MPS contributions to Metis

MPS provides the two detector assemblies forming the Metis Detection Subsystem.

Contact

Dr. Luca Teriaca
Dr. Luca Teriaca
Phone:+49 551 384979-453

Metis team at MPS

Scientists:
Sami K. Solanki (Co-I)
Luca Teriaca (Co-PI)
Udo Schuehle (Co-I)
Regina Aznar Cuadrado
Hardi Peter (Co-I)
Joachim Woch (Co-I)

Engineers and Technicians:                   
Miguel Alvarez Copano
Bernd Chares
Rainer Enge   
German Fernandez Rico          
Klaus Heerlein         
Martin Kolleck         
Tanja Macke
Thimo Meierdierks           
Stefan Meining       
Sabrina Meyer
Reinhard Mueller   
Ioanna Papagiannaki            
Sandeep Ramanath                              
Michael Sperling     
Jan Staub                  
Stephan Werner                    
Andreas Zerr

Metis

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The Metis Coronagraph

A coronal imager for the Solar-Orbiter mission

The Metis instrument is an inverted-occultation coronagraph part of the Solar Orbiter payload. The instrument flight model has been integrated on the spacecraft and it is undergoing testing at spacecraft level. It will study the structure and dynamics of the solar corona with unprecedented temporal and spatial resolution at different heights over the ecliptic plane. The instrument is crucial to the Solar Orbiter mission as it provides the needed link between the solar atmosphere and the inner heliosphere.

Metis will image the solar corona between 1.5 and 3 solar radii in two different wavelengths, visible light between 580 and 640 nm, and the Lyman-alpha line of hydrogen (H I 121.6 nm) by a combination of broad-band coatings (Al-MgF2) on the mirrors and spectral bandpass filters. The visible channel also includes a polarimeter assembly to observe the linearly polarized component of the K corona.

<em><em>Schematic layout of the optical unit of the Metis inverted occultation coronagraph. <em><em>The visible light channel (visible detector and polarimeter) is fed by the 12° tilted interference filter.</em></em><br /></em></em> Zoom Image
Schematic layout of the optical unit of the Metis inverted occultation coronagraph. The visible light channel (visible detector and polarimeter) is fed by the 12° tilted interference filter.

The Metis Flight Model at Opsys calibration facility at ALTEC, Turin. Zoom Image
The Metis Flight Model at Opsys calibration facility at ALTEC, Turin.

Narrow band imaging in Lyman alpha will allow the determination of the outflow speed of protons. Simultaneous images in linearly polarized and un-polarized white-light will provide information about the electron density in the corona. This will be crucial for understanding solar wind acceleration processes and will put strong constraints on related theories.

MPS provides the Visible Light Detector Assembly (VLDA) and the UltraViolet Detector Assembly (UVDA) that form the Metis Detection Subsystem (MDS). The MDS also includes service units such as the High Voltage Unit (HVU) serving the Ultraviolet detector (intensified APS), the Camera Power Converter (CPC) serving both assemblies, and brackets handling electrical interfaces.

The Flight Models of the Metis MDS at delivery in the Opsys facility in ALTEC, Turin. Zoom Image
The Flight Models of the Metis MDS at delivery in the Opsys facility in ALTEC, Turin.
 
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