 880 micron continuum U Sco: Age = 5 11 Myr Sensitivity: an order of magnitude better than the previous survey. Minimum detected mass = 0.3 Earth-mass No significant difference, or marginal evidence of lower mass compared to he younger region at ~2 Myr. -- need more data. Carpenter et al. (2014) 14

15 Grain growth fundamental step toward planets

16 Grain growth Dust continuum Brightness distribution is frequency dependent. Perez et al. (2012)

17 Β<1 Grain growth β is not constant in radial direction β 2 Grain size segregation in radial F d2 direction F d2 M disk ~ B ~ c2 (T d) 2k 2 T d if, F, = + 2 Measurements for many disks grains are bigger in the inner region Perez et al. (2012)

18 Asymmetry in disks with gaps/holes

19 Credit: NASA; Karen L. Teramura, UH IfA Disks with holes/gaps Williams & Cieza (2011)

20 Large-scale asymmetries Tang et al. (2012), van der Marel et al. (2015), Perez et al. (2014), Marino et al. (2015), Zhang et al. (2014) [ALMA, VLA, PdBI]

21 Gas is less structured General characteristics Gas is present inside the dust cavity but at a reduced level. The outer boundary for the inner cavity 1. Gas radius is smaller 2. Good match between gas & dust Bruderer et al. (2014) Dust ring at AU Gas component starts at 31 AU (Zhang et al. (2014)

22 Extreme asymmetry in dust continuum 440 m Dust cont. 890 m Dust cont. 0.2 van der Marel et al. (2013) Fukagawa et al. (2013)

23 Gas is less asymmetric Bruderer et al. (2014) Fukagawa et al. (2014)

24 van der Marel et al. (2013)

25 Local signature of grain growth Flux ratio is not constant across the disk in azimuthal direction Strong, local grain accumulation and grain growth there Grain size segregation in azimuthal direction. -- Dust trap hypothesis Casassus et al. (2015) Vortex!

26 General characteristics Gas is present inside the dust cavity but at a reduced level. The outer boundary for the inner cavity 1. Gas radius is smaller 2. Good match between gas & dust Gas is less structured Bruderer et al. (2013) Roughly consistent with dust trap idea, but Dust ring at AU Gas component starts at 31 AU

27 How about protoplanets? Catching thermal infrared emission ~6 15 Jupiter-mass at ~20 AU 850 micron dust cont. Giant planet at 53 AU ~30 Jupiter-mass at 23 AU (Kraus and Ireland 2012, Quanz et al. 2012,2014, Reggiani et al. 2014)

28 Multiple, nearly symmetric gaps in HL Tau

29 0.1 Myr ALMA partnership (2015) Close et al. (1997)

30 2.9, 1.3, and 0.87 mm with angular resolutions of (10 AU) to (3.5 AU) Gap location 13, 32, ~42, ~50, 64, 74, ~91 AU The presence of orbital resonances. D1:D2:D3:D4 = 1:4:6:8 β <~ 0.8 in the dark lane grain growth? ALMA partnership (2015)

31 Inspired by ALMA results of HL Tau: condensation fronts? Zhang et al. (2015)

32 0.1 Myr Planet formation begins/proceeds/completes faster than we thought? ALMA partnership (2015) Close et al. (1997)

33 Things to look at in the (near) future 1. Improved statistics for over ~100 disks in nearby star-forming regions 2. Circumplanetary disks 3. Planet formation at an age of <~ 1 Myr 4. High angular resolution for boring, Myrold disks What is the dominant mechanism for planet formation?

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

Astro2020 Science White Paper Dust growth and dust trapping in protoplanetary disks with the ngvla

Astro2020 Science White Paper Dust growth and dust trapping in protoplanetary disks with the ngvla Astro2020 Science White Paper Dust growth and dust trapping in protoplanetary disks with the ngvla Thematic Areas: Star and Planet Formation Principal Author: Name: Nienke van der Marel Institution: Herzberg

More information

Star and Planet Formation: New Insights from Spatially Resolved Observations

Star and Planet Formation: New Insights from Spatially Resolved Observations Star and Planet Formation: New Insights from Spatially Resolved Observations Laura M. Pérez Universidad de Chile Division B, Comision B4 Radio Astronomy August 24, 2018 Setting the stage: Our current view

