Juno Mission Simulation

AbstractThe giant planets of our solar system contain a record of elemental and isotopic ratios of keen interest for what they tell us about the origin of the planets and in particular the volatile compositions of the solid phases. In situ measurements of the Jovian atmosphere performed by the Galileo Probe during its descent in 1995 demonstrate the unique value of such a record, but limited currently by the unknown abundance of oxygen in the interior of Jupiter–a gap planned to be filled by the Juno mission set to arrive at Jupiter in July of 2016. Our lack of knowledge of the oxygen abundance allows for a number of models for the Jovian interior with a range of C/O ratios. The implications for the origin of terrestrial water are briefly discussed. The complementary data sets for Saturn may be obtained by a series of very close, nearly polar orbits, at the end of the Cassini-Huygens mission in 2016-2017, and the proposed Saturn Probe. This set can only obtain what we have for Jupiter if the Saturn Probe mission carries a microwave radiometer.

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Lichenometry and Schmidt hammer tests in the Kaunertal glacier foreland (Ötztal Alps) during the AMADEE-15 Mars Mission Simulation

Miscellanea Geographica ◽

10.1515/mgrsd-2017-0027 ◽

2017 ◽

Vol 21 (4) ◽

pp. 190-196

Author(s):

Jan Czempiński ◽

Maciej Dąbski

Keyword(s):

Little Ice Age ◽

Ice Age ◽

Schmidt Hammer ◽

Mars Mission ◽

Frontal Part ◽

Glacier Foreland ◽

Glacier Front ◽

Relative Stabilization ◽

History Of ◽

Mission Simulation

AbstractThe aim of this article is to show the results of the lichenometrical and Schmidt hammer measurements performed in 2015 during the AMADEE-15 Mars Mission Simulation in the Ötztal Alps in order to test the capabilities of analogue astronauts and collect information on the geomorphic history of the study area since the Little Ice Age (LIA). The results obtained differ significantly from our expectations, which we attribute to differences in the field experience of participants and the astronauts’ technical limitations in terms of mobility. However, the experiments proved that these methods are within the range of the astronauts’ capabilities. Environmental factors, such as i) varied petrography, ii) varied number of thalli in test polygons, and iii) differences in topoclimatic conditions between the LIA moraine and the glacier front, further inhibited simple interpretation. The LIA maximum of the Kaunertal glacier occurred in AD 1850, and relative stabilization of the frontal part of the rock glacier occurred in AD 1711.

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Asteroid masses obtained with INPOP planetary ephemerides

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stz3407 ◽

2019 ◽

Vol 492 (1) ◽

pp. 589-602 ◽

Cited By ~ 2

Author(s):

A Fienga ◽

C Avdellidou ◽

J Hanuš

Keyword(s):

Monte Carlo ◽

Monte Carlo Sampling ◽

New Method ◽

Navigation Data ◽

The Earth ◽

Better Than ◽

Juno Mission

ABSTRACT In this paper, we present masses of 103 asteroids deduced from their perturbations on the orbits of the inner planets, in particular Mars and the Earth. These determinations and the INPOP19a planetary ephemerides are improved by the recent Mars orbiter navigation data and the updated orbit of Jupiter based on the Juno mission data. More realistic mass estimates are computed by a new method based on random Monte Carlo sampling that uses up-to-date knowledge of asteroid bulk densities. We provide masses with uncertainties better than 33${{\ \rm per\ cent}}$ for 103 asteroids. Deduced bulk densities are consistent with those observed within the main spectroscopic complexes.

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