Issue 
A&A
Volume 596, December 2016



Article Number  A114  
Number of page(s)  12  
Section  Planets and planetary systems  
DOI  https://doi.org/10.1051/00046361/201629732  
Published online  14 December 2016 
Jupiter internal structure: the effect of different equations of state^{⋆}
^{1} Laboratoire Lagrange, UMR 7293,
Université de NiceSophia Antipolis, CNRS, Observatoire de la Côte dAzur, Bd de
l’Observatoire, CS
34229, 06304 Nice Cedex
4, France
email: yamila.miguel@oca.eu
^{2} Institut de Physique du Globe de
Paris, 1 rue
Jussieu, 75005
Paris,
France
^{3} AstroParticule et Cosmologie, 10 rue
Alice Domon et Leonie Duquet, 75013
Paris,
France
Received:
16
September
2016
Accepted:
11
November
2016
Context. Heavy elements, even though they are a smaller constituent, are crucial to understand the formation history of Jupiter. Interior models are used to determine the amount of heavy elements in the interior of Jupiter, but this range is still subject to degeneracies because of the uncertainties in the equations of state.
Aims. Before Juno mission data arrive, we present optimized calculations for Jupiter that explore the effect of different model parameters on the determination of the core and the mass of heavy elements of Jupiter. We compare recently published equations of state.
Methods. The interior model of Jupiter was calculated from the equations of hydrostatic equilibrium, mass, and energy conservation, and energy transport. The mass of the core and heavy elements was adjusted to match the observed radius and gravitational moments of Jupiter.
Results. We show that the determination of the interior structure of Jupiter is tied to the estimation of its gravitational moments and the accuracy of equations of state of hydrogen, helium, and heavy elements. Locating the region where helium rain occurs and defining its timescale is important to determine the distribution of heavy elements and helium in the interior of Jupiter. We show that the differences found when modeling the interior of Jupiter with recent EOS are more likely due to differences in the internal energy and entropy calculation. The consequent changes in the thermal profile lead to different estimates of the mass of the core and heavy elements, which explains differences in recently published interior models of Jupiter.
Conclusions. Our results help clarify the reasons for the differences found in interior models of Jupiter and will help interpreting upcoming Juno data.
Key words: planets and satellites: interiors / planets and satellites: individual: Jupiter / equation of state
Full appendix tables are only available at the CDS via anonymous ftp to cdsarc.ustrasbg.fr (130.79.128.5) or via http://cdsarc.ustrasbg.fr/vizbin/qcat?J/A+A/596/A114
© ESO, 2016
1. Introduction
The internal structure of Jupiter is estimated with interior models that use observational constraints such as its mass, radius, and gravitational moments, which are derived from measurements made with Pioneer and Voyager (Campbell & Synnott 1985). The Juno mission is designed to improve our knowledge of the interior of Jupiter and its formation history by a combination of highly accurate measurements of the gravity and magnetic field of Jupiter as well as of the water abundance in the atmosphere.
Models of the internal structure of Jupiter rely on the study of the properties of hydrogen and helium at high pressures (Saumon & Guillot 2004; Fortney & Nettelmann 2010; Baraffe et al. 2014). One of the most successful equations of state (EOS) was published by Saumon et al. (1995; SCvH) and has been used in numerous publications on the interior calculations of giant planets. Since 1995, development in numerical techniques allowed a new generation of EOS calculated from ab initio simulations (Nettelmann et al. 2008; Militzer et al. 2008; Militzer 2006, 2009; Caillabet et al. 2011; Nettelmann et al. 2012; Militzer & Hubbard 2013; Becker et al. 2014). These equations of state, even though calculated from the same principles and numerical techniques, were used to construct interior models of Jupiter with different results.
While results by Nettelmann et al. (2008) suggested low core masses of up to 8 M_{Earth} consistent with previous estimations (Saumon & Guillot 2004), results by Militzer et al. (2008) challenged the small core hypothesis, finding large cores of 14−18 M_{Earth}. Nettelmann et al. (2012) improved their previous model and equation of state (Nettelmann et al. 2008), and tested different models for the distribution of heavy elements in the interior of Jupiter. They found that a Jupiter model with a homogenous interior plus a core will lead to larger cores that are more consistent with the estimates of Militzer et al. (2008), while a discontinuous distribution of helium and heavy elements plus a core leads to core masses of up to 8 M_{Earth} but a high mass of heavy elements (28−32 M_{Earth}). Nettelmann and collaborators concluded that the differences in the internal structure of Jupiter originate from different model assumptions, a conclusion in agreement with the analysis of Militzer & Hubbard (2009). After these papers, two new results were published. Militzer & Hubbard (2013; MH13) presented a new equation of state for an interacting hydrogenhelium mixture with selfconsistent entropy calculations, and a recent paper by Becker et al. (2014; REOS.3) showed updated tables for hydrogen and helium in a wide range that covers all temperatures and densities in the interior of Jupiter. These recent estimates still present differences in interior calculations of Jupiter, showing that one of the great challenges in modeling the internal structure of Jupiter still rests on the determination and accuracy of the equations of state of hydrogen and helium.
We explore the differences in the internal structure of Jupiter, on the mass of its derived core and heavy elements, calculated with the same model assumptions but different equations of state. We also explore the effect of different equations of state for heavy elements, different locations of the separation between the molecular and metallic layer, and different models for the heavy element distribution in the interior of Jupiter. In anticipation of Juno measurements, we also study the gravitational moments used to constrain the solutions, to obtain a better knowledge of the sensitivity of the interior of Jupiter to different model parameters and understand the implications of Juno measurements on internal structure calculations.
2. Modeling Jupiter
The internal structure of Jupiter is determined from the equations of hydrostatic equilibrium, mass and energy conservation, and energy transport, which are calculated using the code CEPAM (Guillot & Morel 1995). We set the boundary condition at 1 bar to be T = 165 K based on Voyager and Galileo measurements (Lindal 1992; Atkinson et al. 1998), where the mass and luminosity are almost equal to the total mass and luminosity of the planet. In this work, we assume that the envelope structure is adiabatic. We note that the presence of deep radiative zones are unlikely (see Guillot et al. 2004). Some recent work included a nonadiabatic, doublediffusive region in the helium demixing region (Nettelmann et al. 2015; Mankovich et al. 2016), but the effect of this on the inferred core mass and mass of heavy elements is significantly smaller than the uncertainties discussed here. We do not consider the possibility that the envelope is entirely doublediffusive, which would yield vastly larger amounts of heavy elements in the interior (Leconte & Chabrier 2012). We note that dry Ledoux convection tends to homogenize a large part of the envelope (Vazan et al. 2016), implying that this possibility is unlikely.
The helium abundance in the external envelope is taken as Y = 0.238 ± 0.007 to match the in situ observations made by the Galileo probe (Zahn et al. 1998). To explain helium depletion compared to the protosolar value (0.270 ± 0.005, Bahcall & Pinsonneault 1995), we assume that a helium phase transition occurs at a pressure P_{sep}, between 0.8 and 4 Mbar according to the immiscibility calculations of Morales et al. (2013). Helium settles down, increasing the abundance at the deeper layer, which in turn accounts for the depleted amount in the outer envelope. Since the physics and dynamics of helium rain are not understood in detail, we consider two different models for the distribution of solids in the planet interior. In one model helium rain has a fast timescale that allows an efficient mixture of solids in the interior of Jupiter, which has a homogeneous distribution (Zhomogeneous). In the other model we assume that helium rain induces a compositional difference between the two layers, and therefore in this scenario there are two different abundances for the metals in the outer and deeper layer (Zdiscontinuous).
3. Equations of state
3.1. Hydrogen and helium
The proper determination of the internal structure of Jupiter is tied to the accuracy of the equations of state at the range of temperatures and pressures reached in the interior of this giant. Since ~85% of the Jupiter mass is hydrogen and helium, the equations of state of these elements determine its internal structure. Nevertheless, we show that the treatment adopted for the heavy elements also affects the core mass and total mass of heavy elements that are retrieved with our calculations (Sect. 4.2.2).
Fig. 1 Phase diagram of hydrogen (adapted from Guillot & Gautier 2015). The range of validity of each equation of state in the range of the figure is shown in different colors: SCvH is shown in purple, MH13 in blue, and REOS.3 in orange. The internal structure of Jupiter is shown as a green thick line. 