More information

HD Transition Disk Herbig Ae/Be stars 2014

HD Transition Disk Herbig Ae/Be stars 2014 a b HD142527 Transition Disk Herbig Ae/Be stars 2014 HD142527 ALMA results by Sebastián Pérez Simon Casassus Valentin Christiaens Francois Ménard also with Gerrit van der Plas, Pablo Román, Christian Flores,

More information

PLANETARY FORMATION THEORY EXPLORING EXOPLANETS

PLANETARY FORMATION THEORY EXPLORING EXOPLANETS PLANETARY FORMATION THEORY EXPLORING EXOPLANETS This is what we call planets around OTHER stars! PLANETARY FORMATION THEORY EXPLORING EXOPLANETS This is only as of June 2012. We ve found at least double

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

ALMA surveys of planet-forming disks

ALMA surveys of planet-forming disks ALMA surveys of planet-forming disks ILARIA PASCUCCI Lunar and Planetary Laboratory, Department of Planetary Sciences The University of Arizona Questions that can be answered in a disk survey: Which are

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

protoplanetary transition disks

protoplanetary transition disks protoplanetary transition disks (Harvard-CfA) 1. disk evolution and planets why does disk dispersal matter? 40 AU orbit 2. transition disks definitions and observational signatures SMA 880 microns 3. resolved

More information

Nature and Origin of Planetary Systems f p "

Nature and Origin of Planetary Systems f p Nature and Origin of Planetary Systems f p " Our Solar System as Example" We know far more about our solar system than about any other" It does have (at least) one planet suitable for life" Start with

More information

Generating Vortices with Slowly-growing Gas Giant Planets

Generating Vortices with Slowly-growing Gas Giant Planets Generating Vortices with Slowly-growing Gas Giant Planets van der Marel, N., et al. 2013 Michael Hammer Collaborators: Kaitlin Kratter, Paola Pinilla, Min-Kai Lin University of Arizona Generating Vortices

More information

Dust Growth in Protoplanetary Disks: The First Step Toward Planet Formation. Laura Pérez Jansky Fellow NRAO

Dust Growth in Protoplanetary Disks: The First Step Toward Planet Formation. Laura Pérez Jansky Fellow NRAO Dust Growth in Protoplanetary Disks: The First Step Toward Planet Formation Laura Pérez Jansky Fellow NRAO From ISM Dust to Planetary Systems Size = µμm ISM Dust mm mm/cm observations Directly observable

More information

Studying the Origins of Stars and their! Planetary Systems with ALMA & VLA"

Studying the Origins of Stars and their! Planetary Systems with ALMA & VLA Studying the Origins of Stars and their! Planetary Systems with ALMA & VLA" 14 th Synthesis Imaging Workshop! Laura Pérez" Jansky Fellow, National Radio Astronomy Observatory! Collaborators:" Claire Chandler

More information

( ) a3 (Newton s version of Kepler s 3rd Law) Units: sec, m, kg

( ) a3 (Newton s version of Kepler s 3rd Law) Units: sec, m, kg Astronomy 18, UCSC Planets and Planetary Systems Generic Mid-Term Exam (A combination of exams from the past several times this class was taught) This exam consists of two parts: Part 1: Multiple Choice

More information

Constraining the Evolution of Molecular Gas in Weak-Line T-Tauri Stars. 1. Motivation

Constraining the Evolution of Molecular Gas in Weak-Line T-Tauri Stars. 1. Motivation Constraining the Evolution of Molecular Gas in Weak-Line T-Tauri Stars 1. Motivation The formation of planets from protoplanetary disks is greatly influenced by the presence or absence of gas in these

More information

Forming habitable planets on the computer

Forming habitable planets on the computer Forming habitable planets on the computer Anders Johansen Lund University, Department of Astronomy and Theoretical Physics 1/9 Two protoplanetary discs (Andrews et al., 2016) (ALMA Partnership, 2015) Two

More information

Searching for Other Worlds

Searching for Other Worlds Searching for Other Worlds Lecture 32 1 In-Class Question What is the Greenhouse effect? a) Optical light from the Sun is reflected into space while infrared light passes through the atmosphere and heats

More information

Observational Properties of Protoplanetary Disks

Observational Properties of Protoplanetary Disks Observational Properties of Protoplanetary Disks Leonardo Testi - ESO/Arcetri ltesti@eso.org; lt@arcetri.astro.it Today: Tracing water, deuteration and link with Solar System Complex Organic Molecule Transition

