Architecture of planetary systems:HR 8799 and ε Eridani
Martin ReidemeisterA. V. Krivov1, T. Lohne1, S. Muller1, T. O. B. Schmidt1, S. Fiedler1,
C. C. Stark2 and J.-C. Augereau3
1 Astrophysikalisches Institut und Universitats-Sternwarte JenaSchillergaßchen 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 5571Universite 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 plane
Sky planeLine of nodes
N
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
Fν
[mJy
]
λ [µm]
101
102
10 100 1000
Fν
[mJy
]
λ [µm]
ring dring cdring bcring bbest fit
101
102
10 100 1000
Fν
[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: 30M� 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: 30M� 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 planet
intermediate (10-55AU)
inner (<10AU)
planet 'A'planet 'B'
0
0.5
1
1.5
2
10 100 1000
exce
ss fl
ux [J
y]
wavelength [µm]
IRASMIPS
MIPS (SED)SHARC II
SCUBA
“The cold origin of the warm dust”
M. Reidemeister et al. (AIU Jena) Architecture of planetary systems 15.11.2010 10 / 13
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
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