System containing 6 transiting planets around a sunlike star. The system is too far away to be confirmed with dopplar spectrometry. Instead, the planets are close enough together that they were confirmed with Transit Timing Variation, which offered measurements for their mass and densities and compositions. The innermost five are Super-Earths and Neptunians and are compact and within Mercury-like distances, and are b (0.09 AU, 4 ME), c (0.10 AU, 13.5 ME), d (0.16 AU, 6.1 ME), e (0.19 AU, 8.4 ME), f (0.25 AU, 2.3 ME). The planets have surprisingly low density for such small planets and not likely rocky. The inner ones are likely mixture of rock/ice or rock/gas, while the outer three are so large for their mass that they have to have a lot of hydrogen/helium. Their outer shells are probably
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| - System containing 6 transiting planets around a sunlike star. The system is too far away to be confirmed with dopplar spectrometry. Instead, the planets are close enough together that they were confirmed with Transit Timing Variation, which offered measurements for their mass and densities and compositions. The innermost five are Super-Earths and Neptunians and are compact and within Mercury-like distances, and are b (0.09 AU, 4 ME), c (0.10 AU, 13.5 ME), d (0.16 AU, 6.1 ME), e (0.19 AU, 8.4 ME), f (0.25 AU, 2.3 ME). The planets have surprisingly low density for such small planets and not likely rocky. The inner ones are likely mixture of rock/ice or rock/gas, while the outer three are so large for their mass that they have to have a lot of hydrogen/helium. Their outer shells are probably
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| - System containing 6 transiting planets around a sunlike star. The system is too far away to be confirmed with dopplar spectrometry. Instead, the planets are close enough together that they were confirmed with Transit Timing Variation, which offered measurements for their mass and densities and compositions. The innermost five are Super-Earths and Neptunians and are compact and within Mercury-like distances, and are b (0.09 AU, 4 ME), c (0.10 AU, 13.5 ME), d (0.16 AU, 6.1 ME), e (0.19 AU, 8.4 ME), f (0.25 AU, 2.3 ME). The planets have surprisingly low density for such small planets and not likely rocky. The inner ones are likely mixture of rock/ice or rock/gas, while the outer three are so large for their mass that they have to have a lot of hydrogen/helium. Their outer shells are probably fluffy, while cores are rock hard. The outermost giant g is just outside Mercury's distance (0.46 AU, 1 MJ) and doesn't perturb neighbors enough for its mass to be calculated. They are all coplanar and have low eccentricities, none are in resonance, and the system is more compact than any other known system. Systems discovery prompted a briefing of Kepler's overall status.
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