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

Planet formation in action

Planet formation in action Planet formation in action Resolved gas and dust images of a transitional disk and its cavity Nienke van der Marel, Ewine van Dishoeck, Simon Bruderer, Til Birnstiel, Paola Pinilla, Kees Dullemond, Tim

More information

Protoplanetary disk demographics. Jonathan Williams! Institute for Astronomy, University of Hawaii

Protoplanetary disk demographics. Jonathan Williams! Institute for Astronomy, University of Hawaii Protoplanetary disk demographics Jonathan Williams! Institute for Astronomy, University of Hawaii Characterizing Planetary Systems Across the HR Diagram Cambridge, July 31, 2014 Disk demographics provide

More information

Planet formation in the ALMA era. Giuseppe Lodato

Planet formation in the ALMA era. Giuseppe Lodato Planet formation in the ALMA era Giuseppe Lodato A revolution in planet formation theory New facilities are revolutionizing our understanding of the planet formation process Extra-solar planet detection

More information

Planet Formation: theory and observations. Sean Raymond University of Colorado (until Friday) Observatoire de Bordeaux

Planet Formation: theory and observations. Sean Raymond University of Colorado (until Friday) Observatoire de Bordeaux Planet Formation: theory and observations Sean Raymond University of Colorado (until Friday) Observatoire de Bordeaux Outline Stages of Planet Formation Solar System Formation Cores to disks (c2d) Observational

More information

Lecture #15: Plan. Telescopes (cont d) Effects of Earth s Atmosphere Extrasolar planets = Exoplanets

Lecture #15: Plan. Telescopes (cont d) Effects of Earth s Atmosphere Extrasolar planets = Exoplanets Lecture #15: Plan Telescopes (cont d) Effects of Earth s Atmosphere Extrasolar planets = Exoplanets Resolving Power (review) The bigger the size of the telescope, the better it is at discerning fine details

More information

Searching for protoplanets. Sebastian Wolf Kiel University, Germany

Searching for protoplanets. Sebastian Wolf Kiel University, Germany Searching for protoplanets Sebastian Wolf Kiel University, Germany 2013 Rocks! Hawaii April 11, 2013 [Wolf & D Angelo 2005] 2 Constraints on the late stages of planet formation Disk physics 3 Early stages

More information

Chapter 13 Lecture. The Cosmic Perspective Seventh Edition. Other Planetary Systems: The New Science of Distant Worlds Pearson Education, Inc.

Chapter 13 Lecture. The Cosmic Perspective Seventh Edition. Other Planetary Systems: The New Science of Distant Worlds Pearson Education, Inc. Chapter 13 Lecture The Cosmic Perspective Seventh Edition Other Planetary Systems: The New Science of Distant Worlds 13.1 Detecting Planets Around Other Stars Our goals for learning: Why is it so challenging

More information

Credit: NASA/Kepler Mission/Dana Berry. Exoplanets

Credit: NASA/Kepler Mission/Dana Berry. Exoplanets Credit: NASA/Kepler Mission/Dana Berry Exoplanets Outline What is an exoplanet? Why are they interesting? How can we find them? Exolife?? The future... Jon Thaler Exoplanets 2 What is an Exoplanet? Most

More information

ALMA Science Cases with our Galaxy. SNU Town hall meeting for ALMA Cycle March 23 Woojin Kwon

ALMA Science Cases with our Galaxy. SNU Town hall meeting for ALMA Cycle March 23 Woojin Kwon ALMA Science Cases with our Galaxy SNU Town hall meeting for ALMA Cycle 5 2016 March 23 Woojin Kwon 1201 refereed articles (ADS) with ALMA in abstracts, as of 3/21/2016 618 publications at www.almascience.org

More information

Lecture #15: Plan. Telescopes (cont d) Effects of Earth s Atmosphere Extrasolar planets = Exoplanets

Lecture #15: Plan. Telescopes (cont d) Effects of Earth s Atmosphere Extrasolar planets = Exoplanets Lecture #15: Plan Telescopes (cont d) Effects of Earth s Atmosphere Extrasolar planets = Exoplanets Collecting Area Light bucket : the bigger the area of the telescope s mirror or lens, the more photons

