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Logo Institut für Geophysik und Extraterrestische Physik der TU Braunschweig

Rosetta

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Die Kometen a) Halley, b) Borrelly, c) Wild2 und d) Tempel 1, gesehen von den Raumsonden GIOTTO, DEEP SPACE1, Stardust und DEEP IMPACT
The comets a) Halley, b) Borrelly, c) Wild2 and d) Tempel 1, as seen by the space crafts GIOTTO, DEEP SPACE1, Stardust and DEEP IMPACT

Comets are an extraordinary occurence on the night sky. Consisting of unprocessed material of the early solar system, they provide important indications of its formation. The European spacecraft Rosetta will rendezvous the comet 67P/Churyumov-Gerasimenko in may 2014 in order to make measurements concerning its physical and chemical properties, the structure of the nucleus and its interaction with the solar wind. Therefore, Rosetta will orbit the comet in a distance of a few kilometers. Additionally, the lander PHILEA will be deployed onto the nucleus to perform the first experiments on the surface of a comet. Together with Churyumov-Gerasimenko, the orbiter and the lander will approach the sun in summer 2015 investigating the comet's increasing activity as an "in-situ" measurement.

The IGEP participates in the Rosetta mission with an experiment both on the orbiter (RPC) as on the lander (ROMAP). That means, that both experiments were partly developped at the IGEP and that scientists at the IGEP are the PIs of the experiments.

The mission was launched on march 2, 2004 by an Ariane-5 launch vehicle from Kourou, French Guayana. During its long way to 67p/Churymov-Gerasimenko, Rosetta will swing-by the planet Mars and fly-by the asteroids 2867 Steins and 21 Lutetia and study them from greater distance.

Rosetta Sonde

Mission schedule

Event Nominal date
Launch March 2004
First Earth gravity assist March 2005
Mars gravity assist February 2007
Second Earth gravity assist November 2007
Asteroid Steins flyby September 2008
Third Earth gravity assist November 2009
Asteroid Lutetia flyby July 2010
Enter hibernation July 2011
Exit hibernation January 2014
Rendezvous manoeuvre May 2014
Start Global Mapping August 2014
Lander Delivery November 2014
Perihelion Passage August 2015
End of Mission December 2015

The Rosetta team at the IGEP

  • Karl-Heinz Glaßmeier (Experiment PI: RPC-MAG)
  • Hans-Ulrich Auster (Experiment PI: ROMAP)
  • Karl-Heinz Fornaçon
  • Ingo Richter (Experiment TM: RPC-MAG)
  • Bernd Stoll
  • Philip Heinisch
  • Dr. Christoph Koenders
  • Christian Narbert
  • Charlotte Götz
  • Katharina Ostaszewski
Der Stein von Rosetta
The Rosetta Stone.

The mission was named after the "Rosetta Stone", found in 1799 in Egypt, which helped the linguists Champollion and Young for the first time to unravel the hieroglyphs. And just as this stone contributed in understanding the civilization of the ancient Egypt, the Rosetta space mission is intended to disclose the last secrets of the oldest inhabitants of our solar system: the comets. Consisting of precursor material of the solar system, comets material has hardly changed for the last 4,6 billion years. The study of comets offers therefore an unique possibility to look back in time and to explore the provenience of our solar system.

 

Scientific aims

As comets have not yet been analyzed in-situ, many questions concerning their structure and composition still remain unanswered. Therefor, the scientific objectives of the Rosetta mission are the followings:

  • a global characterization of the nucleus
  • the determination of its dynamic properties
  • the surface morphology and composition
  • the determination of chemical, mineralogical and isotopic compositions of volatiles and refractories in the cometary nucleus
  • the determination of the physical properties and interrelation of volatiles and refractories in the cometary nucleus
  • studies of the development of cometary activity and the processes in the surface layer of the nucleus and inner coma, that is dust/gas interaction
  • studies of the evolution of the interaction region of the solar wind and the outgassing comet during perihelion approach

