TY  - CHAP
A1  - Grundmann, Jan Thimo
A1  - Bauer, Waldemar
A1  - Borchers, Kai
A1  - Dumont, Etienne
A1  - Grimm, Christian D.
A1  - Ho, Tra-Mi
A1  - Jahnke, Rico
A1  - Lange, Caroline
A1  - Maiwald, Volker
A1  - Mikulz, Eugen
A1  - Quantius, Dominik
A1  - Reershemius, Siebo
A1  - Renger, Thomas
A1  - Riemann, Johannes
A1  - Sasaki, Kaname
A1  - Seefeldt, Patric
A1  - Spietz, Peter
A1  - Spröwitz, Tom
A1  - Toth, Norbert
A1  - Wejmo, Elisabet
A1  - Biele, Jens
A1  - Krause, Christian
A1  - Cerotti, Matteo
A1  - Peloni, Alessandro
A1  - Dachwald, Bernd
T1  - Small Spacecraft Solar Sailing for Small Solar System Body Multiple Rendezvous and Landing
T2  - 2018 IEEE Aerospace Conference : 3-10 March 2018
Y1  - 2018
SN  - 978-1-5386-2014-4
ER  - 
TY  - CHAP
A1  - Jean-Pierre P., de Vera
A1  - Baque, Mickael
A1  - Billi, Daniela
A1  - Böttger, Ute
A1  - Bulat, Sergey
A1  - Czupalla, Markus
A1  - Dachwald, Bernd
A1  - de la Torre, Rosa
A1  - Elsaesser, Andreas
A1  - Foucher, Frédéric
A1  - Korsitzky, Hartmut
A1  - Kozyrovska, Natalia
A1  - Läufer, Andreas
A1  - Moeller, Ralf
A1  - Olsson-Francis, Karen
A1  - Onofri, Silvano
A1  - Sommer, Stefan
A1  - Wagner, Dirk
A1  - Westall, Frances
T1  - The search for life on Mars and in the Solar System - strategies, logistics and infrastructures
T2  - 69th International Astronautical Congress (IAC)
N2  - The question "Are we alone in the Universe?" is perhaps the most fundamental one that affects mankind. How can we address the search for life in our Solar System? Mars, Enceladus and Europa are the focus of the search for life outside the terrestrial biosphere. While it is more likely to find remnants of life (fossils of extinct life) on Mars because of its past short time window of the surface habitability, it is probably more likely to find traces of extant life on the icy moons and ocean worlds of Jupiter and Saturn. Nevertheless, even on Mars there could still be a chance to find extant life in niches near to the surface or in just discovered subglacial lakes beneath the South Pole ice cap. Here, the different approaches for the detection of traces of life in the form of biosignatures including pre-biotic molecules will be presented. We will outline the required infrastructure for this enterprise and give examples of future mission concepts to investigate the presence of life on other planets and moons. Finally, we will provide suggestions on methods, techniques, operations and strategies for preparation and realization of future life detection missions.
KW  - life detection
KW  - Mars
KW  - icy moons
KW  - habitability
KW  - space missions
Y1  - 2018
N1  - 69th International Astronautical Congress (IAC), Bremen, Germany, 1-5 October 2018.
SP  - 1
EP  - 8
ER  - 
TY  - CHAP
A1  - Baader, Fabian
A1  - Reiswich, M.
A1  - Bartsch, M.
A1  - Keller, D.
A1  - Tiede, E.
A1  - Keck, G.
A1  - Demircian, A.
A1  - Friedrich, M.
A1  - Dachwald, Bernd
A1  - Schüller, K.
A1  - Lehmann, R.
A1  - Chojetzki, R.
A1  - Durand, C.
A1  - Rapp, L.
A1  - Kowalski, Julia
A1  - Förstner, R.
T1  - VIPER - Student research on extraterrestrical ice penetration technology
T2  - Proceedings of the 2nd Symposium on Space Educational Activities
N2  - Recent analysis of scientific data from Cassini and earth-based observations gave evidence for a global ocean under a surrounding solid ice shell on Saturn's moon Enceladus. Images of Enceladus' South Pole showed several fissures in the ice shell with plumes constantly exhausting frozen water particles, building up the E-Ring, one of the outer rings of Saturn. In this southern region of Enceladus, the ice shell is considered to be as thin as 2 km, about an order of magnitude thinner than on the rest of the moon. Under the ice shell, there is a global ocean consisting of liquid water. Scientists are discussing different approaches the possibilities of taking samples of water, i.e. by melting through the ice using a melting probe. FH Aachen UAS developed a prototype of maneuverable melting probe which can navigate through the ice that has already been tested successfully in a terrestrial environment. This means no atmosphere and or ambient pressure, low ice temperatures of around 100 to 150K (near the South Pole) and a very low gravity of 0,114 m/s^2 or 1100 μg. Two of these influencing measures are about to be investigated at FH Aachen UAS in 2017, low ice temperature and low ambient pressure below the triple point of water. Low gravity cannot be easily simulated inside a large experiment chamber, though. Numerical simulations of the melting process at RWTH Aachen however are showing a gravity dependence of melting behavior. Considering this aspect, VIPER provides a link between large-scale experimental simulations at FH Aachen UAS and numerical simulations at RWTH Aachen. To analyze the melting process, about 90 seconds of experiment time in reduced gravity and low ambient pressure is provided by the REXUS rocket. In this time frame, the melting speed and contact force between ice and probes are measured, as well as heating power and a two-dimensional array of ice temperatures. Additionally, visual and infrared cameras are used to observe the melting process.
Y1  - 2018
SP  - 1
EP  - 6
ER  -