Issue 
A&A
Volume 540, April 2012



Article Number  A99  
Number of page(s)  11  
Section  Planets and planetary systems  
DOI  https://doi.org/10.1051/00046361/201117317  
Published online  04 April 2012 
Factors affecting the radii of closein transiting exoplanets
School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, KY16 9SS, UK
email: becky.enoch@standrews.ac.uk
Received: 22 May 2011
Accepted: 27 February 2012
Context. The radius of an exoplanet may be affected by various factors, including irradiation received from the host star, the mass of the planet and its heavy element content. A significant number of transiting exoplanets have now been discovered for which the mass, radius, semimajor axis, host star metallicity and stellar effective temperature are known.
Aims. We use multivariate regression models to determine the powerlaw dependence of planetary radius on planetary equilibrium temperature T_{eq}, planetary mass M_{p}, stellar metallicity [Fe/H], orbital semimajor axis a, and tidal heating rate H_{tidal}, for 119 transiting planets in three distinct mass regimes.
Methods. We fit models initially to all 119 planets, resulting in fairly high scatter between fitted and observed radii, and subsequently to three subsets of these planets: Saturnmass planets, Jupitermass planets, and highmass planets.
Results. We find models for each subset that fit the observed planetary radii well and show the importance of the various environmental parameters on each subset.
Conclusions. We determine that heating leads to larger planet radii, as expected, increasing mass leads to increased or decreased radii of lowmass (<0.5 R_{J}) and highmass (>2.0 R_{J}) planets, respectively (with no mass effect on Jupitermass planets), and increased hoststar metallicity leads to smaller planetary radii, indicating a relationship between hoststar metallicity and planet heavy element content. For Saturnmass planets, a good fit to the radii may be obtained from log(R_{p}/R_{J}) = –0.077 + 0.450 log(M_{p}/M_{J}) – 0.314 [Fe/H] + 0.671 log(a/AU) + 0.398 log(T_{eq}/K). The radii of Jupitermass planets may be fit by log(R_{p}/R_{J}) = − 2.217 + 0.856 log(T_{eq}/K) + 0.291 log(a/AU). Highmass planets’ radii are best fit by log(R_{p}/R_{J}) = –1.067 + 0.380 log(T_{eq}/K) – 0.093 log(M_{p}/M_{J}) – 0.057 [Fe/H] + 0.019 log(H_{tidal}/1 × 10^{20}). These equations produce a very good fit to the observed radii, with a mean absolute difference between fitted and observed radius of 0.11 R_{J}, compared to the mean reported uncertainty in observed radius of 0.07 R_{J}. A clear distinction is seen between the coredominated Saturnmass (0.1–0.5 M_{J}) planets, whose radii are determined almost exclusively by their mass and heavy element content, and the gaseous envelopedominated Jupitermass (0.5–2.0 M_{J}) planets, whose radii increase strongly with irradiating flux, partially offset by a powerlaw dependence on orbital separation.
Key words: methods: statistical / planetary systems / planets and satellites: general / planets and satellites: physical evolution
© ESO, 2012
1. Introduction
The massradius relationship of gravitationally bound objects may be approximated by a polytropic relationship given by R ∝ M^{(1 − n)/(3 − n)} (Burrows & Liebert 1993). The polytropic index n ranges from 0 for low mass planets made of incompressible matter, i.e. R ∝ M^{1/3}, to 3/2 for lowmass stars with electron degeneracy, i.e. R ∝ M^{ − 1/3} (Chabrier et al. 2009). Between these two regimes, at approximately Jupitermass objects (Zapolsky & Salpeter 1969), n ~ 1, i.e. R ∝ M^{0}, showing that the radii of Jupitermass planets do not depend on their masses. The variation in radii of most known exoplanets must therefore arise from other influencing factors. For example, Guillot (2005) derive a massradius relationship for highly irradiated planets, incorporating heating effects.
Various potential effects on planetary radii have been discussed in the literature. The equilibrium temperature of the planet, related to the irradiating flux received from the host star, is likely to affect the radius (Guillot et al. 1996; Guillot & Showman 2002) in that planets that are strongly heated by their host stars may have inflated radii.
Additional heating effects have also been proposed, including Ohmic heating (Batygin & Stevenson 2010; Batygin et al. 2011; Laughlin et al. 2011), a mechanism of planetary heating from the coupling of the planetary magnetic field and atmospheric flows; kinetic heating (Guillot & Showman 2002) where a small amount of flux from the host star is transformed into kinetic energy and then thermal energy in the atmosphere of the planet; and tidal heating (Bodenheimer et al. 2001, 2003; Jackson et al. 2008) due to circularisation of closein exoplanet orbits.
Saturnmass transiting planets used in the analysis of radii.
Jupitermass transiting planets used in the analysis of radii.
Highmass transiting planets used in the analysis of radii.
The metallicity of the system is also thought to affect planetary radii. Increasing the metallicity could lead to an increased heavy element abundance in the atmosphere, producing higher atmospheric opacity which could again retard the loss of heat from a planet and thus slow its contractions (Burrows et al. 2007). However, an enriched atmosphere would also have a higher mean molecular weight, offsetting partially or totally any reduction in contraction (Burrows et al. 2007; Guillot 2008). Alternatively, the higher metallicity may result in increased heavy elements in the core, leading to a decreased planetary radius relative to a planet of the same mass but lower metallicity (Guillot et al. 2006; Burrows et al. 2007). Fortney & Nettelmann (2010) set this out in their “basic questions” about planetary structure and composition, including whether heavy elements in a planet mix into the HHe envelope, or are found in the core, and whether a planet’s heavy element mass fraction depends on that of its parent star.
Recently, Laughlin et al. (2011) found a correlation between the radius anomalies from comparing observed radii with model radii based on calculations of coreless giant planets tabulated for various mass and insolation values (Bodenheimer et al. 2003). They found an additional radius dependence on planetary temperature of R ∝ T^{1.4}, and suggested Ohmic heating may be largely responsible. They also noted that even including this additional dependence, there remained significant scatter in the observed radii and suggested evidence of a signficant correlation with host star metallicities, and that tidal heating may also contribute.