More information

Stuctural diversity resolving Herbig Ae/Be circumstellar Disks at AU using PDI

Stuctural diversity resolving Herbig Ae/Be circumstellar Disks at AU using PDI Stuctural diversity resolving Herbig Ae/Be circumstellar Disks at 10150 AU using PDI Henning Avenhaus Institute for Astronomy, ETH Zürich 2013 ROCKS! Conference, Hawaii Sascha Quanz, Hans Martin Schmid,

More information

Stuctural diversity resolving Herbig Ae/Be circumstellar Disks at AU using PDI

Stuctural diversity resolving Herbig Ae/Be circumstellar Disks at AU using PDI Stuctural diversity resolving Herbig Ae/Be circumstellar Disks at 10150 AU using PDI Henning Avenhaus Institute for Astronomy, ETH Zürich 2013 ROCKS! Conference, Hawaii Sascha Quanz, Hans Martin Schmid,

More information

Why is it hard to detect planets around other stars?

Why is it hard to detect planets around other stars? Extrasolar planets Why is it hard to detect planets around other stars? Planets are small and low in mass Planets are faint The angular separation between planets and their stars is tiny Why is it hard

More information

ALMA Observations of Circumstellar Disks in the Upper Scorpius OB Association

ALMA Observations of Circumstellar Disks in the Upper Scorpius OB Association ALMA Observations of Circumstellar Disks in the Upper Scorpius OB Association Based on Barenfeld et al. (2016) Image Credit: ESO/L. Calçada Scott Barenfeld (Caltech) with John Carpenter, Luca Ricci, and

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

Exoplanet Detection and Characterization with Mid-Infrared Interferometry

Exoplanet Detection and Characterization with Mid-Infrared Interferometry Exoplanet Detection and Characterization with Mid-Infrared Interferometry Rachel Akeson NASA Exoplanet Science Institute With thanks to Peter Lawson for providing material Sagan Workshop July 21, 2009

More information

2010 Pearson Education, Inc.

2010 Pearson Education, Inc. Thought Question Suppose you found a star with the same mass as the Sun moving back and forth with a period of 16 months. What could you conclude? A. It has a planet orbiting at less than 1 AU. B. It has

More information

10/16/ Detecting Planets Around Other Stars. Chapter 10: Other Planetary Systems The New Science of Distant Worlds

10/16/ Detecting Planets Around Other Stars. Chapter 10: Other Planetary Systems The New Science of Distant Worlds 10/16/17 Lecture Outline 10.1 Detecting Planets Around Other Stars Chapter 10: Other Planetary Systems The New Science of Distant Worlds Our goals for learning: How do we detect planets around other stars?

More information

The large-scale magnetic field in protoplanetary disks

The large-scale magnetic field in protoplanetary disks The large-scale magnetic field in protoplanetary disks Jérôme Guilet MPA, Garching Max-Planck-Princeton center for plasma physics In collaboration with Gordon Ogilvie (Cambridge) 1/24 Talk outline 1) Impacts

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

Ruth Murray-Clay University of California, Santa Barbara

Ruth Murray-Clay University of California, Santa Barbara A Diversity of Worlds: Toward a Theoretical Framework for the Structures of Planetary Systems Ruth Murray-Clay University of California, Santa Barbara Strange New Worlds. Slide credit: Scott Gaudi ~1500

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

A Tale of Star and Planet Formation. Lynne Hillenbrand Caltech

A Tale of Star and Planet Formation. Lynne Hillenbrand Caltech A Tale of Star and Planet Formation Lynne Hillenbrand Caltech Vermeer s The Astronomer (1688) Mauna Kea (last week) photos by: Sarah Anderson and Bill Bates Context: Our Sun The Sun is a completely average

More information

SIMULTANEOUS FORMATION OF GIANT PLANETS

SIMULTANEOUS FORMATION OF GIANT PLANETS SIMULTANEOUS FORMATION OF GIANT PLANETS ANDREA FORTIER O. GUILERA, O.G. BENVENUTO, A. BRUNINI RINGBERG, 30 NOVEMBER 2010 PHYSIKALISCHES INSTITUT, UNIVERSITY OF BERN, SWITZERLAND FCAGLP, UNIVERSIDAD DE

More information

E-ELT/HIRES Disk-Star Interactions at the epoch of planet formation

E-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 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