The interaction between the comet and the solar wind can be characterized by plasma properties as for example plasma waves plasmaboundaries. It depends on the solar wind intensity, on the comets outgassing rate increasing with its vicinity to the sun and its potentially intrinsic magnetic field. The magnetic properties of comets could hint at its own origin: Up to now, it is not yet well understood, how and why dust and ice stuck together to form comets. Magnetic attraction could possibly have contributed to this process. Hence, both the orbiter as the lander are equipped with a combined

plasma and magnetometer experiment (RPC onboard the orbiter and ROMAP onboard the Lander). To estimate the required instruments sensitivity, numerical simulations concerning the interactions between the solar wind plasma and the comets ionosphere were performed at the Institut for Theoretical Physics. They shed light on the plasmaphysical environment of the comets nucleus. Besides the electromagnetic field distribution also energy spectra of the involved ion species are computed by these simulations. According to these simulations, C-G has to be classified as a "weak comet", meaning that the qualitative conditions in the plasma environment are significantly different in comparison to the classical description of a strong comet. Therefore, the simulations provide precious assistance at the mission planning as well as at the interpretation of the measurement results.

Landeanimation

Wissenschaftlerinnen und Wissenschaftler vom Institut für Geophysik und extraterrestrische Physik der Technischen Universität Braunschweig haben eine Videoanimation erstellt, die die Landung von Philae auf der Kometenoberfläche zeigt. Genutzt haben sie dafür die wissenschaftlichen Messdaten der beiden Braunschweiger Magnetometer "RPC-Mag" und "ROMAP" sowie weiterer Instrumente an Bord der Landeeinheit. Das internationale Forscherteam um Dr. Hans-Ulrich Auster, Dr. Ingo Richter und Prof. Dr. Karl-Heinz Glaßmeier stellte am 12. November 2014 mithilfe des Magnetometers "ROMAP" als erstes die ungeplante mehrmalige Landung auf dem Kometen 67P/Churyumov-Gerasimenko fest. Doch was die Wissenschaftlerinnen und Wissenschaftler damals anhand ihrer Messdaten ablesen konnten, machte ihr Kollege Philip Heinisch vom Braunschweiger Rosetta-Team zum ersten Jahrestag der Landung in einer Videoanimation sichtbar.
Seit der Landung war der Rosetta-Orbiter auf der Suche nach dem genauen Standort von Philae auf der Kometenoberfläche. Unter anderem mithilfe der rekonstruierten Flugbahn des Landers gelang es dem OSIRIS-Team am 5. September 2016 auf einer hochaufgelösten Fotografie Philae wieder zu finden.

 

Rosetta at the comet

Since August, 6 2014 Rosetta is in orbit around the comet 67P/Churyumov-Gerasimenko. On the November, 12 the Rosetta mission reached one of its highlights when the lander Philae was separated from the orbiter to land on the comet's surface. Both the magnetometer on board the orbiter (RPC-Mag) as well as the magnetometer on board the lander (ROMAP) recorded the different events on this day.

 

Separation of the Philae

RPC-Mag bestätigt Seperation
ROMAP bestätigt Seperation

The separation of the lander left a clear signature in the magnetic field data at 08:35 UTC recorded by the orbiter magnetometer. The lander creates his own magnetic field which is superimposed on the background magnetic field. As this influence disappears after separation it can be seen as a clear jump in the data. In the same way the lander magnetometer is also influenced by the orbiter's presence and a similar jump can be seen in the magnetic field data obtained by the lander instrument.

 

Boom deployment

Ausklappen des Booms

The instrument ROMAP (Rosetta Lander Magnetometer and Plasma Monitor) is located at the end of a boom. During the journey to the comet the boom was retracted to the lander body. After separation this boom deployed and the magnetometer changed its position relative to Philae's body. This was recorded and confirmed by the magnetometer at 08:56 UTC.

 

Landing on the surface of the comet

Landung auf der Oberfläche des Kometen
EDM der Landungen

After seven hours of decent Philae arrived at the desired landing site at 15:34 UTC. There the lander rebounced and floated above the comet's surface for another two hours. The comet's gravity pulled Philae back to the ground and the lander touched the surface for the second time at 17:25. Once again it bounced back into space and stayed on the ground after the third landing at 17:31. With each ground contact the landing gear of Philae was moving while adapting to the ground. These movements have been detected by ROMAP and every single touchdown left specific signatures in the data (left figure).

