Extreme solar sailing for fast transit exploration of solar system and interstellar medium

2021 ◽  
Author(s):  
Artur Davoyan
1992 ◽  
Vol 9 ◽  
pp. 341-345
Author(s):  
T. Owen

AbstractValues of D/H measured in the methane on the giant planets and Titan indicate the presence of two distinct reservoirs of deuterium in the outer solar system. The dominant reservoir is in hydrogen gas, the second, multi-component reservoir is found in the hydrogen that is bound in condensed compounds. Both reservoirs appear to have originated in the interstellar medium. In contrast, the values of D/H in water vapor on Mars and Venus (especially) exhibit a large enrichment from the “condensed matter” starting value. Interpretation of this enrichment may illuminate the history of water on these two planets.


1992 ◽  
Vol 150 ◽  
pp. 97-101 ◽  
Author(s):  
T. Owen

Values of D/H measured in the methane on the giant planets and Titan indicate the presence of two distinct reservoirs of deuterium in the outer solar system. The dominant reservoir is in hydrogen gas, the second, multi-component reservoir is found in the hydrogen that is bound in condensed compounds. Both reservoirs appear to have originated in the interstellar medium. In contrast, the values of D/H in water vapor on Mars and Venus (especially) exhibit a large enrichment from the “condensed matter” starting value. Interpretation of this enrichment may illuminate the history of water on these two planets.


2020 ◽  
pp. 115-129
Author(s):  
Ю.Д. КУЗЬМИН ◽  
В.Г. САХНО

По одной из гипотез, вода на Земле имеет метеорное (поверхностное), а не ювенильное (земное) происхождение. Она не может образовываться в конденсированных средах, т.е. в недрах планеты, как считали и считают многие геологи и геофизики. Данный вывод требует других подходов, отличных от устоявшихся взглядов на происхождение воды, эволюцию гидросферы, атмосферы и содержания воды в горных породах на разных геофизических уровнях Земли и других планетах Солнечной системы. Согласно нашей гипотезе, вода на Земле образовалась в результате синтеза водорода и кислорода из космического газопылевого вещества на горячей поверхности твердой планеты с последующим формированием атмосферы, гидросферы Земли и их активным участием в эволюции Земли, во всех геофизических и геохимических процессах. There is one hypothesis that the Earths water is of meteoric rather than endogenous origin. It cannot emerge in condensed environments, namely in the planets interior, as it was believed by many geologists and geophysics. This inference requires other approaches differing from the fixed views on the water origin, evolvement of hydrosphere and atmosphere, water content of rocks in various geophysical layers of the Earth and on other planets of the Solar System. According to our hypothesis, water is a result of synthesis of hydrogen and oxygen from interstellar medium on a hot surface of terrestrial planet followed by the birth of atmosphere and hydrosphere which played a great part in the evolution and all geophysical and geochemical processes of the Earth.


2003 ◽  
Vol 718 ◽  
pp. 659-661 ◽  
Author(s):  
S. Kawanomoto ◽  
K.T. Suzuki ◽  
H. Ando ◽  
T. Kajino

2002 ◽  
Vol 12 ◽  
pp. 48-51 ◽  
Author(s):  
L.B.F.M. Waters ◽  
F.J. Molster

AbstractAn overview is given of the occurrence and properties of crystalline silicates in space. Crystalline silicates are found in circumstellar shells of both young and evolved stars, and are present in Solar System comets. These silicates are Mg-rich and Fe-poor, in contrast to amorphous silicates. We discuss the formation mechanism of crystalline silicates and the apparent lack of these grains in the interstellar medium.


2003 ◽  
Vol 288 (3) ◽  
pp. 369-375 ◽  
Author(s):  
T.W. Hartquist ◽  
S.A.E.G. Falle ◽  
D.A. Williams

2002 ◽  
Vol 12 ◽  
pp. 79-81
Author(s):  
Kenneth R. Sembach

AbstractThe Far Ultraviolet Spectroscopic Explorer (FUSE) is presently producing high resolution (R ∼ 20,000) absorption-line spectra of astronomical objects ranging from Solar System planets to quasars. The 900-1200 Å spectral region observed by FUSE is exceedingly rich in atomic and molecular transitions arising out of the ground state. It is already clear from early FUSE observations that the atomic data (e.g., oscillator strengths) for some transitions are considerably different than those predicted by theoretical calculations. I briefly describe the most pressing oscillator strength needs in this wavelength range for studies of the interstellar medium.


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