Hot Jupiters

There is an increasing effort to model the processes and effects of photochemistry in exoplanet atmospheres [79-82], The absorption of UV and VUV radiatiOTi will lead to dissociation of atmospheric molecules this will occur high in the atmosphere before most incident UV is scattered back into space. The dissociaticMi products will participate in complex reaction schemes. For hot Jupiters, photochemistry will likely be more complex than for our solar system Jupiter. Molecules that are cmidensed below the Jovian clouds (e.g. H2O, H2S, NH3) and are thus protected from photodissociation, will be gaseous in the atmospheres of hot Jupiters. Sulphur and nitrogen compounds may play an important role in hot Jupiter photochemistry and also perhaps in haze production [83]. 

The first discovery of a massive planet, 51 Peg B, was made in 1995 by Mayor and Queloz, 1995 [221], This object is also close to its parent star 51 Peg, at a distance of only 0.05 AU. A new class of planets was defined when it became clear that such objects are quite common. About 50% of known extrasolar planets belong to this group. These hot Jupiters have the following characteristics ... 

A study of a typical hot Jupiter (HD 209458 b, see Chap. 7) was made to model the expected dynamic processes in its atmosphere. The day-night temperature differences are expected about 200 K. Also the existence of jets and up- and downwelling regions is predicted (Showman and Guillot, 2000 [309]). 

The spectroscopic signatures of transiting hot Jupiters were studied by Brown et al., 2000 [46]. The depth of absorption features could reach up to 10 of the parent star s continuum intensity. 

Unite the one with the other, so that the two waters may be one This [conjoined] stream will possess the forces of each of them, mixed together, just as the fountain of Jupiter Hammon is hot and cold at the same time. 

Evaporites on Mars and Europa. The NASA s robotic explorers, Spirit and Opportunity, landed on at Mars and examined their landing sites for past environmental conditions. Kinds of minerals in a hot-spring environment and dried-up lake beds were photographed suggesting future use of ESR to date these evaporate with a portable ESR on the rover. Sulfate mineral precipitation, epsonite, MgS04 with 7 hydration water molecules in frozen ice, was studied by sampling the icy environment, especially icy fault on the surface of Europa, a satellite of Jupiter.61... 

Although the disk mass is dominated by hydrogen, much less is known about its dispersal. Tracers of hot gas in the innermost disk regions show a one-to-one correspondence to the presence of hot dust (Harfigan et al. 1995) and gas accretion to the stars declines at the same rate as hot dust disperses. Spitzer studies of mid-infrared ro-vibrational lines probe warm gas on orbits similar to Jupiter s and demonstrate the loss of gas in few tens of millions of years (Pascucci et al. 2007). Gas in the coldest disk regions can be traced through CO rotational lines such studies also suggest a gas depletion by 10 Myr. The combined astronomical evidence shows that (1) dust disks dissipate in 3—8 Myr via rapid inside-out dispersal (2) gas dissipates in a similar, or perhaps even shorter timescale. 

Figure 5.5 Winds in the solar nebula might be one of the possible processes responsible for the mixing of hot and cold components found in both meteorites and comets. Meteorites contain calcium-aluminum-rich inclusions (CAIs, formed at about 2000 K) and chondrules (formed at about 1650K), which may have been created near the proto-Sun and then blown (gray arrows) several astronomical units away, into the region of the asteroids between Mars and Jupiter, where they were embedded in a matrix of temperature-sensitive, carbon-based cold components. The hot component in comets, tiny grains of annealed silicate dust (olivine) is vaporized at about 1600 K, suggesting that it never reached the innermost region of the disk before it was transported (white arrows) out beyond the orbit of Pluto, where it was mixed with ices and some unheated silicate dust ( cold components). Vigorous convection in the accretion disk may have contributed to the transport of many materials and has been dramatically confirmed by the Stardust mission (Nuth 2001).

During the preparation of this manuscript, we identified a hot-band transition in the Jupiter spectrum see below). We believe the sensitivity of modern spectrometers is sufficient to observe many of them. These spectral lines will serve as a useful thermometer for astronomical objects. 

Nebular Gases and Earth-like versus Jupiter-like Planets Depletion in Moderately Volatile Elements Solar Mass Stars and Heating of the Inner Disk The Hot Nebula" Model... 

On Earth, sulfur is nearly ubiquitous because of its connection with volcanic activity. Volcanoes and other hot spots, like Yellowstone National Park, emit sulfur-containing gases, notably sulfur dioxide (SO ). The gases cool and condense, eventually hardening into sulfur crystals and compounds, the purest being lemon yellow in color. (Extraterrestrial sulfur atoms, and SO, have been also detected in the atmosphere of one of Jupiter s moons, lo, which boasts numerous active volcanoes.)... 

Good Jupiter (Tin) possesses almost the middle or mean place between metals, it being not too hot, nor too cold, nor too warm, nor too moist, it hath no excess of Mercury, nor of Salt, and it hath the least of Sulphur in it. 

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