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In this study we use three different equations of state for hydrogen and helium: the widely used Saumon et al. (1995) equations of state, and the more recent equations of state derived from ab initio calculations published by Militzer & Hubbard (2013) and by Becker et al. (2014). Figure 1 shows the phase diagram of hydrogen and the range of pressure and temperature covered by each equation of state.
3.1.1. Pure hydrogen equation of state from results of MH13
The table presented by MH13 lists pressure, internal energy, Helmholtz free energy, and specific entropy as functions of density and temperature, while CEPAM uses tables where entropy and density are given as functions of pressure and temperature. We use cubic spline interpolation to create a table in CEPAM format.
As shown in Fig. 1, the MH13 EOS was made for a small range of pressure and temperature that does not cover all pressures and temperatures in the interior of Jupiter. We extend the table using the SCvH EOS for those temperatures and pressures with no data. To smoothen the limits between the two tables, we use linear interpolation. The new table covers a range of pressures between 10^{4} and 10^{19} g/(cm s^{2}) and a range of temperatures 2.25 ≤ Log(T) ≤ 7 K.
The MH13 EOS was made for a mixture of hydrogen and helium (Y_{MH13} = 0.245). To allow a change in the composition of the molecular and metallic envelopes, we extracted the hydrogen from the table, creating a pure hydrogen equation of state based on MH13 results. We calculated density and entropy for each pressure and temperature in the table using the equations for a mixture and the SCvH equation of state for helium: with ρ_{H} and S_{H} the density and entropy of the pure hydrogen equation of state we extracted from the table of MH13, ρ_{SCvH,He} and S_{SCvH,He} the density and entropy in the helium table of SCvH, X_{MH13}, ρ_{MH13} and S_{MH13} the hydrogen mass fraction, density, and entropy of MH13. Equation (2)neglects the entropy of mixing. Detailed calculations using the SCvH EOS with and without this entropy of mixing show that this is a much smaller effect than the uncertainties on the EOSs themselves discussed here. We call this new hydrogen table MH13+SCvH (shown in Appendix A).
3.1.2. Entropy calculation for hydrogen and helium using REOS.3
Fig. 2 Specific internal energy as a function of density at different temperatures for hydrogen (left panel) and helium (right panel), using two different equations of state. SCvH is shown as green solid lines, and the values shown as blue dotted lines correspond to the u in REOS.3 plus Δu (Δu_{H} = 1590.12135 for hydrogen and Δu_{He} = 1843.06795 for helium) or REOS3b. 