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

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

The Solar Nebula Theory

The Solar Nebula Theory Reading: Chap. 21, Sect.21.1, 21.3 Final Exam: Tuesday, December 12; 4:30-6:30PM Homework 10: Due in recitation Dec. 1,4 Astro 120 Fall 2017: Lecture 25 page 1 Astro 120 Fall 2017: Lecture 25 page 2 The

More information

Transitional disks and their host stars

Transitional disks and their host stars Transitional disks and their host stars Nienke vander dermarel Marel Nienke van Leiden Observatory rd September 23 2011 The Netherlands August 13th 2013 (ING) Star and planet formation Class II => III:

More information

Galaxies: The Nature of Galaxies

Galaxies: The Nature of Galaxies Galaxies: The Nature of Galaxies The Milky Way The Milky Way is visible to the unaided eye at most place on Earth Galileo in 1610 used his telescope to resolve the faint band into numerous stars In the

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

The formation & evolution of solar systems

The formation & evolution of solar systems The formation & evolution of solar systems Content expectations Birth of the Solar System What did the material that eventually became the Sun and planets look like originally? Interstellar clouds like

More information

Side View. disk mostly young stars and lots of dust! Note position of the Sun, just over half way out. This Class (Lecture 28): More Milky Way

Side View. disk mostly young stars and lots of dust! Note position of the Sun, just over half way out. This Class (Lecture 28): More Milky Way This Class (Lecture 28): More Milky Way Next Class: Nearby Galaxies Music: Under the Milky Way The Church HW 10 due on 2 nd Sunday! Nov. 17, 2009! The 2009 Leonids could produce more than 500 shooting

More information

Formation of the Solar System Chapter 8

Formation of the Solar System Chapter 8 Formation of the Solar System Chapter 8 To understand the formation of the solar system one has to apply concepts such as: Conservation of angular momentum Conservation of energy The theory of the formation

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

Our Planetary System & the Formation of the Solar System

Our Planetary System & the Formation of the Solar System Our Planetary System & the Formation of the Solar System Chapters 7 & 8 Comparative Planetology We learn about the planets by comparing them and assessing their similarities and differences Similarities

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

PProbing New Planet Views Forming on Disks: INTRODUCTION! Contributions from Spitzer and Ground-based Facilities. Joan Najita (NOAO)

PProbing New Planet Views Forming on Disks: INTRODUCTION! Contributions from Spitzer and Ground-based Facilities. Joan Najita (NOAO) PProbing New Planet Views Forming on Disks: Gas Clues in the to the Planet Origins Formation of Planetary Region Systems! of Disks INTRODUCTION! Contributions from Spitzer and Ground-based Facilities Joan

More information

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

2018 TIARA Summer School Origins of the Solar System. Observations and Modelling of Debris Disks. J.P. Marshall (ASIAA) Wednesday 18 th July 2018 2018 TIARA Summer School Origins of the Solar System Observations and Modelling of Debris Disks J.P. Marshall (ASIAA) Wednesday 18 th July 2018 [Hogerheijde 1998] Debris disks Tenuous belts of icy and

More information

Super-Earths as Failed Cores in Orbital Migration Traps

Super-Earths as Failed Cores in Orbital Migration Traps Super-Earths as Failed Cores in Orbital Migration Traps Yasuhiro Hasegawa (Jet Propulsion Laboratory, California Institute of Technology) Hasegawa 2016, ApJ, 832, 83 Copyright 2017. All rights reserved.

More information

PART 3 Galaxies. Gas, Stars and stellar motion in the Milky Way

PART 3 Galaxies. Gas, Stars and stellar motion in the Milky Way PART 3 Galaxies Gas, Stars and stellar motion in the Milky Way The Interstellar Medium The Sombrero Galaxy Space is far from empty! Clouds of cold gas Clouds of dust In a galaxy, gravity pulls the dust

More information

Star Formation. Answering Fundamental Questions During the Spitzer Warm Mission Phase

Star Formation. Answering Fundamental Questions During the Spitzer Warm Mission Phase Star Formation Answering Fundamental Questions During the Spitzer Warm Mission Phase Lori Allen CfA John Carpenter, Caltech Lee Hartmann, University of Michigan Michael Liu, University of Hawaii Tom Megeath,

More information

Other Planetary Systems (Chapter 13) Extrasolar Planets. Is our solar system the only collection of planets in the universe?

