Download Water ice lines around super-Jovian planets and Implications for

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Water ice lines around super-Jovian planets and
Implications for giant moons
René Heller
In collaboration with
Ralph Pudritz (McMaster University, CAN)
Rory Barnes
(University of Washington, USA)
Simon Albrecht (Århus University, DK)
the content of this talk has been modified
to comply with publication embargos
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Why bother about moons?
They tell us about the fine structure of planet formation.
(1) Earth and Moon formed after a giant collision (Hartmann & Davis 1975).
(2) The Galilean moons constrain the late stages in Jupiter’s accretion disk
(Canup & Ward 2006).
(3) The tilt of Uranian moon system suggests multiple giant impacts on
the young Uranus (Morbidelli+ 2012).
(4) Neptune captured Triton from a minor body binary (Agnor & Hamilton 2006).
Moons could outnumber planets in the stellar HZs (Heller & Barnes 2014).
René Heller
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Why bother about exomoons?
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They could be detectable with Kepler and Plato 2.0.
• The “Hunt for Exomoons with Kepler” (Kipping et al. 2012) searches TTV and
TDV of transiting planets.
René Heller
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Why bother about exomoons?
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They could be detectable with Kepler and Plato 2.0.
• Ganymede-sized moons can be detected by Kepler and Plato 2.0 (Heller 2014).
Saturn-sized exoplanet with moon transiting a 0.57 R⨀ star
Kepler light curve compared to models
Stellar Brightness [%]
detrended Kepler data
no moon
Ganymede-sized moon
slope indicates
an exomoon
Time around mid-transit [hours]
René Heller
Downlo
in of b Pictoris in the fall of 2009. The data do not
show such a source (fig. S2). On the contrary, the
=1408.6164
al source position in fall 2009 is compatible with the
ar, projected position in November 2003 if the source
w- is gravitationally bound to the star (see below).
Based on the system age, distance, and
ne A CRIRES-like
spectrograph
at
E-ELT
can
determine
nd apparent brightness of the companion, the widely
used Baraffe
et al.via
(23)the
evolutionary
models
ar, orbital
motion
Rossiter-McLaughlin
effect.
ky predict a mass of ~9 T 3 Jupiter masses (MJup).
Why bother about exomoons?
rons) with the VLT/NaCo instrument in November 2003
beta
Pic
b
mages of the comparison star HR2435 to estimate and
ts are obtained when using angular differential imaging
(Lagrange et al. 2010, NaCo @ VLT)
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a moon’s sense of
(Heller & Albrecht 2014, submitted)
René Heller
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Can giant planets form giant moons?
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We trace H2O ice lines in accretion disks around super-Jovian planets
(Heller & Pudritz 2014, submitted).
• 2D semi-analytical model
in vertical hydrostatic balance
(based on Canup & Ward 2006;
Makalkin & Dorofeeva 2014;
Machida+ 2008; Mordasini 2013)
FIGURE UNDER
PUBLICATION EMBARGO
• rotationally symmetric
circumplanetary disk with
(1) planetary irradiation
(2) viscous heating
(3) accretional heating
(4) heating from the ambient stellar nebula
René Heller
1408.6164
1403.5839
H2O ice lines around accreting super-Jovians
FIGURE UNDER
PUBLICATION EMBARGO
M13 = Mordasini (2013) — Thanks Christoph!
René Heller
1408.6164
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René Heller
1408.6164
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H2O ice lines around accreting super-Jovians
FIGURE UNDER
PUBLICATION EMBARGO
(Heller & Pudritz 2014, submitted)
René Heller
1408.6164
1403.5839
H2O ice lines around accreting super-Jovians
We randomize disk opacities (κP) and shutdown accretion rates (Ṁshut).
Dust-to-mass ratio is X = 0.006, all planets are at 5.2 AU from a Sun.
FIGURE UNDER
PUBLICATION EMBARGO
(Heller & Pudritz 2014, submitted)
René Heller
1408.6164
1403.5839
H2O ice lines around accreting super-Jovians
FIGURE AND CONCLUSIONS
UNDER
PUBLICATION EMBARGO
René Heller
1403.5839
20
20
If we further inspect Fig
Mass Mass
[M!] [M!]
Population synthesis method
points to a statistically sign
20
104
mass of approximately 40 E
tary desert”, Ida & Lin 2004
3
10
15 interesting question f
103
a very
15
that
will
be
discussed
later
o
3
Jupiter
10
Jupiter
Jupiter
et al.152011).
The
semimajor
axis
distr
2
10
Jupiter
Saturn
2
Saturn
10
Saturn
function
are two fundamen
10
10 encoded into the a-M
that
are
2
10
Saturn
Neptune
are
(besides
of
the
radius
di
Neptune
10
Uranus
Neptune
statistical studies
(e.g., Ida
Uranus
10
Uranus
UranusNeptune
Uranus
10
2008;
Mordasini
et
al.
2009a
Uranus
5
Radial velocity
Uranus
retical5results with
Kolmog
10
Venus
Radial
velocity
& Transits
et al. 52009b).
The planetary
Earth
Earth
Venus
&
Transits
Microlensing
1
Radial
velocity
Earthin Sect. 6.1.
ther addressed
Earth
Venus
Venus
Earth
Microlensing
Direct
imaging
1
& Transits
Nep
In the Earth
figure there are
Venus Earth
Venus
Direct
imaging
Microlensing
0
1
Nt
ered
by
direct
imaging.