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Fig. 3 Specific entropy vs. density at different temperatures for hydrogen (left panel) and helium (right panel). For hydrogen we show a comparison between the entropy calculated with REOS3b (blue), the one published in SCvH (green), and MH13+SCvH values (red). Since MH13+SCvH is a pure hydrogen table, the right panel shows a comparison between REOS3b and SCvH only. 

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REOS.3 is a densitytemperature equation of state with pressure and specific internal energy that covers a wide range in pressure and temperature (Fig. 1, for hydrogen). To allow comparisons between the tables and avoid errors in the entropy calculation, we changed the zero point of the specific internal energy in the REOS.3 tables to make them coincide in the ideal gas regime with the SCvH EOS (N. Nettelmann and A. Becker, priv. comm.). Since the difference between the specific internal energy of REOS.3 and SCvH equations of state at T = 60 K and ρ = 10^{3} g/cm^{3} is Δu_{H} = 1590.12135 for hydrogen and Δu_{He} = 1843.06795 for helium, we added these values to all the specific internal energies in the REOS.3 H and He tables, respectively. Figure 2 shows a comparison between the internal energies of SCvH and REOS.3 + Δ_{u}.
The entropy is a necessary parameter in internal structure calculations. The two layers considered in the model follow an adiabat, therefore the ratio between the derivatives of the entropy with respect to pressure and temperature gives us the temperature gradient in the planet interior. We calculate the specific entropy, s, for each point of the REOS.3 table through thermodynamic relations between the published u,P,T, and ρ (Nettelmann et al. 2012). From the definition of the Helmholtz free energy, (3)it follows (4)Since(5)and (6)it follows from Eq. (3)that (7)and (8)Then Eq. (6)can be written as (9)using that (10)then (11)Now, in the ρ and T plane, (12)Finally, (13)and returning to Eq. (4), (14)The specific entropy at each point is calculated from Eq. (14), using the trapezoid rule for the numerical integration and cubic splines interpolation to add temperature and density points to improve the numerical calculation. Figure 3 shows a comparison of the entropy calculated at different temperatures with other equations of state.
These new equations of state with entropy and internal energies that coincide with SCvH at T = 60 K and ρ = 10^{3} g/cm^{3} are called REOS3b (see Appendix A).
3.2. Comparison with experiments
The original equations of state of MH13 and REOS.3 experienced some changes, such as the creation of a pure hydrogen table and the extension of this table for a wide pressure and temperature range (MH13+SCvH, Sect. 3.1.1), the change of the u_{0} , and the entropy calculation (REOS3b Sect. 3.1.2), and interpolation to add more points and make a pressuretemperature table (MH13+SCvH and REOS3b). To test our final tables, we make comparisons with highpressure experiments.
Much attention has been devoted to experiments designed to understand the properties of hydrogen (or deuterium) and helium at high densities (Nellis et al. 1983, 1984; Holmes et al. 1995; Collins et al. 1998; Belov et al. 2002; Boriskov et al. 2003; Grishechkin et al. 2004; Knudson et al. 2004; Eggert et al. 2008; Hicks et al. 2009; Celliers et al. 2010; Loubeyre et al. 2012). In these experiments a gas at rest with an initial thermodynamic state (u_{0},ρ_{0},P_{0}) is exposed to an abrupt change in pressure, temperature, and density. Applying the laws of conservation of mass, momentum, and energy at both sides of this shock wave, we derive a relation between the state of the gas before and after the shock, which is called the RankineHugoniot equation: (15)where ρ,P,andu are the density, pressure, and internal energy of the final shocked gas. Equation (15) defines all states on the (u, ρ, P) surface that can be reached from the initial condition by a single shock.
Fig. 4 Principal Hugoniot of hydrogen (left panel) and helium (right panel). The curves were calculated for an initial state of ρ_{0} = 0.0855 g/cm^{3} and T_{0} = 20 K for hydrogen and ρ_{0} = 0.123 g/cm^{3} and T_{0} = 4 K for helium. Experimental results are shown with different point styles for comparison. We included recent estimates by Brygoo et al. (2015), who presented corrections of previously published data on He (Eggert et al. 2008; Celliers et al. 2010), H_{2} , and D_{2} (Loubeyre et al. 2012) based on a better understanding of shocked compressed SiO_{2}. 