The system age may also have an effect since the radius of an isolated planet should decrease with time due to KelvinHelmholtz contraction.
Additionally, Valencia et al. (2010) and Jackson et al. (2010) recently investigated CoRoT7b, concluding that it is likely to have initially had a much larger mass than currently, possibly including a substantial gaseous component which would have given it a larger radius than the 0.15 R_{J} observed today. Closein planets are susceptible to evaporation due to intense radiation from the star. A large loss of mass (and radius) can occur due to enhanced atmospheric escape for exoplanets that are very close to their stars. Molecules are able to escape even if below the normal escape velocity, needing only to reach the Roche Lobe. The atmosphere of HHe planets is only loosely bound to the planetary core, so evaporation can be quicker than the contraction of a planet, which may result in loss of the whole envelope for a planet of up to 1 M_{J} initially (Valencia et al. 2010). A planet which lost a significant fraction of mass may become stable when the EUV flux from the young host star drops (Valencia et al. 2010). Models by Hubbard et al. (2007) show significant initial mass loss in the first 0.1 Gyr of a system. Baraffe et al. (2005) show that recent Neptunian objects could have originally been more massive irradiated gas giants.
The reduction in required escape energy may be given by (Jackson et al. 2010; Erkaev et al. 2007) (1)where (2)The mass loss rate due to stellar irradiation is then given by (3)where F_{xuv} is the extreme UV flux from the star and ϵ is the fraction of incoming energy that is removed by escaping gas. Thus planets of smaller semimajor axis may be trimmed down by atmospheric blowoff. Atmospheric escape of HD 209458, with K_{tide} = 0.65, has been observed in the Ly α line (VidalMadjar et al. 2003). More recently, Fossati et al. (2010) report finding enhanced transit depths when observing the very closein exoplanet WASP12b with the HST/COS instrument using UV transmission spectroscopy. All the planets considered here have K_{tide} values below 1, while some have very low values and thus significant enhancement of mass loss, for example WASP19b and WASP12b with K_{tide} values of 0.29 and 0.27 respectively.
We previously investigated the effect of metallicity and equilibrium temperature on the radii of planets in a mass range of 0.1 − 0.6 M_{J}, finding a strong correlation of stellar radius with irradiating flux, and a weaker anticorrelation with hoststar metallicity (Enoch et al. 2011). In this paper, we seek to illuminate the main trends seen in the radii of the majority of known transiting exoplanets with a wide range of masses and radii using several parameters. Section 2 sets out the method of analysis and gives the resulting calibrations for the planetary radii, while Sect. 3 provides a discussion of the results.
2. Analysis
There are currently (November 2011) almost 200 known transiting exoplanets^{1}, for which values have been published for both mass and radius. To perform our analysis we selected all known transiting planets in the mass range 0.1–12.0 M_{J} with orbital periods below 10 days for which values have been published for host star metallicity and effective temperature. This resulted in a sample of 119 planets, given in Tables 1 to 3.
We used updated parameters for WASP17b, as given in Anderson et al. (2011), with a planetary radius of 2.0 R_{J} and eccentricity 0.03 found from secondary eclipse timing, for WASP7b, as given in Southworth et al. (2011), with a planetary radius of 1.33 R_{J}, and for CoRoT13b, with a radius of 1.25 R_{J} (Southworth 2011).
We fixed the eccentricities of many of these planets to zero: WASP6b, WASP12b, WASP22b, WASP28b and WASP32b were reported to have eccentricities of 0.05 (Gillon et al. 2009), 0.02 (Hebb et al. 2009), 0.02 (Maxted et al. 2010), 0.05 (West 2011) and 0.02 (Maxted et al. 2011) respectively. However, LucySweeney tests (Lucy & Sweeney 1971) on the original data give values of 0.22, 0.17, 0.26, 1.0 and 0.68 respectively for the probability that the measured eccentricities could have arisen by chance from underlying circular orbits, given the uncertainties and uneven sampling of the radialvelocity observations, showing that in all these cases a circular orbit is likely.
Secondary eclipse timings often show eccentricities to be considerably lower than the upper limits allowed by radialvelocity measurements alone. For WASP12b, Husnoo et al. (2011) and Campo et al. (2010) find a likely circular orbit, based on secondary eclipse timings. Similarly, WASP19b was attributed an eccentricity of 0.02 in Hebb et al. (2010) but Gibson et al. (2010) find a circular orbit from the timing of the measured secondary eclipse, though conversely, a small eccentricity (0.009) in the orbit of WASP18b was confirmed to 7σ by Nymeyer et al. (2011) from their secondary eclipse measurements. WASP10b was originally reported to have an eccentricity of 0.06 (Christian et al. 2009), but Maciejewski et al. (2011) find that a circular orbit is likely, with the difference in radial velocities due to starspot activity.
Additionally, Pont et al. (2011) point out that a finite bestfit eccentricity will always be found where the eccentricity is allowed to float as a free parameter in fitting the data. Spurious eccentricities with apparent significance as great as 3σ often arise from a combination of measurement error and uneven sampling around the orbit. From a homogeneous reanalysis of available data, Pont et al. (2011) find that the eccentricities of CoRoT5b and HAT13b should be set to zero. For other planets in our sample announced with small eccentricity values, we also fix them to zero if the values are within 3σ of 0, which was the case for HAT18b, 19b, 20b, 22b, 23b, 25b, 28b, 29b, 32b and 33b, CoRoT12b, 18b and 19b, Kepler12b, 14b and 17b, WASP23b and 50b and HD 209458b, for which the data has previously been noted to be consistent with a circular orbit (Laughlin et al. 2005; Snellen et al. 2008).
