The data collected at Jupiter (after a 1.5 Instrument to determine the interior structures of Jupiter and Uranusĭuring flybys of each planet. We have designed a Discovery mission around such an
The greatĪdvantage of a DI is that its observations do not require the spacecraft Revolutionized our understanding of the interior of stars. The well-established fields of helio- and stellar-seismology, which have A planetary Doppler Imager (DI) builds on Provide detailed information on interior structure from great distances Spacecraft in low orbits have been the primary way to tease out That Ice Giants are far more abundant in our galaxy than Gas Giants Measurement needed to advance our understanding of the formation andĮvolution of planetary systems, particularly. Knowing the interior structure of both types of planets is a key
Water by mass, compared to Gas Giants which are ~95% hydrogen and The Ice Giants (Uranus and Neptune) are fundamentally different than theīetter-known Gas Giants (Jupiter and Saturn). Uranus/Neptune-like giant planets by a hydrodynamical accretion in. The latter explain low-mass gaseous envelopes and Observation to decide between migration models and in-situ formation Models for the formation of hot giant planets and is a critical Hence I argue that the detection of a Hot Neptune would refute migration The formation of Hot Jupiters, they are expected to have large They are expected to grow the large, Jupiter-mass envelopes thatĬorrespond to their supercritical cores. They do so in the presence of a disk of considerable mass. The presence of a significant nebula disk. Necessary condition for the proposed type-I/II migration to operate, is Small orbital radii, after they accumulated their massive envelopes. Their formation regions, beyond the snow-line, say, to their ultimately The other hand, formation models for Jupiters, like 51 Pe- gasi b or HDĢ09458 b, often invoke orbital migration to transfer giant planets from Grow to masses comparable to Jupiter's mass under such conditions. Hence a proto Neptune should accrete gas and rapidly More precisely the core is supercriticalīut the mass of hydrogen and helium envelope is only a small fraction ofīecause the core mass is supercritical, quasi-hydrostatic giant planetįormation mod- els predict envelope growth to large masses, if nebula A hot Neptune is a hypothetical giant planet in an orbit close to its
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