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3.2.1. Hugoniotcurve calculation from P, T, ρ, and s
The Hugoniot curve, H(ρ, P), is defined by (16)Since our EOS tables give us P, T, ρ, and s, we wish to write Eq. (16)as a function of these variables. If we differentiate Eq. (16), we obtain(17)Now we know that (18)where , and therefore (19)Using Eqs. (18)and (19)in Eq. (17), (20)To integrate in the P,T plane, we use Equation (20)is written as (23)Integrating Eq. (23)between an initial point and the final state, we obtain the Hugoniot curve as a function of the variables present in our EOS tables: (24)To find the zeros in Eq. (24), we calculate H(P,T) at each P and T in the EOS table, and when it changes sign, we perform a cubic spline interpolation in P and T to find the exact values of P, T, ρ(P,T) and s(P, T) that will give us H(P,T) = 0. Figure 4 shows Hugoniot curves for hydrogen and helium obtained when using different equations of state and compared with experimental data.
3.3. Heavy elements
Hydrogen and helium are the most relevant species, but an accurate description of the interior of Jupiter needs a definition of the heavy elements equation of state. In our model heavy elements are water and rocks, and we use three different equations of state to test their sensitivity. Following Saumon & Guillot (2004), we use for rocks the equation of state for a mixture of silicates called “dry sand” in SESAME (Lyon & Johnson 1992). For water we use the SESAME EOS (Lyon & Johnson 1992) and a more recent equation of state calculated in Valencia et al. (2013), which combines an equation of state for water at high temperatures (T> 1000 K) (French et al. 2009) with results taken from the NIST database (Saul & Wagner 1989).
4. Results
4.1. Different thermal structures
In this section we compare the interior of Jupiter with different equations of state. Figure 5 shows that REOS3b leads to higher temperatures for all densities than the other two equations of state. The differences are large even at relatively low densities, being close to 1000 K for ρ ≃ 0.2 g/cm^{3}. Since MH13+SCvH uses SCvH equation of state for densities ρ < 0.22246 g/cm^{3}, the differences between these two EOS arise for high densities, where MH13+SCvH reaches lower temperatures. These differences in the thermal profiles explain the different mass of metals in the envelope and mass of the core derived with the optimized models.
Fig. 5 Top panel: Jupiter density and temperature for different equations of state: SCvH (green solid), REOS3b (blue dashed), and MH13+SCvH (red dotted line). The discontinuity is due to the separation of the outer and deeper envelope at P_{sep} = 1 Mbar. Bottom panel: differences in the temperature obtained with the three different equations of state. The blue line is the temperature difference between REOS3b and SCvH, the red dotted line is the difference between SCvH and MH13+SCvH, and the orange dashed line is the difference between REOS3b and MH13+SCvH. 

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Gravitational moments we explored.
4.2. Optimized models
We calculated optimized models of Jupiter, in which the abundance of heavy elements and the mass of the core (M_{core}) are adjusted to reproduce the observables within their error bars (see Guillot et al. 1994, for more details on the method).
4.2.1. Gravitational moments of Jupiter
Our models match the radius and gravitational moments J_{2} and J_{4} of Jupiter. These last ones have changed with time according to our improved knowledge of the Jupiter gravity field. Table 1 shows the gravitational moments adopted in this paper. We consider gravitational moments derived from preJuno observations by Voyager 1 and 2, Pioneer 10 and 11 (Campbell & Synnott 1985), as well as more recent values derived from JUP230 and JUP310 orbit solutions^{1}, and also values with a correction by differential rotation effects, where the solution of Hubbard (1982) to the planetary figure problem was adopted for a deep rotation field with cylindrical symmetry (Guillot 1999).
Our calculation of the gravitational moments is based on the theory of figures of fourth order. A comparison with more detailed calculations made with a concentric Maclaurin spheroid (Hubbard2012, 2013; W. B. Hubbard, N. Movshovitz, priv. comm.) showed that our approximation leads to an error on the order of 1e7 in J_{4} and 2e6 in J_{6}. Figure 6 shows gravitational moments of order 4 and 6 as well as the resulting Js in all our optimized models with different equations of state. The black arrow shows the error in the determination of J_{6}. The observed Js change when considering differential rotation (indicated with the gray arrow in the figure). Further studies including interior dynamics will help improve our understanding of the Jupiter interior from gravity measurements (Kaspi et al. 2010; Galanti & Kaspi 2016).
The results of our simulations are very confined in the J_{4}J_{6} diagram, especially in the case of J_{6}, which is narrowly defined within this framework. We find larger  J_{4}  and J_{6} than observed values and the most recent estimates of 2013. Our results with MH13+SCvH and a recent estimate by Hubbard & Militzer (2016) show a similar tendency toward preferred J_{4} and J_{6} values.
Fig. 6 J_{4} and J_{6} preJuno observed values (Campbell & Synnott1985; purple), those with a correction due to differential rotation (Guillot 1999; dark green), and more recent estimates by Jacobson in 2003 (black) and 2013 (brown). Js solutions of our optimized models within 2σ of Campbell & Synnott (1985) and modeled with Zdiscontinuous are shown in different colors according to the equation of state used in the simulation: SCvH (green), REOS3b (blue), and MH13+SCvH (red). The pink dot shows a recent model by Hubbard & Militzer (2016) and the orange box shows estimates by Nettelmann et al. (2012) for comparison. 