In
Direct
imaging
0,1 Venus 1
1
10
10
102
10–2
0
Nep
course
not
the
mass,
but
th
0,1 Semimajor
1 axis [AU] 10
1 of luminosity
10
102 conversion
10–2
0
Mass i[
0,1 Semimajor
1 axis [AU] 10
1
10 Mass
102
10–2
and uncertain as shown by
Semimajor axis [AU]
& Burrows (2012). InMass
Mord[
Fig.
1.
Semimajor
axis
mass
diagram
of
extrasolar
planfor planets
of
Fig. III.1.1: Two of the most
important2014)
statistical observational mass-radius
(Mordasini+
pointed outlines
which
is
impor
René Heller
ets. The colors show the observational technique that was
10
102
103
Mass
[M!
]
Mass
[Earth
masses]
0
1
Neptune
III. Selected
Research Areas
4
4
1010
alone. An example are the observational constraints
coming from the M – R diagram on the extent of orbital
migration. Efficient inward migration brings ice-dominated, low-density planets from the outer parts of the
disk close to the star. These planets can be distinguished
from planets consisting only of silicates and iron, which
have presumably formed in situ in the inner, hotter parts
of the disk. In future, the atmospheric composition of
exoplanets as measured by, e.g., the planned EChO mission will provide additional,
important
constraints.
Radius
[R
]
Radius
[R
]
Earth
Earth
Radius
[REarth
]
Another important goal of population synthesis that
goes beyond the purely planetary properties is to understand the correlations between planetary and host star
properties.
H O ice linesC.around
accreting
super-Jovians
Mordasini et al.: Global Models of Planet Formation and Evol
III.Selected
SelectedResearch
ResearchAreas
Areas
III.
2
mass-radius lines for planets of different compositions. In both
panels, the planets of the Solar System are also shown. Note
that these figures are not corrected for the various observational
biases, which favor for the radial velocity and the transit technique the detection of close-in, giant planets.
104
1408.6164
1403.5839
10
102
103
Mass
[M!
]
Mass
[Earth
masses]
104
3
10
103
103
20
20
If we further inspect Fig
Jupiter
Jupiter
Jupiter
points tosuper-Jovians
a statistically sign
These
20
mass of approximately 40 E
should
be orbited
tary desert”,
Ida & Linby
2004
15 interesting question f
a very
15
Mars-mass
moons!
that will be discussed later o
Population synthesis method
et al.152011).
The
semimajor
axis
distr
2
10
Jupiter
Saturn
2
Saturn
10
Saturn
function
are two fundamen
10
10 encoded into the a-M
that
are
2
10
Saturn
Neptune
are
(besides
of
the
radius
di
Neptune
10
Uranus
Neptune
statistical studies
(e.g., Ida
Uranus
10
Uranus
UranusNeptune
Uranus
10
2008;
Mordasini
et
al.
2009a
Uranus
5
Radial velocity
Uranus
retical5results with
Kolmog
10
Venus
Radial
velocity
& Transits
et al. 52009b).
The planetary
Earth
Earth
Venus
&
Transits
Microlensing
1
Radial
velocity
Earthin Sect. 6.1.
ther addressed
Earth
Venus
Venus
Earth
Microlensing
Direct
imaging
1
& Transits
Nep
In the Earth
figure there are
Venus Earth
Venus
Direct
imaging
Microlensing
0
1
Nt
ered
by
direct
imaging.
In
Direct
imaging
0,1 Venus 1
1
10
10
102
10–2
0
Nep
course
not
the
mass,
but
th
0,1 Semimajor
1 axis [AU] 10
1 of luminosity
10
102 conversion
10–2
0
Mass i[
0,1 Semimajor
1 axis [AU] 10
1
10 Mass
102
10–2
and uncertain as shown by
Semimajor axis [AU]
& Burrows (2012). InMass
Mord[
Fig.
1.
Semimajor
axis
mass
diagram
of
extrasolar
planfor planets
of
Fig. III.1.1: Two of the most
important2014)
statistical observational mass-radius
(Mordasini+
pointed outlines
which
is
impor
René Heller
ets. The colors show the observational technique that was
Mass Mass
[M!] [M!]
0
1
Neptune
III. Selected
Research Areas
4
4
1010
alone. An example are the observational constraints
coming from the M – R diagram on the extent of orbital
migration. Efficient inward migration brings ice-dominated, low-density planets from the outer parts of the
disk close to the star. These planets can be distinguished
from planets consisting only of silicates and iron, which
have presumably formed in situ in the inner, hotter parts
of the disk. In future, the atmospheric composition of
exoplanets as measured by, e.g., the planned EChO mission will provide additional,
important
constraints.
Radius
[R
]
Radius
[R
]
Earth
Earth
Radius
[REarth
]
Another important goal of population synthesis that
goes beyond the purely planetary properties is to understand the correlations between planetary and host star
properties.
H O ice linesC.around
accreting
super-Jovians
Mordasini et al.: Global Models of Planet Formation and Evol
III.Selected
SelectedResearch
ResearchAreas
Areas
III.
2
mass-radius lines for planets of different compositions. In both
panels, the planets of the Solar System are also shown. Note
that these figures are not corrected for the various observational
biases, which favor for the radial velocity and the transit technique the detection of close-in, giant planets.
104
1408.6164
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1403.5839
Predictions
FIGURE AND CONCLUSIONS
UNDER
PUBLICATION EMBARGO
René Heller
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