WATER-ICE CONTENT

IN TITAN AND CALLISTO

Dunaeva A.N., Kronrod V.A., Kuskov O.L.

Vernadsky Institute of Geochemistry and Analytical Chemistry, Russian Academy of Sciences,

Moscow, Russia

Callisto and Titan:were formed in the outer zones of their central planets (Jupiter and Saturn);

are the largest and well-formed satellites of gas giant planets;

are regular satellites (their orbits and rotation are the same as the rotation of associated central planets);

satellites rotation is synchronous with their orbits (like our Moon);

low density of the satellites suggests that they could contain remarkable amounts of H2O.

Jupiter Saturn

Callisto Titan

Models of Titan and Callisto.

Wilson L., 2002

Callisto:

Callisto’s general image from NASA, JPL

Titan:

Grasset et al., 2005 Sohl F. et al., 2003

Mitri et al., 2009

Sohl F., 2010 Titan’s general image from NASA

Models of the satellites internal structure described by the system of following equations: Equations of hydrostatic equilibrium:

,

The equations of the satellites mass and moment of inertia: ,

The equation for calculating ice component concentration in mantle:

High-pressure water ices equations of state.

Physical characteristics of satellites:- Pressure and temperature at the surface, P[bar] , T [K];- Gravity acceleration, [m/s2];- Radius, R [km]- Average density, g/cm3

- Mass, M [kg]- Normalized moment of inertia, I/MR2

RR iii

n

i

I 5

1

5

0158

The initial data for modeling, problem setting and methods of solution

RgRdRdP RRgRG

dRdg 24

RR iii

n

i

M 3

1

3

034

miceSiFem

mSiFemiceiceC

,

,

R

Rg

m

density of the water-ice shell,

average density of ice in mantle,

density of the rock–iron component,

average density of mantle

mice,

SiFe

= 3.15 - 3.62 g/cm3 (LL-chondrites)SiFe

Callisto Titan

Tsurf., K 110 93

M,1024g 107.6 134.6

ρ, g/cm3 1.8344 1.881

RP 26.4 20.25

R, km 2410.3 2575.0

I/MR2 0.3549 0.3414

H(ice), km 330 520

Rcore, km 1280 1490

H2O, wt% 47.6-53.8 45.1-51.6

Comparison of Callisto and Titan.

p a r a m e ter s o f T ita n

para

met

ers

of C

allis

to

I /M R 2 R P MH 2 O T H iceR co re R sat

I/M R 2

R co reR P

H 2 OT

H iceM

R sat

+

+++

Similar characteristic parameters of Callisto and Titan suggest that satellites could be

built from the identical material and have a similar water/rock ratio (being close to 1).

5 10 15 20 25 30Orbital distance (in Rplanet)

0

20

40

60

H2O

, wt %

IoEuropa

GanymedeCallisto

Titan

Water content and density gradients in large icy satellites of Jupiter and Saturn.

5 10 15 20 25 30Orbital distance (in Rplanet)

1 . 6

2

2 . 4

2 . 8

3 . 2

3 . 6

dens

ity, g

/cm

3

Io

Europa

Ganymede CallistoTitan

The blue outline is the model of Titan and the black outline is the model of Callisto.

The specks show the range of parameters in which the same content of H2O in satellites is possible.

The solid and dotted lines within the contours are the lines of the satellites water-ice crust equal thickness (indicated by numbers, in km).

The total content of water in Callisto and Titan

3 3.2 3.4 3.6 3.8density of the Fe-Si component, g/cm3

4 4

4 6

4 8

5 0

5 2

5 4

H2O

, wt %

Callisto

Titan

100 200 300

200300

400

500

330 10

10

1 a

The internal structure of Titan and Callisto.

500

1500

2500

Dis

tanc

e fr

om th

e sa

telli

te's

cen

ter,

km

C a llisto T ita n

500

1500

2500 w a ter-ice sh e ll

ro ck -ice m a n tle

ro ck -iro n co re

“Is Titan just Callisto with weather?”(c) J. Moore Callisto and Titan located in different planetary systems have similar physical characteristics and the same internal structure.

Thus, they can be considered as space satellites-twins.

Conclusion.

Titan and Callisto are partially differentiated satellites, consisting, in general, of an outer ice shell, rock-ice mantle and rock-iron core.

The satellites do not differ in terms of bulk water content which in average is about 50 wt.%.

The satellites differ just a little from each other in density of rock-iron component composing of their inner regions. The density of the satellites’ rock material is in the range of 3.15 - 3.36 g/cm3, which is typical for the hydrated L/LL chondrites.

The equal content of bulk H2O and the same density of the satellites’ rock material allow to have assumption that ice and rock-icy planetesimals, with the similar ice and rock composition, were captured into accretion disks of Jupiter and Saturn, and from this material the satellites of outer planet zone Titan and Callisto were formed.