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Fig. 7 Model results when adjusting the mass of the core and heavy elements to reproduce the radius and J_{2} of Jupiter. In these models the atmospheric helium mass mixingratio is fixed to Y_{atm} = 0.238, and we change the helium abundance in the deeper layer to match the protosolar value within its error bars. Different panels show J_{4} (upper panel), J_{6} (middle panel), and M_{Z} (lower panel). Different colors show results for the three different equations of state of hydrogen and helium: SCvH (green), MH13+SCvH (red), and REOS3b (blue). The lines indicate different locations of the helium phase that separates the two envelopes at 0.8 Mbar (dashed), 2 Mbar (solid), and 4 Mbar (dotted lines). The vertical dashed line indicates the protosolar helium mixing ratio, and the horizontal lines in the upper panel show estimates of J_{4} from observations and models as a reference. 

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In our models Y_{deep} is calculated to account for the missing helium in the atmosphere of Jupiter with respect to the protosolar value (Sect. 2). Figure 7 shows J_{4}, J_{6} , and M_{Z} found in our optimized models when changing Y_{proto} and maintaining Y_{atm} fixed, to test the effect of changing the abundance of helium in the deep layer of Jupiter. To satisfy the constraint in J_{2}, larger Y_{deep} leads to a lower mass of heavy elements in the envelope, which decreases approximately 5 M_{Earth} when going from Y_{deep} = 0.238 to Y_{deep} = 0.28 in all cases. A larger abundance of helium in the deep layer ensures solutions closer to current J_{4} and J_{6} estimates.
The mass of the core and the mass of heavy elements found in our models depend on the Js used to constrain the solutions. Figure 8 shows that solutions found with Js derived from observations published by Campbell & Synnott (1985) lead to larger M_{core} and smaller M_{Z} than the values found with more recent estimates by Jacobson (2003, 2013). M_{core} estimates derived using Js by Campbell & Synnott (1985) reach core masses 4M_{Earth} higher than the values found with Js by Jacobson (2003) for REOS3b and SCvH. The lowest M_{Z} find with Js by Campbell & Synnott (1985) are 6M_{Earth} lower than estimates found with values calculated by Jacobson (2003) for REOS3b and SCvH. Results found with MH13+SCvH do not change significantly for M_{Z}, but there is a difference of 2M_{Earth} in M_{core} in the solutions estimated with the different Js. There are no solutions found within 2σ with Js estimated by Jacobson (2003). New information provided by Juno will contribute to more accurate data to calculate gravitational moments of higher order and improve the uncertainty in lower orders, toward a better determination of the internal structure of Jupiter.
Fig. 8 Mass of the core and heavy elements in the interior of Jupiter derived with different Js. Models use Zdiscontinuous scenario, P_{sep} = 2 Mbar and different EOS indicated in the figure. Colored areas show solutions within 2σ from the radius, J_{2} and J_{4} of Jupiter estimated by Campbell & Synnott (1985; black), Guillot (1999; orange), Jacobson (2003; yellow), and Jacobson (2013; red). No solution was found with MH13+SCvH and constraints by JUP230. 

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4.2.2. Jupiter core and mass of heavy element
For the following optimized models we adjusted our solutions to reproduce the radius, J_{2} and J_{4} of Jupiter. For Zhomogeneous cases we adjusted the core mass and heavy element mass mixingratio, while for Zdiscontinuous we found the difference between the abundance of heavy elements in the outer and deeper envelope (ΔZ) and the core mass that best reproduce the observables. Our baseline models were made using J_{2} and J_{4} derived from observations of Jupiter gravity field (Campbell & Synnott 1985), P_{sep} = 2 Mbar and the NIST equation of state for hot H_{2}O as the equation of state for heavy elements. Models that differ from these conditions are indicated in the text and figure captions. We considered uncertainties in the averaged helium mass mixingratio, the atmospheric helium mass mixingratio, the mass mixingratio of rocks and ices, and the ice fraction in the core. Due to these uncertainties, our range of potential solutions covers an area in the M_{core}M_{Z} diagram. In addition, we explored different values of J_{2} and J_{4} (see Table 1), different equations of state for heavy elements, and we changed the location of the helium phase transition to explore the sensitivity of the results to different model input parameters.
We ran optimizations for the three different equations of state for hydrogen and helium explored in this work. It is important to note that we started each one of these runs with the same model, the same initial conditions, and the same space of parameters to vary, but changed only the equation of state for hydrogen and helium.
Fig. 9 Areas in the mass of the core and heavy elements space correspond to solutions found within 2σ and different equations of state for H and He: SCvH (green), MH13+SCvH (red) and REOS3b (blue area). Results found with Zhomogeneous are the areas within the dashed lines and correspond to a subgroup of the Zdiscontinuous solutions (we maintain this in all figures from now on). 

