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1. Imke
de
Pater
(UC
Berkeley)
Outline
• Jupiter:
the
planet
• Why
study
Jupiter?
Origin
of
our
Solar
System
• Recent
work
by
our
group
• The
Juno
Mission
HST/NASA

2. • Largest
planet
in
our
SS
• ~12
x
larger
than
Earth
• ~300
times
more
mass
• ~85%
H2,
15%
He
• trace
amounts
CH4,
NH3,
H2O,
H2S
(on
Sun:
C,N,O,S)
Cassini,
Oct.
31
– Nov.
9,
2000
HST/NASA

3. Cassini,
Oct.
31
– Nov.
9,
2000
HST/NASA
So,
Why
study
Jupiter?

4. • Composition
and
internal
structure
Jupiter
à
information
on
conditions
of
our
solar
nebula
during
the
time
the
Sun
and
planets
formed.
Fundamental
Question:
How
did
our
Solar
System
Form?
Composition
of
a
planet
can
be
determined
through
remote
sensing
or
in
situ
(probe)

5. IRTF
20
0
titude
o
o
a b c
Visible
(HST)
5
µm
(IRTF)
2
cm
(VLA)
1995-­‐1996:
Galileo
Probe
entry
Determine
composition
through
observations
at
different
wavelengths
Beebe
Ortiz
et
al.,
1998 de
Pater
et
al.
2001

6. IRTF
20
0
titude
o
o
a b c
Visible
(HST)
5
µm
(IRTF)
2
cm
(VLA)
1995-­‐1996:
Galileo
Probe
entry
Radio: clouds
are
transparant;
Most
of
the
opacity
is
caused
by
NH3 gas.
At
longer
wavelengths
radiation
is
received
from
deeper
levels
in
the
atmosphere.
à NH3
abundance
very
similar
to
solar
N
value.
Beebe
Ortiz
et
al.,
1998 de
Pater
et
al.
2001

7. Two
questions
surface:
• What
is
the
H2O
abundance
in
Jupiter’s
deep
atmosphere?
• How
to
reconcile
the
groundbased (radio)
measurement
of
NH3 with
the
Galileo
Probe
data?
Owen
et
al.
1999

8. How
can
we
“loose”
NH3 gas
between
4 and
8
bar?
• Chemistry;
perhaps
H2S
binds
with
more
than
1
NH3
molecules?
Or
the
water
cloud
takes
up
more
NH3
than
hitherto
assumed?
Lab
work
ongoing
• Dynamics:
updrafts,
downdrafts,
drying
out
air,
as
the
zone-­‐belt
generic
picture.
10–16
10–14
10–12
10–10
10–8
Cloud density rate Rx
(g cm–3
cm–1
)
300
250
200
150
Temperature(K)
7.0
5.0
4.0
3.0
2.0
1.5
1.0
0.5
0.75
Pressure(bar)
Water solution
Water ice
NH4
SH solid
NH3
ice
Wong
et
al.,
2014

9. In
order
to
solve
the
NH3 and
H2O
questions,
we
obtained
data
to
probe
below
Jupiter’s
clouds:
• Spectroscopic
data
at
5
µm
• Maps
at
radio
wavelengths
at
2-­‐6
cm
(4-­‐18
GHz)
De
Pater
et
al.,
2011
5-­‐µm
image
of
Jupiter’s
northern
hemisphere.
In
hot
regions
(hot
spots,
5-­‐µm
rings
around
vortices)
we
probe
down
to
5-­‐7
bar

10. Bjoraker et
al.,
2015
Zones
exhibit
narrow
CH3D
line
profiles.
Modeling
indicates
the
presence
of
a
cloud
at
~4
bars,
which
must
be
a
water
cloud.
à Consistent
with
historical
picture
of
rising
air
in
zones,
sinking
in
belts;
H2O
must
be
>1.2
x
solar
O.
Hot
Spots,
Belts,
and
high-­‐latitude
regions
exhibit
broad
CH3D
line
profiles
àprobing
~7
bar
àNo
opaque
H2O
clouds.
5-­‐µm
Spectra

11. de
Pater
et
al.,
2016
Radio
observations
at
2
-­‐ 6
cm
(or
4
– 18
GHz)
NH3
Solution
H2
O
NH4
SH
Equilibrium NH3
(Fig. 3A, profile a)
Depleted NH3
(Fig. 3A, profile e)
17.4 GHz
4.42 GHz
7.45 GHz
11.5 GHz
14.2 GHz
1.46 GHz
17.4 GHz
4.42 GHz
7.45 GHz
11.5 GHz
14.2 GHz
1.46 GHz
A B
Fig. 1
0
10
1
0.1
10
1
0.1
0.5 1 1.5
100 200 300 400
Normalized contribution functions
Pressure(bar)
Pressure(bar)
Temperature (K)
0 0.5 1 1.5
100 200 300 400
Normalized contribution functions
Temperature (K)