This resulted in 17 out of 119 planets having an eccentricity greater than zero, as shown in Tables 1 to 3, with significantly more highmass planets (greater than 2.0 M_{J}) showing a nonzero eccentricity: 11 of 32 highmass planets, compared to 1 of 16 Saturnmass (0.1–0.5 M_{J}) and 4 of 71 Jupitermass (0.5–2.0 M_{J}) planets. This difference does not seem to be explained by the known periodeccentricity relationship (Halbwachs et al. 2005, for example), that exoplanets on short periods have circular orbits due to tidal circularisation while exoplanets on wider orbits have a range of eccentricity values, since both lowmass and highmass eccentric and noneccentric planets cover a range of orbital periods. The difference may therefore lend support to the trend discussed by Ribas & MiraldaEscudé (2007) for radial velocitydiscovered planets that highmass planets have an eccentricity distribution closer to binary stars than lowmass planets. It should be noted though that it is easier to detect genuine eccentricity in highmass planets than in lowmass ones because the velocity measurement errors are small relative to the total RV amplitude.
To determine the factors that have a significant effect on planetary radii, we performed multivariate regression analyses (singular value decomposition (SVD) fits), weighted by the uncertainties on the measurements for planetary radii, for a variety of explanatory parameters, including the planetary equilibrium temperature, T_{eq}, in Kelvin, semimajor axis, a, in AU, planetary mass, M, in Jupiter masses, stellar metallicity, [Fe/H] and tidal heating rate on the planet, H_{tidal}, divided by 1 × 10^{20} W. The equilibrium temperature of the planet is given by (4) where T_{∗,eff} is the host star’s effective temperature, R_{∗} is the stellar radius, a is the semimajor axis, A is the planetary Bond albedo and F is the fraction of the planet surface that is reradiating flux. Albedo values have not so far been determined for the majority of exoplanets, but Rowe et al. (2008) determined a very low albedo for HD 209458b, finding just 0.04 ± 0.05 for the geometric albedo and inferring a Bond albedo of less than 0.12 from this. We set A = 0 (F = 1) here to calculate the equilibrium temperatures. For a given A and F then, T_{eq} is directly proportional to the irradiating flux from the star.
The tidal heating rate is given by (5)where Q is the tidal dissipation factor (taken to be 10^{5}) and k is the Love number (=0.51) (Jackson et al. 2008),
To determine the bestfitting SVD model, we used the Bayesian Information Criterion, BIC, value where (6)where N_{P} is the number of parameters used in the fit and N_{D} is the number of datapoints (Szydlowski & Kurek 2008). Initially, we used a oneparameter model, and used the BIC values to determine the parameter with the strongest influence on planetary radii. Next, we tried a twoparameter model, using the best parameter from the oneparameter fits, and adding each of the other parameters in turn. If a twoparameter model was found to have a lower BIC value than the best oneparameter model, we selected this and attempted a threeparameter model using the best twoparameter model plus a further parameter, and so on until the best model was found.
2.1. All planets
To find the bestfitting model for planetary radius for all 119 planets over the full mass range of 0.1 to 12.0 M_{J}, we initially subtracted the expected coldbody massradius relationship determined by Seager et al. (2007) using interior models. Figure 1 shows log(M/M_{J}) against log(R/R_{J}) for the 119 planets used in this analysis, with the Seager et al. (2007) massradius relationship for pure hydrogen with a solid line. Most of the planets follow the pure H relationship, or lie above it, while a few (notably CoRoT8b), perhaps strongly coredominated, lie below it. We subtracted the logarithmic massradius relationship expected for pure H from the planets, leaving the log(M/M_{J})–log(R/R_{J}) scatter shown in 2.
Fig. 1
MassRadius plot of 119 transiting exoplanets showing the expected massradius relationship for pure H (solid line) Seager et al. (2007). 
Fig. 2
Mass against radius residuals after subtracting the Seager et al. (2007) massradius relationship. 
BIC values for SVD fits on all 119 transiting exoplanets.
We then performed an SVD analysis on the radius residuals, and found a bestfit model where (7)A table of BIC values summarising the model building process is given in Table 4.
The use of the logarithm of planetary equilibrium temperature may incorporate several possible heating effects showing a powerlaw relationship of planetary temperature with radius.
A relationship between planetary radius was not only found with planetary equilibrium temperature, as expected, but also with the semimajor axis. The relationship with temperature contains a separate and opposing dependence on semimajor axis than that seen in the direct relationship with semimajor axis where the planetary radius tends to be smaller for closerin planets. This tendency can actually be seen directly by comparing pairs of planets for which parameters other than the semimajor axis are very similar. For example WASP19b and WASP4b have very similar mass (1.15 and 1.12 M_{J}, respectively), metallicity (~0) and equilibrium temperatures (1995 and 1875 K, respectively) but WASP19b has a radius of 1.31 R_{J} at 0.016 AU while WASP4b has 1.42 R_{J} at 0.023 AU. Direct comparisons between planets are generally difficult due to the different values of the various parameters affecting the radii, and thus analyses such as set out here can help to disentangle each effect. The direct relationship of semimajor axis on radius is seen more clearly when analysing subsamples of planets, below, and is discussed further in those sections.
A plot of observed planetary radii against fitted radii using the above equation is given in Fig. 3, showing significant scatter (mean error in fitted radius of 0.16 R_{J}), with 35 of 119 fitted radii values more than 0.2 R_{J} from the observed values (7 with more than 0.4 R_{J} error). This calibration was not therefore felt to provide a very good fit to the data. We then partitioned the 119 planets into 16 Saturnmass planets, 0.1 − 0.5 M_{J}, dealt with in Sect. 2.2, 71 Jupitermass planets, 0.5 − 2.0 M_{J}, discussed in Sect. 2.3, and 32 highmass planets, 2.0 − 12.0 M_{J}, in Sect. 2.4. For each subset of planets, we performed SVD fits as above, without subtracting the (Seager et al. 2007) massradius relationships first. We discuss the significant effects on radii for each mass range below, and provide a bestfitting equation.
