Leitung
Prof. Dr. rer. nat. Alfred Krabbe

Assistenz
Barbara Klett

Geschäftsleitung
Dr.-Ing. Thomas Keilig

Deputy SMO Director (Kalifornien)
Dr. rer. nat Bernhard Schulz

Standortleiter AFRC & SOFIA Teleskop Manager
Dipl.-Ing. Michael Hütwohl

Standortleiter ARC & und Facility Scientist
Dr. rer. nat. Jürgen Wolf

Technology Advisor
Prof. Dr.-Ing. Jörg Wagner

Bildungs- und Öffentlichkeitsarbeit
Dr. rer. nat. Dörte Mehlert


Deutsches SOFIA Institut
Pfaffenwaldring 29
70569 Stuttgart

Tel. +49 (0)711/685-62379
Fax +49 (0)711/685-63596
 

Deutsches SOFIA Institut

 Vom 15. - 20. September 2019 wird SOFIA am Stuttgarter Flughafen zu Besuch sein!

 

News

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Instrument from University of Stuttgart Provides Surprising Insights into the Companion of the Whirlpool Galaxy

April 3, 2019

ApJL Focus Issue published on Scientific Results of the Airborne Infrared Observatory SOFIA

Young, hot stars heat up their environment and thus also their birthplace itself. For more stars to form, this excess heat energy must be dissipated. Astronomers now know how this cooling works: So, for instance, the UV radiation of the young, hot stars ionizes the available neutral carbon - so one electron of each carbon atom is released - and in addition transferring it into an excited, so-called fine structure state through collisions. Subsequently, the energy supplied by this process is removed very efficiently by emission via the so-called fine-structure line [CII] at 158 μm. Thus, the strength of the [CII] 158 μm line is a direct measure of the energy or the number of young, hot stars, and thus the star formation rate in an area.

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Eine außergewöhnliche Lehrerfortbildung in der Stratosphäre

February 28, 2019

Abenteuer pur – „Spontanitätstest“ bestanden

Olaf Graf (Schulsternwarte "Sigmund Jähn" Rodewisch, SN), Joachim Groß (Graf-Eberhard-Gymnasium, Bad Urach, BW), Margarita Riedel (Keplergesellschaft Weil der Stadt, BW) und Andrea Sittig-Kramer (Drawehn-Schule, Clenze, NI) sind bereits am 17. Februar nach Kalifornien gereist und sollten am Mittwoch, 20. Februar ihren ersten Mitflug an Bord der fliegender Sternwarte SOFIA (Stratosphären Observatorium Für Infrarot Astronomie) haben. Doch erstens kam es anders und zweitens als gedacht.

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MIT - "Global Seed Fund" Promotes DSI Junior Scientists

February 11, 2019

Karsten Schindler and scientists at MIT jointly explore the edge of our solar system

The "Global Seed Fund" of the Massachusetts Institute of Technology (MIT) funds ambitious young researchers at the University of Stuttgart to kick-start their research projects. In addition, it aims at strengthening the research partnership between MIT and University of Stuttgart. Karsten Schindler of the German SOFIA Institute (DSI) successfully proposed his project "A peek into the outer solar system through stellar occultations" in the last call for proposals, which has been awarded $24,200.

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The GENESIS Project S106 - on the Trail of the Formation of Massive Stars

December 3, 2018

How exactly do massive stars form in our Milky Way? Dr. Nicola Schneider from the University of Cologne and her international team pursues this question in the GENESIS project S106 by combining observations with SOFIA, the Stratospheric Observatory for Infrared Astronomy, with data from other observatories. These sort of studies are the main objectives of GENESIS, a German-French collaborative project between N. Schneider, R. Simon from the I. Physik. Institut, Cologne and S. Bontemps from the Laboratoire d’Astrophysique of Bordeaux. All stars, even ordinary ones like our Sun, are formed by interstellar gas and dust clouds. These clouds show a complex structure with filaments and clumps. The mass flow along the filaments ends in an accretion disk around the proto star. This disk gradually collects the surrounding matter and finally the star is formed inside. Triggered by this process additionally ionized gas is ejected perpendicular to the disk in so-called jets. In a low-mass star, these processes occur comparatively ordered in clearly distinguishable phases and altogether last about one million years. If the pressure inside the proto star is high enough, the hydrogen burning (the fusion of hydrogen nuclei to helium) is ignited - the new star is born.

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