12. JUPITER:
Radio spectrum
Temperature (K)
De
Pater
et
al.,
2016
NH4SH
à
NH3-­‐ice
à

13. brg c
Temperature (K)
TP profile
de
Pater
et
al.,
2016

14. de
Pater
et
al.,
2016
2
cm
2
cm
6 cm
3.5
cm

15. de
Pater
et
al.,
2016

16. SUMMARY:
• Microwave
maps
show
spatial
variations
in
Tb,
resembling
visible
light
maps.
• Radio-­‐hot
belt
at
~8
deg N
• Localized
NH3 depletions
(hot
spots)
down
to
>
8
bar
• Localized
upwellings (plumes)
from
P
>
8
bar:
planetary
wave,
connecting
the
5-­‐µm hot
spots
and
plumes.
• Plumes
explain
radio
– Galileo
conundrum

17. NASA’s
Juno
Mission
• Launch
Aug
5th 2011.
• Arrival
July
4th 2016
• 2700
miles
above
the
jovian
cloud
tops
in
a
polar
orbit
• Key
goals:
– Gravity
field
mapping
to
detect
the
presence
of
a
core.
– Microwave
mapping
to
peer
beneath
the
clouds,
constrain
oxygen.
• 32
orbits:
1-­‐8
for
remote
sensing
and
microwave.
• 9-­‐32
for
gravity
mapping
• De-­‐orbit
March
2018.
Slide
adapted
from
Orton

18. 26
Juno’s
Specific
Science
Objectives
Origin
Determine
water
abundance
and
constrain
core
mass
to
decide
among
alternative
theories
of
origin.
Interior
Understand
Jupiter's
interior
structure
and
dynamical
properties
by
mapping
its
gravitational
and
magnetic
fields
Atmosphere
Map
variations
in
atmospheric
composition,
cloud
opacity
and
dynamics
to
depths
greater
than
100
bars
at
all
latitudes.
Magnetosphere
Characterize
the
three-­‐dimensional
structure
of
Jupiter's
polar
magnetosphere
and
auroras.
Slide
adapted
from
Orton

19. Probing
the
deep
interior
from
orbit
Juno
maps
Jupiter
from
the
deepest
interior
to
the
atmosphere
using
microwaves,
and
magnetic
and
gravity
fields.
Slide
adapted
from
Orton

20. Mapping
Jupiter’s
gravity
Tracking
changes
in
Juno’s
velocity
reveals
Jupiter’s
gravity
(and
how
the
planet
is
arranged
on
the
inside).
Precise
Doppler
measurements
of
spacecraft
motion
reveal
the
gravity
field.
Slide
adapted
from
Orton

21. Juno’s Microwave Radiometer
measures thermal radiation from
the atmosphere to as deep as a
few 100 bar pressure (few 100 km
below the visible cloud tops).
Sensing
the
deep
atmosphere
Goal: to determine the 3D
H2O and NH3 abundances.

22. Sensing
the
deep
atmosphere
At
wavelengths
>
6
cm
(freqs<
4
GHz)
Jupiter’s
synchrotron
radiation
makes
it
very
difficult
to
map
the
atmosphere
from
the
Earth.
Juno
flies
inside
the
radiation
belts.
VLA
map
at
21
cm;
de
Pater
et
al.,
1997
Juno’s
field
of
view
is
tiny
à need
context
maps.

23. Slide
adapted
from
Bagenal
Mapping
Jupiter’s
magnetic
field
and
aurora
HST/NASA

24. Ground-­‐based
observing
campaign
to
support
Juno
• Dedicated
network
of
amateur
astronomers.
• Many
telescopes
allocated
time,
from
X-­‐rays
to
uv-­‐visible,
near-­‐
and
mid-­‐infrared,
and
radio
from
cm—m
wavelengths.
• Unique
opportunity
to
characterize
Jupiter’s
atmosphere
from
the
stratosphere
down
to
100’s
of
bars.
Time
variability
mandates
simultaneous
data
to
fully
characterize
the
planet.
• Synergy
VLA
&
Juno:
VLA
provides
context
maps
to
put
Juno
MWR
data
in
perspective;
Juno
extends
the
information
to
much
deeper
levels.
Juno
also
has
a
superb
view
of
the
poles.