Fig. 3
Results of the radius calibration on all 119 transiting exoplanets using the Seager et al. (2007) massradius relationship and a single fourparameter SVD fit. 
2.2. Saturnmass planets
Sixteen known transiting exoplanets fall into the mass range 0.1–0.5 M_{J} (including WASP6b). The upper mass cutoff of 0.5M_{J} was chosen to represent the point where the massradius relationship changes slope from a steep correlation in the low mass planets to an almost flat relationship in the Jupitermass group, thereby splitting the planets into distinct groups with different relationships between radius and mass.
The bestfitting model for this mass range was found using the procedure described for the global SVD fit above, with the model BIC values provided in Table 5, and was found to be a fourparameter model, mainly determined by planet mass and host star metallicity: (8)The equilibrium temperature of the planet only minimally affects the planet radius here (though it has a strong effect on more massive planets, below). We did not include tidal heating in the fit, since only 1 of the 16 planets have eccentricities demonstrably greater than zero (WASP17b).
Eight planets have radii with residuals greater than ± 0.2 R_{J} relative to the fitted model: HAT18b (0.20), HAT19b (0.31) and Kepler12b (0.26) all have their radii underestimated, such that their observed radii are greater than expected from the model fit. The radii of CoRoT5b, CoRoT8b, WASP6b, WASP13b and WASP21b are overestimated by 0.32, 0.21, 0.20, 0.26 and 0.47 R_{J} respectively.
BIC values for SVD fits on 16 lowmass transiting exoplanets.
Planetary mass.
As mentioned in Sect. 1, the radii of gaseous planets do not generally depend on their masses but there is an effect on radii for lowermass planets, made up of essentially incompressible matter. For the Saturnmass subset of planets, the mass has the strongest effect on planet radius. A correlation between mass and adjusted radius, after removing the effects of the other parameters, produces a coefficient of 0.51, shown in Fig. 4, with a leastabsolutedeviation model overplotted. The positive coefficients in the correlation and the SVD model fit shows that for lowmass planets, radius increases as mass increases, as expected.
The fit coefficient for mass, at 0.45, is in fact higher than expected from the polytropic relationship with n ~ 1 for incompressible matter, such that R ∝ M^{1/3}, or log R ∝ 0.33 log M. The additional dependence of radius on mass indicates that the density of the planet itself is dependent on mass, suggesting that the coreenvelope ratio increases towards lower mass, as recently shown in Miller & Fortney (2011).
Fig. 4
The correlation between observed radius and mass for Saturnmass planets, after removing the effects of the other parameters used in the SVD fit. 
Metallicity.
A correlation between the adjusted radius, after removing effects due to other parameters, and the host star metallicity results in a coefficient of –0.56, shown in Fig. 5. The strong negative coefficient, as well as the negative coefficient value in the SVD fit, indicates that as the metallicity of the host star increases, planetary radius decreases. This lends support to the theory that higher system metallicity produces larger planetary cores, and thus smaller radii (Guillot et al. 2006). Given that a strong correlation is found at all between host star metallicity and planetary radius, this implies that a planet’s heavy element mass fraction is related to that of its host star.
Fig. 5
The correlation between observed radius and metallicity for Saturnmass planets, after removing the effects of the other parameters used in the SVD fit. 
Planetstar separation.
A small effect on BIC value was also produced by the starplanet separation, however a correlation between the semimajor axis and the observed radius, after removing the effects on radius of the other terms by subtracting these parameters multiplied by their coefficients above, produces a low coefficient value of 0.34, shown in Fig. 6, clearly not a strong effect in this mass range.
Fig. 6
The correlation between observed radius and planetstar distance for Saturnmass planets, after removing the effects of the other parameters used in the SVD fit. 
Stellar irradiation.
The equilibrium temperature of the planet also has an effect on the radii. Performing a simple correlation between the logarithms of observed radius and equilibrium temperature, after adjusting for the other terms in the radius fit, gives a weak coefficient of 0.28, shown in Fig. 7. The positive coefficient shows that planets of a higher equilibrium temperature generally have larger radii, but for coredominated Saturnmass planets, this appears to be only a minor effect. The apparent contrast in results found here in comparison to Enoch et al. (2011) is due to lowering the upper mass cutoff from 0.6 M_{J} to 0.5 M_{J} here. In Enoch et al. (2011), over half the planets in the small sample analysed were in the mass range 0.5–0.6 M_{J}, which is here part of the larger Jupitermass planet group where a large effect of equilibrium temperature on radius is seen (see below).
Fig. 7
The correlation between observed radius and equilibrium temperature for Saturnmass planets, after removing the effects of the other parameters used in the SVD fit. 
Age.
All 16 planets have published values for isochrone age. To see if the age of a system affects the radius of closein planets, for example due to KelvinHelmholtz contraction, we tried adding a parameter for age to the model, but it produced no improvement in the model, with BIC = 474 compared to 470 without the age parameter. The expected KelvinHelmholtz contraction is likely to be mostly offset by the continued heating from strong stellar irradiation on the closein planets.
2.3. Jupitermass planets
This is the largest subset of transiting planets, with 71 having a mass between 0.5 and 2.0 M_{J}. A fit to all 71 planets resulted in a twoparameter fit given by (9)Again, we did not attempt to fit tidal heating, since only 4 of the 71 planets have nonzero eccentricity. This model produced a mean error of 0.106 R_{J} in fitted radii, with five planets having errors in fitted radii of greater than 0.2R_{J} (up to 0.27R_{J}), plus one significant outlier, HAT32b, underestimated by 0.63 R_{J}. HAT32b is an extremely bloated planet with a measured radius of over 2 R_{J}, which may be in a slightly eccentric orbit (Hartman et al. 2011). Tidal heating on the planet could potentially explain the extra inflation above that fitted here.