Other Planetary Systems (Chapter 13) Extrasolar Planets. Is our solar system the only collection of planets in the universe? Other Planetary Systems (Chapter 13) Extrasolar Planets Is our solar system the only collection of planets in the universe? Based on Chapter 13 No subsequent chapters depend on the material in this lecture

More information

arxiv: v1 [astro-ph.sr] 4 Feb 2014

arxiv: v1 [astro-ph.sr] 4 Feb 2014 Draft version February 5, 2014 Preprint typeset using L A TEX style emulateapj v. 5/2/11 LARGE-SCALE ASYMMETRIES IN THE TRANSITIONAL DISKS OF SAO 206462 AND SR 21 Laura M. Pérez 1,2, Andrea Isella 3, John

More information

Akimasa Kataoka (NAOJ fellow, NAOJ)

Akimasa Kataoka (NAOJ fellow, NAOJ) Investigating planet formation by FIR and sub-mm polarization observations of protoplanetary disks The Astrophysical Journal Letters, 844:L5 (5pp), 2017 July 20 ALMA Band 7 (870 µm) essential. The wavelength

More information

Astro 1010 Planetary Astronomy Sample Questions for Exam 3

Astro 1010 Planetary Astronomy Sample Questions for Exam 3 Astro 1010 Planetary Astronomy Sample Questions for Exam 3 Chapter 6 1. Which of the following statements is false? a) Refraction is the bending of light when it passes from one medium to another. b) Mirrors

More information

8. Solar System Origins

8. Solar System Origins 8. Solar System Origins Chemical composition of the galaxy The solar nebula Planetary accretion Extrasolar planets Our Galaxy s Chemical Composition es Big Bang produced hydrogen & helium Stellar processes

More information

The evolution of a Solar-like system. Young Solar-like Systems. Searching for Extrasolar Planets: Motivation

The evolution of a Solar-like system. Young Solar-like Systems. Searching for Extrasolar Planets: Motivation Young Solar-like Systems The evolution of a Solar-like system FIG.2. Panels(a),(b),and(c)show2.9,1.3,and0.87mmALMAcontinuum images of HL Tau. Panel (d) shows the 1.3 mm psf for the same FOV as the other

More information

HW #2. Solar Nebular Theory. Predictions: Young stars have disks. Disks contain gas & dust. Solar System should contain disk remnants

HW #2. Solar Nebular Theory. Predictions: Young stars have disks. Disks contain gas & dust. Solar System should contain disk remnants Astronomy 330: Extraterrestrial Life This class (Lecture 9): Next Class: Planet Formation Zachary Brewer Quinn Calvert Exoplanets Itamar Allali Brian Campbell-Deem HW #3 due Sunday night. Music: Another

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

Radial Dust Migration in the TW Hydra protoplanetary disk

Radial Dust Migration in the TW Hydra protoplanetary disk Radial Dust Migration in the TW Hydra protoplanetary disk Sarah Maddison (Swinburne) Christophe Pinte, François Ménard, Wing-Fai Thi (IPAG Grenoble), Eric Pantin (CEA-Paris), Jean-François Gonzalez (Lyon),

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

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

Tue 16:40-16:55 M. Tamura AO188

Tue 16:40-16:55 M. Tamura AO188 HiCIAO Early Result from SEEDS and The Subaru s Next Step 2011.5.3 Tue 16:40-16:55 M. Tamura AO188 SEEDS Strategic Exploration of Exoplanets and Disks with Subaru First Subaru Strategic Program (SSP) a

More information

Chapter 19 Reading Quiz Clickers. The Cosmic Perspective Seventh Edition. Our Galaxy Pearson Education, Inc.

Chapter 19 Reading Quiz Clickers. The Cosmic Perspective Seventh Edition. Our Galaxy Pearson Education, Inc. Reading Quiz Clickers The Cosmic Perspective Seventh Edition Our Galaxy 19.1 The Milky Way Revealed What does our galaxy look like? How do stars orbit in our galaxy? Where are globular clusters located

More information

Star Formation. Spitzer Key Contributions to Date

Star Formation. Spitzer Key Contributions to Date Star Formation Answering Fundamental Questions During the Spitzer Warm Mission Phase Lori Allen CfA John Carpenter, Caltech Lee Hartmann, University of Michigan Michael Liu, University of Hawaii Tom Megeath,

