Architecture of planetary systems: HR8799 and Eridani · two dust rings gas giants in between"...

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Architecture of planetary systems: HR 8799 and ε Eridani Martin Reidemeister A. V. Krivov 1 , T. L¨ ohne 1 , S. M ¨ uller 1 , T. O. B. Schmidt 1 , S. Fiedler 1 , C. C. Stark 2 and J.-C. Augereau 3 1 Astrophysikalisches Institut und Universit¨ ats-Sternwarte Jena Schillerg ¨ aßchen 2-3, 07745 Jena 2 Department of Physics, University of Maryland Box 197, 082 Regents Drive, College Park, MD 20742-4111 3 Laboratoire d’Astrophysique de Grenoble, CNRS UMR 5571 Universit ´ e Joseph Fourier, Grenoble, France 15.11.2010 M. Reidemeister et al. (AIU Jena) Architecture of planetary systems 15.11.2010 1 / 13
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Transcript of Architecture of planetary systems: HR8799 and Eridani · two dust rings gas giants in between"...

  • Architecture of planetary systems:HR 8799 and ε Eridani

    Martin ReidemeisterA. V. Krivov1, T. Löhne1, S. Müller1, T. O. B. Schmidt1, S. Fiedler1,

    C. C. Stark2 and J.-C. Augereau3

    1 Astrophysikalisches Institut und Universitäts-Sternwarte JenaSchillergäßchen 2-3, 07745 Jena

    2 Department of Physics, University of MarylandBox 197, 082 Regents Drive, College Park, MD 20742-4111

    3 Laboratoire d’Astrophysique de Grenoble, CNRS UMR 5571Université Joseph Fourier, Grenoble, France

    15.11.2010

    M. Reidemeister et al. (AIU Jena) Architecture of planetary systems 15.11.2010 1 / 13

  • Content

    1 Introduction

    2 HR 8799

    3 ε Eridani

    4 Summary

    M. Reidemeister et al. (AIU Jena) Architecture of planetary systems 15.11.2010 2 / 13

  • Introduction

    DefinitionArchitecture of planetary system:

    starplanet(s)dustplanetesimal belts(source of dust)

    Motivationmultiple interactions betweendust, planetesimals and planetsconstrain planet masses,eccentricity, inclinationplanetesimals are remnants ofplanet formation

    M. Reidemeister et al. (AIU Jena) Architecture of planetary systems 15.11.2010 3 / 13

  • Introduction

    DefinitionArchitecture of planetary system:

    starplanet(s)dustplanetesimal belts(source of dust)

    Motivationmultiple interactions betweendust, planetesimals and planetsconstrain planet masses,eccentricity, inclinationplanetesimals are remnants ofplanet formation

    M. Reidemeister et al. (AIU Jena) Architecture of planetary systems 15.11.2010 3 / 13

  • Content

    1 Introduction

    2 HR 8799

    3 ε Eridani

    4 Summary

    M. Reidemeister et al. (AIU Jena) Architecture of planetary systems 15.11.2010 4 / 13

  • HR 8799 – Introduction

    ParametersA5 V star with d = 39.4 pcage of . 50 Myr Reidemeister et al. (2009)(20 Myr up to 1 Gyr)γ Doradus (variable star)λ Bootis (metalpoor Pop. I)

    Observationsstrong IR excess (IRAS, ISO)Sadakane&Nishida (1986), Zuckerman&Song (2004),

    Moor et al. (2006), Rhee et al. (2007)

    Spitzer/IRS spectrumJura et al. (2004), Chen et al. (2006)

    3 directly imaged planetsat 68, 38 & 24 AUwith MP =5–13MJup

    100

    101

    102

    10310

    −4

    10−2

    100

    wavelength [µm]

    flux

    [Jy]

    Marois et al. (2008)

    M. Reidemeister et al. (AIU Jena) Architecture of planetary systems 15.11.2010 5 / 13

  • HR 8799 – The planets

    toE

    arth

    System' sangularmomentum

    System' s

    symmetry plan

    e

    Sky p

    laneLine of

    nodesN

    E

    W

    i

    Resultsinclination of 20–30◦

    (rotational period: 13–30◦)rotation angle of 0–50◦

    slipping in 1:2:4 resonance

    2:1 b-c

    2:1 c-d

    duration of stability in years

    0 20 40 60 80 100 120 140 160 180

    rotation angle [deg]