The addition of a coefficient for mass produced a small improvement of 20.1 in BIC value, but increased the mean error in fitted radii to 0.113, so was felt to be insignificant, particularly since a correlation of mass with radius adjusted for the fitted effects of temperature and semimajor axis yielded a very small coefficient of 0.13. Model BIC values are given in Table 6.
Planetary temperature is the strongest parameter in the fit: the high planetary equilibrium temperatures sustained due to the strong stellar irradiation on closein exoplanets produces a shallow temperature gradient in the planet, impeding the interior cooling and thus contraction. These planets must have migrated early and not contracted as a planet orbiting further from the star would have (Guillot & Showman 2002) since if they had formed and cooled at a larger semimajor axis before inward migration, their radii would only be marginally increased due to a puffedup atmosphere (Iro et al. 2005; Burrows et al. 2000) and such a strong effect on radius due to irradiation would not be seen.
Correlations of radius with equilibrium temperature and semimajor axis, after removing effects on the radius due to the other terms, give coefficients of 0.84 and 0.62, respectively, shown in Figs. 8 and 9. The positive correlation and fit coefficient for the semimajor axis indicate that the closer the planet is to the star, the smaller the radius. This could be due to the ease of atmospheric escape described in Sect. 1, where the atmospheric escape of closer planets is enhanced by the K_{tide} factor given in Eq. (1). As mentioned above, WASP19b has a K_{tide} value of 0.29 at 0.016 AU, and its measured radius is 0.11 R_{J} lower than that of WASP4b, of similar mass, equilibrium temperature and host star metallicity, orbiting slightly farther from its host star.
Fig. 8
The correlation between observed radius and equilibrium temperature for Jupitermass planets, after removing the effects of semimajor axis. 
BIC values for SVD fits on 71 Jupitermass transiting exoplanets.
Fig. 9
The correlation between observed radius and semimajor axis for Jupitermass planets, after removing the effects of equilibrium temperature. 
In this mass range, planet mass has no apparent effect on planet radius. This is as expected from the relationship R ∝ M^{(1 − n)/(3 − n)}, as discussed in Sect. 1, where the polytropic index is n ~ 1 for Jupitermass planets. A lack of massradius effect in this mass range also indicates that, in contrast to the Saturnmass planets discussed above, the cores of these planets are either unimportant, or are not correlated with planet mass.
Adding a coefficient for age to the model increases the BIC value from 218 to 220, for the 57 planets with published isochrone ages. To investigate whether the relationship between semimajor axis and radius has any correlation with the isochrone age of the system, we altered the model parameter from log(a) to log(a)/log(age). This increased the model BIC value to 306. If there is no dependence here on age, a reduction in radius of closein exoplanets due to blowoff could occur early in the system history. The T Tauri phase (Joy 1945; Herbig 1952) in the evolution of lowmass stars (<2 M_{⊙}) produces strong XUV radiation and intense stellar winds that cause the disappearance of the gas component of the disc (Hayashi 1981) via outflow. The K_{tide} enhanced atmospheric escape due to the XUV radiation combined with the strong stellar wind could strip these close exoplanets of their outer layers of atmosphere, reducing their radii. MurrayClay et al. (2009) calculated that a hot Jupiter at 0.05 AU from its host star could lose around 6 × 10^{12} g s^{1} due to the intense XUV from a TTauri star, equating to around 1% of a Jupiter mass during the ~100 Myr T Tauri phase; more for a planet orbiting closer than 0.05 AU. Thus the relationships of radius with semimajor axis and equilibrium temperature could both be due to proximity of the planet to the host star, but from entirely different processes, namely atmospheric blowoff and retarded contraction, respectively. However, a small reduction in the overall mass of a Jupitermass planet is not likely to produce a noticeable effect on radius in this mass regime, so the radiussemimajor axis relationship may be due to another factor, perhaps a migration halting mechanism resulting in planets with larger cores/higher heavy element content orbiting closer to their host stars than otherwise similar planets with lower heavy element content.
2.4. Highmass planets
Thirtytwo transiting exoplanets used in this analysis have a mass in the range 2.0–12.0 M_{J}. Equilibrium temperature, planet mass, metallicity and tidal heating were found to be important in determining their radii. The SVD fit resulted in (10)with model BIC values provided in Table 7. The mean error in fitted radius is 0.10 R_{J}, with four planets having an error in fitted radius greater than 0.2 R_{J} (WASP18b, CoRoT2b, CoRoT17b and CoRoT23b), though none was greater than 0.3 R_{J}. Adding a coefficient for semimajor axis did not improve the BIC.
BIC values for SVD fits on 32 highmass transiting exoplanets.
Summary of radius calibration coefficients.
The correlation of equilibrium temperature and highmass planet radii gives a coefficient of 0.72, shown in Fig. 10.
Fig. 10
The correlation between observed radius and equilibrium temperature for highmass planets. 
As expected, the mass term again becomes important for more massive planets, greater than a few Jupiter masses, where electron degeneracy in the dense cores produces a contraction of the planet and thus a smaller radius. The correlation of planet mass with radius adjusted for equilibrium temperature and semimajor axis effects is –0.47, as seen in Fig. 11. Planet mass here thus has the opposite effect on radius as it does on lowmass planets, where the correlation and SVD fit coefficient were positive.
Fig. 11
The correlation between observed radius and mass for highmass planets, after removing the effects of other terms. 
The addition of a term for tidal heating also has a small effect on the fit –12 of the 32 planets have nonzero eccentricity. A correlation between tidal heating and adjusted radius gives a coefficient of 0.28.
Fig. 12