More information

The ALMA SKA Synergy For Star and Stellar Cluster Formation

The 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 information

Interstellar molecules: from cores to disks

Interstellar molecules: from cores to disks Interstellar molecules: from cores to disks Ewine F. van Dishoeck Leiden Observatory Thanks to the c2d and DIGIT teams and many others and i.p. our PhD students! April 25, 2013 Nealfest, Austin, TX My

More information

Planetary System Stability and Evolution. N. Jeremy Kasdin Princeton University

Planetary System Stability and Evolution. N. Jeremy Kasdin Princeton University Planetary System Stability and Evolution N. Jeremy Kasdin Princeton University (Lots of help from Eric Ford, Florida and Robert Vanderbei, Princeton) KISS Exoplanet Workshop 10 November 2009 Motivation

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

Kevin France University of Colorado AXIS Science Workshop August 6 th 2018

Kevin France University of Colorado AXIS Science Workshop August 6 th 2018 Kevin France University of Colorado AXIS Science Workshop August 6 th 2018 Star-Planet Interactions at High-energies Introduction: In the solar system: Solar Influences, Living with a Star, etc. Afar:

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

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

Clicker Question: Clicker Question: What is the expected lifetime for a G2 star (one just like our Sun)?

Clicker Question: Clicker Question: What is the expected lifetime for a G2 star (one just like our Sun)? How Long do Stars Live (as Main Sequence Stars)? A star on Main Sequence has fusion of H to He in its core. How fast depends on mass of H available and rate of fusion. Mass of H in core depends on mass

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

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

Global models of planetary system formation. Richard Nelson Queen Mary, University of London

Global models of planetary system formation. Richard Nelson Queen Mary, University of London Global models of planetary system formation Richard Nelson Queen Mary, University of London Hot Jupiters Cold Jupiters Super-Earths/ Neptunes 2 Sumi et al (2016) Occurence rates 30-50% of FGK stars host

More information

Structure of the Milky Way. Structure of the Milky Way. The Milky Way

Structure of the Milky Way. Structure of the Milky Way. The Milky Way Key Concepts: Lecture 29: Our first steps into the Galaxy Exploration of the Galaxy: first attempts to measure its structure (Herschel, Shapley). Structure of the Milky Way Initially, star counting was

More information

How migrating geese and falling pens inspire planet formation

How migrating geese and falling pens inspire planet formation How migrating geese and falling pens inspire planet Common Seminar, Department of Astronomy and Theoretical Physics Lund University, November 2010 About me Biträdande universitetslektor (associate senior

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

The Galaxy. (The Milky Way Galaxy)

The Galaxy. (The Milky Way Galaxy) The Galaxy (The Milky Way Galaxy) Which is a picture of the Milky Way? A A is what we see from Earth inside the Milky Way while B is what the Milky Way might look like if we were far away looking back

More information

Chapter 15 The Formation of Planetary Systems

Chapter 15 The Formation of Planetary Systems Chapter 15 The Formation of Planetary Systems Units of Chapter 15 15.1 Modeling Planet Formation 15.2 Formation of the Solar System 15.3 Terrestrial and Jovian Planets 15.4 Interplanetary Debris 15.5 Solar

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

Cradle of Life Science Working Group

Cradle of Life Science Working Group Report from the Cradle of Life Science Working Group Andrea Isella (Rice), Arielle Moullet (NRAO), Chat Hull (CfA) Collaborators and Contributors John Tobin (Leiden) Laurent Loinard James di Francesco

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

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

The Milky Way - Chapter 23

The Milky Way - Chapter 23 The Milky Way - Chapter 23 The Milky Way Galaxy A galaxy: huge collection of stars (10 7-10 13 ) and interstellar matter (gas & dust). Held together by gravity. Much bigger than any star cluster we have

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

Chapter 14 The Milky Way Galaxy

Chapter 14 The Milky Way Galaxy Chapter 14 The Milky Way Galaxy Spiral Galaxy M81 - similar to our Milky Way Galaxy Our Parent Galaxy A galaxy is a giant collection of stellar and interstellar matter held together by gravity Billions

More information

The dynamical evolution of the asteroid belt in the pebble accretion scenario

The dynamical evolution of the asteroid belt in the pebble accretion scenario The dynamical evolution of the asteroid belt in the pebble accretion scenario S. Pirani 1, A. Johansen 1, B. Bitsch 1, A. J. Mustill 1 and D. Turrini 2,3 1 Lund Observatory, Department of Astronomy and

More information