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Figure 9 shows that the internal structure of Jupiter is extremely sensitive to the adopted equation of state, as expected from the differences in thermal profiles shown in static models (Sect. 4.1). The different equations of state lead to a completely different set of solutions that do not intersect with each other. While SCvH leads to an interior of Jupiter with a small core and a large amount of heavy elements, results found with REOS3b indicate a much higher mass of heavy elements in general: a large core and a large abundance of heavy elements, and MH13+SCvH leads to a large core and a very small amount of heavy elements in the interior of Jupiter.
Fig. 10 Space of solutions obtained with different equations of state for H and He and for heavy elements. The equations of state for hydrogen and helium are indicated above the areas, and the equations of state of heavy elements have different colors: H_{2}O NIST is black, Drysand SESAME is purple, and H_{2}O NIST is pink. 

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Figure 10 shows that the structure of Jupiter is also sensitive to the equation of state for heavy elements adopted in the model (Sect. 3.3).
For REOS3b, both M_{core} and M_{Z} become lower when we use the dry sand SESAME, while the mass of heavy elements increases when we use H_{2}O SESAME, when compared with results found with H_{2}O NIST EOS. For SCvH M_{core} is lower for dry sand SESAME and M_{Z} is also lower for the same core masses in comparison to results found with H_{2}O NIST EOS. MH13+SCvH is less sensitive to changes in the EOS for heavy elements.
We tested the sensitivity of the results to different P_{sep}. Figure 11 shows that when P_{sep} moves from higher (4 Mbar) to lower pressures (0.8 Mbar), more solids are found in the core.
Fig. 11 Results of optimization models with different equations of state for H and He and changing the location of the P_{Sep}: 4 Mbar (black), 2 Mbar (blue), 1 Mbar (green), and 0.8 Mbar (light blue). 

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4.3. Discussion: sensitivity to internal energy calculations
The REOS.3 tables were constructed with a different scheme than SCvH tables. Their internal energies are not the same, not even in the H_{2} regime. We constructed REOS3b tables by changing the zero point of the specific internal energy to coincide with SCvH values at T = 60 K and ρ = 10^{3} g/cm^{3}, but the difference between the tables differs at different temperatures. Results by Militzer & Ceperley (2001), Militzer (2013), Militzer & Hubbard (2013) also show differences with SCvH internal energies. The authors found that the SCvH model considers lower temperature intervals for the ionization of hydrogen atoms, which causes the discrepancy with their internal energies results.
To test the sensitivity of the internal structure calculations to differences in the internal energy derivation, we calculated a second equation of state based on the REOS.3 results, in which we calculated the difference between REOS.3 and SCvH and shifted the internal energies at all densities accordingly so that they coincided at ρ = 10^{3} g/cm^{3} for all temperatures. We then calculated the entropy for each point of the table and performed static and optimized calculations. We called these new tables REOS3sc (shown in Appendix A). Figure 12 shows the internal structure of Jupiter calculated with REOS3b and REOSsc. The differences in internal energy lead to a difference in the entropies that affects the thermal profile.
Fig. 12 Thermal profile calculated for Jupiter when using two equations of state derived using different internal energies. Top panel shows temperature vs. density, where blue is REOS3b and dashed magenta line was obtained with our test case the REOS3sc eos. Lower panel shows the differences in temperatures derived with the different equations of state: blue line is the difference between REOS3b and SCvH, dashed magenta line is the difference between REOS3sc and SCvH and orange line is the difference between REOS3b and REOS3sc. 

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Fig. 13 Differences between the results obtained with REOS3b and REOS3sc equations of state. 