The correlation between observed radius and tidal heating for highmass planets of nonzero eccentricity, after removing the effects of the other terms. 
Metallicity also has an effect on planet radius: a radiusmetallicity correlation gives a fairly weak coefficient of –0.25, shown in Fig. 13, but the inclusion of a term for metallicity does improve the SVD fit.
Fig. 13
The correlation between observed radius and metallicity for highmass planets, after removing the effects of the other terms. 
The semimajor axis is no longer seen to have the same effect on planet radii as was seen for lowermass planets. The higher mass of these planets may act to prevent the atmospheric escape that may produce the correlation of radius with semimajor axis seen in lowermass planets.
Adding age to the model slightly decreases the model BIC, from 105 to 96, for the 26 planets that have published isochrone ages, so a small age dependence is seen for highmass planets. This SVD fit produces a small negative coefficient for age of –0.03, showing that radius decreases as the planet ages, as would generally be expected due to KelvinHelmholtz contraction.
3. Discussion
We have attempted to determine the factors that have an effect on planetary radii, along with the magnitude and direction of each significant effect. A positive relationship between planetary equilibrium temperature and radius is seen for Jupiter and highmass planets, showing that the higher the equilibrium temperature, the larger the planet radius, though not significantly for the Saturn mass planets. The radius dependence found here is not as strong as that reported recently by Laughlin et al. (2011) who found a proportionality of above that expected from theoretical calculations. Here, the Saturnmass and lowmass planets show around while the Jupitermass planets show , in total. These lower values of proportionality suggest that kinetic heating (Guillot & Showman 2002), expected to lead to (Laughlin et al. 2011), could be the major source of providing the additional heating to inflate planetary radii, since Ohmic heating should yield a higher dependence on temperature of around (Laughlin et al. 2011).
A negative relationship between host star metallicity and planetary radius is seen for the Saturnmass and highmass planets, showing that as host star metallicity increases, planet radius decreases. This implies firstly that there is a relationship between host star metallicity and the fraction of heavy elements present in a planet, and secondly that the higher metallicity likely results in larger planetary cores, producing smaller radii, both as discussed by Guillot et al. (2006). No relationship with metallicity is seen for the gaseous envelopedominated Jupiter mass planets.
A strong positive relationship between semimajor axis and planetary radius is seen for the Jupitermass planets, such that planets closer to their host stars have smaller radii, an effect in opposition to the bloating caused by strong stellar irradiation which tends to make planets closer to their stars larger. This may be due to atmospheric blowoff in the early stages of the system development or a migration stopping mechanism that leads to planets of higher heavy element contect orbiting closer to the star. The relationship is much weaker for the coredominated Saturnmass planets, and no such relationship is seen for the highmass planets, perhaps because their larger gravitational pull prevents atmospheric escape.
The radii of the planets rises with mass for lowmass planets, is unaffected by mass for Jupitermass planets, and falls with mass for the highmass planets. This changing relationship is as expected with the move from incompressible matter to partially electron degenerate bodies at high mass, though the relationship with mass for Saturnmass planets is stronger than expected from the polytropic relationship, indicating an additional dependence that may be due to the coreenvelope ratio increasing towards lower mass.
A clear contrast between the coredominated Saturnmass planets of < 0.5M_{J} and the gaseous envelopedominated Jupitermass planets of 0.5–2.0 M_{J} is therefore seen in the fits. Planetary mass and heavy element content almost exclusively determine the radius of a Saturnmass planets, with stellar irradiation having little effect, while stellar irradiation and semimajor axis determine the radius of a Jupitermass planet almost entirely.
Once we had determined the best SVD model for each subset of planets, we performed a Monte Carlo SVD analysis of 50 000 runs to determine the uncertainties on the fit coefficients. In each run, each input parameter to the SVD fit was perturbed randomly on a normal distribution about their observed values with standard deviations as their published parameter uncertainty values. A summary of the radius calibration terms and uncertainties is provided in Table 8.
Using the fits obtained for the three subsets of transiting planets to obtain fitted radii for the 119 planets results in Fig. 14, with a generally good agreement between fitted and observed radii. The mean error in fitted radius to the observed radius is 0.11 R_{J} compared to the mean uncertainty in reported observed radius of 0.07 R_{J}. This solution using three subsets of planets provides a better calibration to radius than the single global analysis, where 35 planets had fitted radius errors of greater than 0.2 R_{J} (17 greater than 0.3 R_{J}), and the mean error in fitted radius was 0.16 R_{J}. Here, 18 of the 119 planets have errors greater than 0.2 R_{J} (only 4 greater than 0.3 R_{J}): 8 Saturnmass planets, 6 Jupitermass planets and 4 highmass planets. The two significant outliers are WASP21b, with an overestimated fitted radius of 1.54 R_{J} compared to its measured radius of only 1.07 R_{J}, and HAT32b with an extremely large measured radius of 2.04 R_{J} compared to the low fitted radius of 1.41 R_{J}. The simiarly bloated Saturnmass planet WASP17b, with measured radius 1.99 R_{J} is fitted fairly well to 1.87 R_{J}.
Fig. 14
Results of the radius calibration on 119 transiting exoplanets using the 3 equations given for each subset. 
Approximations such as setting the albedo of all planets to zero in calculating planetary equilibrium temperature may have contributed to the poorer radii fits for some planets, and the model scatter may be reduced if all albedos were known. Additionally, the planetary metallicity may sometimes be enhanced or depleted compared to an average planet orbiting a host star of a certain metallicity, which may lead to larger or smaller than expected cores and thus smaller or larger than expected radii.