    0

    5

    10

    15

    20

    25

    30

    35

    40

    45

    incl

    inat

    ion

    angl

    e [d

    eg]

    103

    104

    105

    106

    107

    108

    2:1 b-c

    2:1 c-d

    duration of stability in years

    M. Reidemeister et al. (AIU Jena) Architecture of planetary systems 15.11.2010 6 / 13

  • HR 8799 – The dust

    100AU

    d

    cb

    outer dust disk

    outer ring ofplanetesimals

    planetesimals

    inner ring of

    and dust

    dust ringsouter ring & 100 AUMdust ≈ 4× 10−2M⊕inner ring 2–10 AUMdust ≈ 10−5M⊕

    101

    102

    10 100 1000

    [mJy

    ]

    λ [µm]

    101

    102

    10 100 1000

    [mJy

    ]

    λ [µm]

    ring dring cdring bcring bbest fit

    101

    102

    10 100 1000

    [mJy

    ]

    λ [µm]

    M. Reidemeister et al. (AIU Jena) Architecture of planetary systems 15.11.2010 7 / 13

  • HR 8799

    Stability

    Dust mass

    Ring position

    Planetary mass

    Inclination

    Rotational period

    Age

    M. Reidemeister et al. (AIU Jena) Architecture of planetary systems 15.11.2010 8 / 13

  • Content

    1 Introduction

    2 HR 8799

    3 ε Eridani

    4 Summary

    M. Reidemeister et al. (AIU Jena) Architecture of planetary systems 15.11.2010 9 / 13

  • ε Eridani

    ParameterK2 V star at d = 3.2 pcage . 1 Gyr DiFolco et al. (2004)SW: 30Ṁ� Wood et al. (2002)“Kuiper belt” analog in sub-mmaround 65 AU Greaves et al. (1998, 2005)assumed outer planetRV planet at 3.4 AU Hatzes et al. (2000)A: e = 0.70 Benedict et al. (2006)B: e = 0.25 Butler et al. (2006)Spitzer/IRS spectrum indicateswarm dust at a few AU Backman et al. (2009)

    “The cold origin of the warm dust”

    M. Reidemeister et al. (AIU Jena) Architecture of planetary systems 15.11.2010 10 / 13

  • ε Eridani

    ParameterK2 V star at d = 3.2 pcage . 1 Gyr DiFolco et al. (2004)SW: 30Ṁ� Wood et al. (2002)“Kuiper belt” analog in sub-mmaround 65 AU Greaves et al. (1998, 2005)assumed outer planetRV planet at 3.4 AU Hatzes et al. (2000)A: e = 0.70 Benedict et al. (2006)B: e = 0.25 Butler et al. (2006)Spitzer/IRS spectrum indicateswarm dust at a few AU Backman et al. (2009)

    outer ring (55-90AU)

    oute

    r plan

    et

    intermediate (10-55AU

    )

    inner (

  • ε Eridani – ResultsSpectral energy distribution

    0

    0.5

    1

    1.5

    2

    10 100 1000

    exce

    ss f

    lux [

    Jy]

    wavelength [µm]

    Planet A: a=3.4AU, e=0.70

    0-10AU, 0.05-1.42µm, q=3.010-90AU (ACE)

    totalIRASMIPS

    MIPS (SED)SHARC II

    SCUBA

    M. Reidemeister et al. (AIU Jena) Architecture of planetary systems 15.11.2010 11 / 13

  • ε Eridani – ResultsSurface brightness profile

    10-3

    10-2

    10-1

    100

    101

    0 5 10 15 20 25 30 35 40

    su

    rfa

    ce

    brig

    htn

    ess [

    mJy/a

    rcse

    c2]

    distance [arcsec]

    24µm70µm

    160µmSpitzer/MIPS

    PSF

    M. Reidemeister et al. (AIU Jena) Architecture of planetary systems 15.11.2010 12 / 13

  • Summary

    HR 8799young system (. 50 Myr)- planets with lower mass- high dust masssolar system like architecture:two dust ringsgas giants in between

    ε Eridanigap in the sub-mm indicatesan outer planetinner planetesimal beltunstablemassive dust disk (10−3M⊕)but transport dominateddust can stem from outer ringand supply the inner system

    M. Reidemeister et al. (AIU Jena) Architecture of planetary systems 15.11.2010 13 / 13

    IntroductionHR 8799 EridaniSummary