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The different temperatures in the interior of the planet lead to a different core mass and mass of heavy elements derived in the optimized calculations. Figure 13 shows the solutions found with both equations of state, which shows that results are very sensitive to the internal energy and entropy calculations.
5. Conclusions
The reservoir of heavy elements in Jupiter is key to understanding the origin of our solar system. Nevertheless, the distribution and amount of heavy elements in the planet interior is difficult to constrain and degeneracies arise depending on the assumed observational constraints and model parameters in interior structure calculations. We presented optimized models of Jupiter, where the mass of the core and the mass of heavy elements are adjusted to reproduce the Jupiter radius, J_{2} and J_{4}. We showed the drastic change in our solutions with the EOS for hydrogen and helium and also explored the sensitivity to heavy elements equations of state, to the separation between metallic and molecular envelope, and to the distribution of heavy elements in the interior of Jupiter.
We adopted two different models for Jupiter. The two scenarios considered helium phase separation and correspondingly different helium abundances in the outer and deeper layer. The difference is in the heavy elements distribution: one scenario has a homogeneous distribution of heavy elements, and its mass mixingratio is adjusted according to the observables. In the second scenario, Jupiter has different compositions of heavy elements in the two layers, and the difference in the abundance in the outer and deeper envelope (ΔZ) is adjusted to find solutions that best reproduce observational data of Jupiter. Allowing a change in heavy elements between the two layers adds a degree of freedom to the problem that grants more solutions in the M_{Z}M_{core} space. The pressure at which the separation between the two envelope layers occurs affects the solutions. This separation occurs between 0.8 and 4 Mbar, according to the helium rain studies of Morales et al. (2013). We found that M_{Z} decreases and M_{core} increases when P_{sep} moves from high to low pressures.
Based on the works by Saumon et al. (1995), Militzer & Hubbard 2013, Becker et al. (2014), we explore hydrogen and helium equations of state and showed that significant differences remain in these EOSs, although they match experimental data obtained by compression experiments along a Hugoniot. Some of the differences come from internal energy and entropy calculations. We showed that small changes in the internal energy lead to differences in the entropy that is calculated, which in turn affects the thermal profile and the estimation of the mass of the core and heavy elements. This explains differences seen in recently published interior models of the planet. The internal structure of Jupiter has a much higher temperature when REOS3b is used than what is derived with SCvH. For densities ρ> 0.22246 g/cm^{3}, MH13+SCvH leads to much lower temperatures than the other two EOS. These differences in the thermal structure lead to differences in the derived M_{core} and M_{Z}. MH13+SCvH allows higher M_{core} and lower M_{Z}, while REOS3b has higher M_{core} but similar M_{Z} as results found with SCvH.
In our baseline simulations, MH13+SCvH leads to M_{core} between 11 and 17 M_{Earth}, in agreement with results by Militzer & Hubbard 2013 and the preferred model of Hubbard & Militzer (2016). REOS3b leads to M_{core} between 7 and 16 M_{Earth}, higher than estimates by Nettelmann et al. (2012) and Becker et al. (2014). While their preferred model has P_{sep} ≥ 4 Mbar, our models place the separation between Z_{atm} and Z_{deep} in the same place as the helium phase transition, between 0.8 and 4 Mbar (Morales et al. 2013), and the baseline simulations have P_{sep} = 2 Mbar. When comparing the results at P_{sep} = 4 Mbar, we find a lower limit for the mass of the core of 4 M_{Earth}, consistent with the small core hypothesis shown by Nettelmann et al. (2012) and Becker et al. (2014) for the same case. Other small differences are due to different model parameters such as the temperature at the 1 bar limit, the equation of state used for solids, and differences in the entropy calculation.
The equation of state for the heavy elements is also relevant. We studied three different equations of state for rocks and water. Dry sand SESAME (Lyon & Johnson 1992) allows a lower M_{core}, while M_{Z} increases when we used H_{2}O SESAME (Lyon & Johnson 1992) when compared with solutions obtained with the hot water NIST EOS (Valencia et al. 2013).
Our results help in the interpretation of observational data of Jupiter. Its gravitational moments changed from the first preJuno data (Campbell & Synnott 1985) to the constraints we have today (Jacobson 2013). They also change according to the dynamics and rotation of Jupiter that are adopted in the model. Given the relatively large scatter in the gravitational moments of Jupiter inferred between 1985 and today, in our baseline simulations we chose to use conservative 2σ error bars based on the published value of Campbell & Synnott (1985), which encompasses all of these values. We also showed that different Js lead to different estimates of the core and heavy elements masses, with a difference of up to 4 M_{Earth} in M_{core} and ~6 M_{Earth} in M_{Z} for REOS3b and SCvH. Our preferred results have larger J_{6} than previously published. The Juno mission will provide more accurate data that will improve our knowledge of the internal structure of Jupiter.
Values calculated by R. A. Jacobson in 2003 and 2013, respectively, and published at the JPL website: http://ssd.jpl.nasa.gov/?gravity_fields_op
Acknowledgments
Y.M. greatly appreciates the CNES postdoctoral fellowship program. Y.M. and T.G. acknowledge the support of CNES for travel funding. Computations have been done on the “Mesocentre SIGAMM” machine, hosted by the Observatoire de la Côte d’Azur. We thank Bill Hubbard and Naor Movshovitz for valuable comments and for providing model comparisons to estimate the error in the Js calculation. We also thank Andreas Becker, Nadine Nettelmann, and Burkhard Militzer for fruitful discussions regarding equations of state.
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Appendix A: Equations of state
We present the equations of state derived in this paper. We note that the equations of state were tested and used only in a restricted range of pressures (10^{6} to 10^{14} dyn/cm^{2}) and temperatures (100 to 10^{5} K) relevant for modeling the internal structure of Jupiter. There are some deviations between the entropies we calculated and those in SCvH table for log (s) < 8.6 in the hydrogen tables and for log (s) < 8.2 and densities log (ρ) < −5 in the helium tables.
All the tables in this Appendix are available in their entirety at the CDS. A portion is shown here for guidance regarding their form and content.
MH13+SCvH table for hydrogen.
REOS3b table for hydrogen.
REOS3b table for helium.
REOS3sc table for hydrogen.
REOS3sc table for helium.
All Tables
All Figures
Fig. 1 Phase diagram of hydrogen (adapted from Guillot & Gautier 2015). The range of validity of each equation of state in the range of the figure is shown in different colors: SCvH is shown in purple, MH13 in blue, and REOS.3 in orange. The internal structure of Jupiter is shown as a green thick line. 

Open with DEXTER  
In the text 
Fig. 2 Specific internal energy as a function of density at different temperatures for hydrogen (left panel) and helium (right panel), using two different equations of state. SCvH is shown as green solid lines, and the values shown as blue dotted lines correspond to the u in REOS.3 plus Δu (Δu_{H} = 1590.12135 for hydrogen and Δu_{He} = 1843.06795 for helium) or REOS3b. 

