Transits Jupiter

In my experience, a Jupiter transit is a trumpet call to arms. When you see Jupiter poised on the brink of your Sun sign, about to contact your career-oriented Midheaven, or entering your seventh house of marriage, you know that opportunities are available in those arenas. But you have to do your part. To get the most out of Jupiter, make a legitimate effort to learn something, to tackle an old dilemma in a novel way, or to find time for the things you always say you want to do. When you take action under a Jupiter transit, lBE rewards inevitably follow. 

Jupiter transits bring growth, opportunity, and the danger of indolence. 

When the atoms are forced to move closer by the exertion of pressure, their interaction increases and the bands become wider. At sufficiently high pressures the bands overlap again and the properties become metallic. The pressure-induced transition from a non-metal to a metal has been shown experimentally in many cases, for example for iodine and other nonmetals. Under extremely high pressures even hydrogen should become metallic (metallic hydrogen is assumed to exist in the interior of Jupiter). 

The transit method requires that the central star, the planet and the observer are connected by a line of sight. The dark planet passes across the light source and thus diminishes its light intensity to some extent. Observation is only possible when observer, star and planet are in a favourable position, i.e., the planet lies between the star and the observer. In spite of this requirement, the method permits the discovery of planets of about the size of the Earth information is also available on the size, mass and density of the planet as well as on its orbit. Because of its limits of applicability, this method is not often used. In the case of the star OGLE-TR-56, it was possible to detect an extrasolar planet, the orbit of which is very close to its sun only a twentieth of the distance of Mercury away from it. The temperature of the planet was determined to be around 1,900 K its diameter is about 1.3 times larger than that of Jupiter, its density about 500 kg/m3 (Brown, 2003 Konacki, 2003). 

The masses of the planets so far discovered vary between about 0.02 and 18 Jupiter masses. There are also very large variations in the values of the semi-major axis of the planetary orbits. If the first two methods for the discovery of extrasolar planets are compared (Doppler and transit methods), Doyle et al. (2000) point out the following facts around 40,000 photons are required to determine the transit of an extrasolar planet across the star HD 209548 using a photometer. But detection of the same system using variations in radial velocity requires 10 million photons. 

The study of spectroscopy has provided all of the information required to make a positive identification of molecules in space. More interestingly, once the spectrum of a molecule or atom is understood accurately, the interaction of the molecule with its surroundings can be understood as well. Atoms and molecules, wherever they are, can report on their local conditions and be used as probes. We shall see many of these examples where knowledge of molecular properties provides insight into astrochemistry. For example, the understanding developed below will take us from the transition wavelength of Ha to the radius of Jupiter. 

Calculate the Doppler shift that should be observed in the hydrogen atom transition at 656.300 nm for the ascending and descending limbs of Jupiter at the equator. 

A recent success in the detection of H species has been that of the molecular ion H3+. All of the models of ion-molecule chemistry in hydrogen-dominated regions are controlled by reactions of H3+ but until recently the H2+ molecular ion had not been detected. However, the modes of vibration of H3"1" provide for an allowed IR transition at 3.668 pin used for its detection. These ro-vibrational transitions have now been observed in a number of places, including the interstellar medium and in the aurorae of Jupiter. Not all astronomical detection and identification problems have been solved, however, and the most annoying and compelling of these is the problem of diffuse interstellar bands. 

A Doppler shift for the Ha transition is induced by the rotation of Jupiter. 

Fig. 6.5. Computed structures due to the hydrogen dimer, in the quadrupole-induced (0223,2023) components near the So(0) line center at 120 K (the temperature of Jupiter s upper atmosphere). Superimposed with the smooth free — free continuum (dashes) are structures arising from bound — free (below 354 cm-1) and free - bound (above 354 cm-1) transitions of the hydrogen pair (dotted). The convolution of the spectrum with a 4.3 cm-1 slit function (approximating the instrumental profile of the Voyager infrared spectrometer) is also shown (heavy line) [282].

Fig. 7.3. Upper figure Emission spectrum of Jupiter in the far infrared two diffuse, dark fringes are seen at the H2 Sb(0) and Sb(l) rotational transition frequencies, caused by collision-induced absorption in the upper, cool regions. The lower figure presents an enlarged portion which shows the dimer structures near the So(0) transition frequency [150].

The nature of these two phases helps to throw light on the metal-nonmetal transition. For example there has been much speculation that hydrogen molecules at sufficiently high pressure, such as those occurring on the planet Jupiter, might undergo a transition to un alkali metal The fundamental transition is one of a dramatic change of the van der Waals interactions of H, molecules into metallic cohesion. ... 

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. 

Because of the small mass of the proton, the decrease of the transition dipole moment as we move to higher overtone bands of H3 is not as drastic as in ordinary molecules. The band origins, transition moments, relative intensities and Einstein s spontaneous emission probabilities theoretically calculated by Dinelli, Miller and Tennyson are listed in Table 1. Note that the value of Aij is larger for the 2v2(2) overtone band than for the Vj fundamental band because the factor in the Einstein formula overrides the reduction of j n. This explains the strong 2 pm overtone emission observed in Jupiter. ... 

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