With the help of appropriate analyses methods the measured events can be seen more clearly in the data. In the right figure the second and third touchdown are shown after a method called EMD (Empirical Mode Decomposition) was applied to the data. The EMD is a numerical procedure to find and separate the intrinsic modes of a time series.

ROMAP - Lander-Magnetometer and Plasma Monitor
ROMAP

ROMAP (ROsetta Lander MAgnetometer and Plasma Monitor) consists of the Rosetta Lander-Magnetometer (ROLAND) and the Lander Plasma Monitor (SPM). The Fluxgate-Magnetometer, designed and built lead-managed by the Institute for Geophysics und extraterrestrial Physics, is situated in zhe center of the experiment. It consists of two entwined ringcores plus pick-up coils and Helmholtz coils for each sensor axis. With a weight of less than 40 g it can perform measurements betweenn +/- 2000nT with a resolution of 10 pT. The IWF (Graz) and the MPE Garching joined the development and construction of the magnetometer and its electronics.

 

ROMAG: Parameter

Parameter  
Sensor mass 35 g
Sensor volume 523 cm³
Electronics mass 150 g
Resolution 10 pT
Dynamic range 4000nT
Sensor noise (@1Hz) 10pT/(Hz)1/2
Bandwidth 0 - 32Hz
Sample rate [1; 64] vecs/s
Power (incl. plasmamonitor) 1 W
Temperature range -160 ... +120C
Time of operation ~ weeks

The plasma monitor, a cooperation between KFKI (Budapest),MPS (Katlenburg-Lindau) and IKI (Moskau), measures the electron and ion distribution in a wide energy range. Furthermore, a Penning sensor and a Pirani sensor for pressure measurements are available (10-8-10-3mbar respectively 10-3-10mbar). The electronics for both experiments are located inside the lander, the sensors, except for the pressure sensors,are mounted on a small boom.

 

Links

  • Science Operation and Navigation Center (SONC),CNES
  • Lander Control Center (LCC), DLR
  • Max-Planck-Institut für Sonnensystemforschung, Katlenburg-Lindau
  • Max-Planck-Institut für extraterrestrische Physik, Garching
  • Institut für Weltraumforschung, Graz
The Orbiter magnetometer: RPC-MAG
Der RPC Fluxgate Sensor

The Orbiter-Magnetometer is part of the Rosetta Plasma Consortium (RPC) and was developped in a close cooperation with the Imperial College (London). The instrument consists of two identical fluxgate sensors mounted on a 1.5 m long boom outside the spacecraft andan electronics box placed inside the orbiter.The sensor has beeen designed and manufactured in lead-management by Prof. Dr. Karl-Heinz Glaßmeier at the IGEP in Braunschweig. The development of the electronics was a teamwork with the IWF in Graz.

 

RPC-MAG Parameter

Parameter  
Sensor mass 45 g
Sensor volume 23 cm³
Electronics mass 336 g
Resolution 31 pT
Dynamic range 16384 nT
Sensor noise(@1Hz) 10pT/(Hz)1/2
Bandwidth 0 10 Hz
Sample rate 20 vectors/s
Power 840 mW
Temperature range -160 ... +120C
Time of operation 15 years

Links

  • Institut für Weltraumforschung, Graz
  • Imperial College, London
  • Max-Planck-Institut für Sonnensystemforschung, Katlenburg-Lindau
  • Max-Planck-Institut für extraterrestrische Physik, Garching
Rosettas Mars swing-by

On Sunday, 25th february 2007, Rosetta flew by Mars performing a gravityt assist manoeuvre. Rosetta passed by the red planet's surface in a distance of some hundred kilometers. This close approach was a good opportunity to switch on the lander experiment ROMAP in order to calibrate its magnetometer. Additionally, the data set taken during the flyby provides an insight into the plasma environment around Mars.

 

Magnetfeld des Mars, gemessen während des Rosetta Vorbeiflugs im Februar 2007
Magnetic Field measured by ROMAP during Mars flyby.

All components of ROMAP worked satisfyingly during the flyby. In the magnetogramm plotted above, one can follow Rosettas itinerary around Mars: its approach through the solar wind and the crossing of the bowshock and he tail.

See also ESA article about Rosettas flyby.

 

Links

  • ESA - Rosetta
  • ESA Science & Technology
  • DLR - Rosetta

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