References
 Anderson, D. R., Smith, A. M. S., Lanotte, A. A., et al. 2011, MNRAS, 416, 2108 [Google Scholar]
 Baraffe, I., Chabrier, G., Barman, T. S., et al. 2005, A&A, 436, L47 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Batygin, K., & Stevenson, D. J. 2010, ApJ, 714, L238 [NASA ADS] [CrossRef] [Google Scholar]
 Batygin, K., Stevenson, D. J., & Bodenheimer, P. H. 2011, ApJ, 738, 1 [NASA ADS] [CrossRef] [Google Scholar]
 Bodenheimer, P., Lin, D. N. C., & Mardling, R. A. 2001, ApJ, 548, 466 [NASA ADS] [CrossRef] [Google Scholar]
 Bodenheimer, P., Laughlin, G., & Lin, D. N. C. 2003, ApJ, 592, 555 [NASA ADS] [CrossRef] [Google Scholar]
 Burrows, A., & Liebert, J. 1993, Rev. Mod. Phys., 65, 301 [NASA ADS] [CrossRef] [Google Scholar]
 Burrows, A., Guillot, T., Hubbard, W. B., et al. 2000, ApJ, 534, L97 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Burrows, A., Hubeny, I., Budaj, J., & Hubbard, W. B. 2007, ApJ, 661, 502 [NASA ADS] [CrossRef] [Google Scholar]
 Campo, C., Harrington, J., Stevenson, K. B., et al. 2010, in BAAS, 42, AAS/Division for Planetary Sciences Meeting Abstracts, 42, 1091 [Google Scholar]
 Chabrier, G., Baraffe, I., Leconte, J., Gallardo, J., & Barman, T. 2009, in AIP Conf. Ser. 1094, ed. E. Stempels, 102 [Google Scholar]
 Christian, D. J., Gibson, N. P., Simpson, E. K., et al. 2009, MNRAS, 392, 1585 [NASA ADS] [CrossRef] [Google Scholar]
 Enoch, B., Collier Cameron, A., Anderson, D. R., et al. 2011, MNRAS, 410, 1631 [NASA ADS] [Google Scholar]
 Erkaev, N. V., Kulikov, Y. N., Lammer, H., et al. 2007, A&A, 472, 329 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Fortney, J. J., & Nettelmann, N. 2010, Space Sci. Rev., 152, 423 [NASA ADS] [CrossRef] [Google Scholar]
 Fossati, L., Haswell, C. A., Froning, C. S., et al. 2010, ApJ, 714, L222 [NASA ADS] [CrossRef] [Google Scholar]
 Gibson, N. P., Aigrain, S., Pollacco, D. L., et al. 2010, MNRAS, 404, L114 [NASA ADS] [Google Scholar]
 Gillon, M., Anderson, D. R., Triaud, A. H. M. J., et al. 2009, A&A, 501, 785 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Guillot, T. 2005, Ann. Rev. Earth Planet. Sci., 33, 493 [NASA ADS] [CrossRef] [MathSciNet] [PubMed] [Google Scholar]
 Guillot, T. 2008, Phys. Scripta T, 130, 014023 [Google Scholar]
 Guillot, T., & Showman, A. P. 2002, A&A, 385, 156 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Guillot, T., Burrows, A., Hubbard, W. B., Lunine, J. I., & Saumon, D. 1996, ApJ, 459, L35 [NASA ADS] [CrossRef] [Google Scholar]
 Guillot, T., Santos, N. C., Pont, F., et al. 2006, A&A, 453, L21 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Halbwachs, J. L., Mayor, M., & Udry, S. 2005, A&A, 431, 1129 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Hartman, J. D., Bakos, G. Á., Sato, B., et al. 2011, ApJ, 726, 52 [NASA ADS] [CrossRef] [Google Scholar]
 Hayashi, C. 1981, in Fundamental Problems in the Theory of Stellar Evolution, ed. D. Sugimoto, D. Q. Lamb, & D. N. Schramm, IAU Symp., 93, 113 [Google Scholar]
 Hebb, L., CollierCameron, A., Loeillet, B., et al. 2009, ApJ, 693, 1920 [NASA ADS] [CrossRef] [Google Scholar]
 Hebb, L., CollierCameron, A., Triaud, A. H. M. J., et al. 2010, ApJ, 708, 224 [NASA ADS] [CrossRef] [Google Scholar]
 Herbig, G. H. 1952, JRASC, 46, 222 [Google Scholar]
 Hubbard, W. B., Hattori, M. F., Burrows, A., Hubeny, I., & Sudarsky, D. 2007, Icarus, 187, 358 [NASA ADS] [CrossRef] [Google Scholar]
 Husnoo, N., Pont, F., Hébrard, G., et al. 2011, MNRAS, 413, 2500 [NASA ADS] [CrossRef] [Google Scholar]
 Iro, N., Bézard, B., & Guillot, T. 2005, A&A, 436, 719 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Jackson, B., Greenberg, R., & Barnes, R. 2008, ApJ, 681, 1631 [NASA ADS] [CrossRef] [Google Scholar]
 Jackson, B., Miller, N., Barnes, R., et al. 2010, MNRAS, 407, 910 [NASA ADS] [CrossRef] [Google Scholar]
 Joy, A. H. 1945, ApJ, 102, 168 [NASA ADS] [CrossRef] [Google Scholar]
 Laughlin, G., Marcy, G. W., Vogt, S. S., Fischer, D. A., & Butler, R. P. 2005, ApJ, 629, L121 [NASA ADS] [CrossRef] [Google Scholar]
 Laughlin, G., Crismani, M., & Adams, F. C. 2011, ApJ, 729, L7 [NASA ADS] [CrossRef] [Google Scholar]
 Lucy, L. B., & Sweeney, M. A. 1971, AJ, 76, 544 [NASA ADS] [CrossRef] [Google Scholar]
 Maciejewski, G., Dimitrov, D., Neuhäuser, R., et al. 2011, MNRAS, 411, 1204 [NASA ADS] [CrossRef] [Google Scholar]
 Maxted, P. F. L., Anderson, D. R., Gillon, M., et al. 2010, AJ, 140, 2007 [NASA ADS] [CrossRef] [Google Scholar]
 Maxted, P. F. L., Anderson, D. R., Collier Cameron, A., et al. 2011, PASP, 123, 547 [NASA ADS] [CrossRef] [Google Scholar]
 Miller, N., & Fortney, J. J. 2011, ApJ, 736, L29 [NASA ADS] [CrossRef] [Google Scholar]
 MurrayClay, R. A., Chiang, E. I., & Murray, N. 2009, ApJ, 693, 23 [Google Scholar]
 Nymeyer, S., Harrington, J., Hardy, R. A., et al. 2011, ApJ, 742, 35 [NASA ADS] [CrossRef] [Google Scholar]
 Pont, F., Husnoo, N., Mazeh, T., & Fabrycky, D. 2011, MNRAS, 414, 1278 [NASA ADS] [CrossRef] [Google Scholar]
 Ribas, I., & MiraldaEscudé, J. 2007, A&A, 464, 779 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Rowe, J. F., Matthews, J. M., Seager, S., et al. 2008, ApJ, 689, 1345 [NASA ADS] [CrossRef] [Google Scholar]
 Seager, S., Kuchner, M., HierMajumder, C. A., & Militzer, B. 2007, ApJ, 669, 1279 [NASA ADS] [CrossRef] [Google Scholar]
 Snellen, I. A. G., Albrecht, S., de Mooij, E. J. W., & Le Poole, R. S. 2008, A&A, 487, 357 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Southworth, J. 2011, MNRAS, 417, 2166 [NASA ADS] [CrossRef] [Google Scholar]
 Southworth, J., Dominik, M., Jørgensen, U. G., et al. 2011, A&A, 527, A8 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Szydlowski, M., & Kurek, A. 2008, unpublished [arXiv:0801.0638] [Google Scholar]
 Valencia, D., Ikoma, M., Guillot, T., & Nettelmann, N. 2010, A&A, 516, A20 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 VidalMadjar, A., Lecavelier des Etangs, A., Désert, J., et al. 2003, Nature, 422, 143 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 West, R. G. 2011, submitted [Google Scholar]
 Zapolsky, H. S., & Salpeter, E. E. 1969, ApJ, 158, 809 [NASA ADS] [CrossRef] [Google Scholar]
All Tables
All Figures
Fig. 1
MassRadius plot of 119 transiting exoplanets showing the expected massradius relationship for pure H (solid line) Seager et al. (2007). 