Open with DEXTER  
In the text 
Fig. 3 Specific entropy vs. density at different temperatures for hydrogen (left panel) and helium (right panel). For hydrogen we show a comparison between the entropy calculated with REOS3b (blue), the one published in SCvH (green), and MH13+SCvH values (red). Since MH13+SCvH is a pure hydrogen table, the right panel shows a comparison between REOS3b and SCvH only. 

Open with DEXTER  
In the text 
Fig. 4 Principal Hugoniot of hydrogen (left panel) and helium (right panel). The curves were calculated for an initial state of ρ_{0} = 0.0855 g/cm^{3} and T_{0} = 20 K for hydrogen and ρ_{0} = 0.123 g/cm^{3} and T_{0} = 4 K for helium. Experimental results are shown with different point styles for comparison. We included recent estimates by Brygoo et al. (2015), who presented corrections of previously published data on He (Eggert et al. 2008; Celliers et al. 2010), H_{2} , and D_{2} (Loubeyre et al. 2012) based on a better understanding of shocked compressed SiO_{2}. 

Open with DEXTER  
In the text 
Fig. 5 Top panel: Jupiter density and temperature for different equations of state: SCvH (green solid), REOS3b (blue dashed), and MH13+SCvH (red dotted line). The discontinuity is due to the separation of the outer and deeper envelope at P_{sep} = 1 Mbar. Bottom panel: differences in the temperature obtained with the three different equations of state. The blue line is the temperature difference between REOS3b and SCvH, the red dotted line is the difference between SCvH and MH13+SCvH, and the orange dashed line is the difference between REOS3b and MH13+SCvH. 

Open with DEXTER  
In the text 
Fig. 6 J_{4} and J_{6} preJuno observed values (Campbell & Synnott1985; purple), those with a correction due to differential rotation (Guillot 1999; dark green), and more recent estimates by Jacobson in 2003 (black) and 2013 (brown). Js solutions of our optimized models within 2σ of Campbell & Synnott (1985) and modeled with Zdiscontinuous are shown in different colors according to the equation of state used in the simulation: SCvH (green), REOS3b (blue), and MH13+SCvH (red). The pink dot shows a recent model by Hubbard & Militzer (2016) and the orange box shows estimates by Nettelmann et al. (2012) for comparison. 

Open with DEXTER  
In the text 
Fig. 7 Model results when adjusting the mass of the core and heavy elements to reproduce the radius and J_{2} of Jupiter. In these models the atmospheric helium mass mixingratio is fixed to Y_{atm} = 0.238, and we change the helium abundance in the deeper layer to match the protosolar value within its error bars. Different panels show J_{4} (upper panel), J_{6} (middle panel), and M_{Z} (lower panel). Different colors show results for the three different equations of state of hydrogen and helium: SCvH (green), MH13+SCvH (red), and REOS3b (blue). The lines indicate different locations of the helium phase that separates the two envelopes at 0.8 Mbar (dashed), 2 Mbar (solid), and 4 Mbar (dotted lines). The vertical dashed line indicates the protosolar helium mixing ratio, and the horizontal lines in the upper panel show estimates of J_{4} from observations and models as a reference. 

Open with DEXTER  
In the text 
Fig. 8 Mass of the core and heavy elements in the interior of Jupiter derived with different Js. Models use Zdiscontinuous scenario, P_{sep} = 2 Mbar and different EOS indicated in the figure. Colored areas show solutions within 2σ from the radius, J_{2} and J_{4} of Jupiter estimated by Campbell & Synnott (1985; black), Guillot (1999; orange), Jacobson (2003; yellow), and Jacobson (2013; red). No solution was found with MH13+SCvH and constraints by JUP230. 

Open with DEXTER  
In the text 
Fig. 9 Areas in the mass of the core and heavy elements space correspond to solutions found within 2σ and different equations of state for H and He: SCvH (green), MH13+SCvH (red) and REOS3b (blue area). Results found with Zhomogeneous are the areas within the dashed lines and correspond to a subgroup of the Zdiscontinuous solutions (we maintain this in all figures from now on). 

Open with DEXTER  
In the text 
Fig. 10 Space of solutions obtained with different equations of state for H and He and for heavy elements. The equations of state for hydrogen and helium are indicated above the areas, and the equations of state of heavy elements have different colors: H_{2}O NIST is black, Drysand SESAME is purple, and H_{2}O NIST is pink. 

Open with DEXTER  
In the text 
Fig. 11 Results of optimization models with different equations of state for H and He and changing the location of the P_{Sep}: 4 Mbar (black), 2 Mbar (blue), 1 Mbar (green), and 0.8 Mbar (light blue). 

Open with DEXTER  
In the text 
Fig. 12 Thermal profile calculated for Jupiter when using two equations of state derived using different internal energies. Top panel shows temperature vs. density, where blue is REOS3b and dashed magenta line was obtained with our test case the REOS3sc eos. Lower panel shows the differences in temperatures derived with the different equations of state: blue line is the difference between REOS3b and SCvH, dashed magenta line is the difference between REOS3sc and SCvH and orange line is the difference between REOS3b and REOS3sc. 

Open with DEXTER  
In the text 
Fig. 13 Differences between the results obtained with REOS3b and REOS3sc equations of state. 

Open with DEXTER  
In the text 
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