Four Sub-Saturns with Dissimilar Densities: Windows into Planetary Cores and Envelopes

被引:71
作者
Petigura, Erik A. [1 ]
Sinukoff, Evan [2 ]
Lopez, Eric D. [3 ]
Crossfield, Ian J. M. [4 ]
Howard, Andrew W. [1 ]
Brewer, John M. [5 ]
Fulton, Benjamin J. [1 ,2 ]
Isaacson, Howard T. [6 ]
Ciardi, David R. [7 ]
Howell, Steve B. [8 ]
Everett, Mark E. [9 ]
Horch, Elliott P. [10 ]
Hirsch, Lea A. [6 ]
Weiss, Lauren M. [11 ]
Schlieder, Joshua E. [7 ]
机构
[1] CALTECH, 1200 E Calif Blvd, Pasadena, CA 91125 USA
[2] Univ Hawaii Manoa, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA
[3] Univ Edinburgh, Inst Astron, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland
[4] Univ Calif Santa Cruz, 1156 High St, Santa Cruz, CA 95064 USA
[5] Yale Univ, New Haven, CT 06520 USA
[6] Univ Calif Berkeley, Berkeley, CA 94720 USA
[7] CALTECH, IPAC NExScI, 770 South Wilson Ave, Pasadena, CA 91125 USA
[8] NASA, Ames Res Ctr, Mail Stop 204-14, Moffett Field, CA 94035 USA
[9] Natl Opt Astron Observ, 950 North Cherry Ave, Tucson, AZ 85719 USA
[10] Southern Connecticut State Univ, Dept Phys, 501 Crescent St, New Haven, CT 06515 USA
[11] Univ Montreal, Inst Rech Exoplanetes, Montreal, PQ, Canada
关键词
planets and satellites: composition; planets and satellites: detection; planets and satellites: dynamical evolution and stability; planets and satellites: formation; planets and satellites: gaseous planets; planets and satellites: interiors; MASS PLANET; URANIAN SATELLITES; TIDAL EVOLUTION; KEPLER PLANETS; STARS; K2; PHOTOMETRY; TRANSIT; HOT; EXOPLANETS;
D O I
10.3847/1538-3881/aa5ea5
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We present results from a Keck/HIRES radial velocity campaign to study four sub-Saturn-sized planets, K2-27b, K2-32b, K2-39b, and K2-108b, with the goal of understanding their masses, orbits, and heavy-element enrichment. The planets have similar sizes (R-P = 4.5-5.5 R circle plus), but have dissimilar masses (M-P = 16-60 M circle plus), implying a diversity in their core and envelope masses. K2-32b is the least massive (M-P = 16.5. 2.7M circle plus) and orbits in close proximity to two sub-Neptunes near a 3: 2: 1 period commensurability. K2-27b and K2-39b are significantly more massive at M-P = 30.9. 4.6M circle plus and M-P= 39.8. 4.4M circle plus, respectively, and show no signs of additional planets. K2-108b is the most massive at M-P= 59.4. 4.4M circle plus, implying a large reservoir of heavy elements of about approximate to 50 M circle plus. Sub-Saturns as a population have a large diversity in planet mass at a given size. They exhibit remarkably little correlation between mass and size; sub-Saturns range from approximate to 6-60 M circle plus, regardless of size. We find a strong correlation between planet mass and host star metallicity, suggesting that metal-rich disks form more massive planet cores. The most massive sub-Saturns tend to lack detected companions and have moderately eccentric orbits, perhaps as a result of a previous epoch of dynamical instability. Finally, we observe only a weak correlation between the planet envelope fraction and present-day equilibrium temperature, suggesting that photo-evaporation does not play a dominant role in determining the amount of gas sub-Saturns accrete from their protoplanetary disks.
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页数:19
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