In the text 
Fig. 2
Mass against radius residuals after subtracting the Seager et al. (2007) massradius relationship. 

In the text 
Fig. 3
Results of the radius calibration on all 119 transiting exoplanets using the Seager et al. (2007) massradius relationship and a single fourparameter SVD fit. 

In the text 
Fig. 4
The correlation between observed radius and mass for Saturnmass planets, after removing the effects of the other parameters used in the SVD fit. 

In the text 
Fig. 5
The correlation between observed radius and metallicity for Saturnmass planets, after removing the effects of the other parameters used in the SVD fit. 

In the text 
Fig. 6
The correlation between observed radius and planetstar distance for Saturnmass planets, after removing the effects of the other parameters used in the SVD fit. 

In the text 
Fig. 7
The correlation between observed radius and equilibrium temperature for Saturnmass planets, after removing the effects of the other parameters used in the SVD fit. 

In the text 
Fig. 8
The correlation between observed radius and equilibrium temperature for Jupitermass planets, after removing the effects of semimajor axis. 

In the text 
Fig. 9
The correlation between observed radius and semimajor axis for Jupitermass planets, after removing the effects of equilibrium temperature. 

In the text 
Fig. 10
The correlation between observed radius and equilibrium temperature for highmass planets. 

In the text 
Fig. 11
The correlation between observed radius and mass for highmass planets, after removing the effects of other terms. 

In the text 
Fig. 12
The correlation between observed radius and tidal heating for highmass planets of nonzero eccentricity, after removing the effects of the other terms. 

In the text 
Fig. 13
The correlation between observed radius and metallicity for highmass planets, after removing the effects of the other terms. 

In the text 
Fig. 14
Results of the radius calibration on 119 transiting exoplanets using the 3 equations given for each subset. 

In the text 
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