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Prof. Dr. Beate Stelzer, Universität Tübingen
Hot side up: The outer atmospheres of cool stars
Veranstaltungsart: Physikalisches Kolloquium
Zeit: 03.07.2017, 17:15 - 18:30 Uhr
Ort: HS 1 Abbeanum, Fröbelstieg 1
Veranstalter: Physikalisch-Astronomische Fakultät


Max-Wien-Platz 1

07743 Jena

Tel. 03641 9-47001


The outer atmospheres of low-mass stars are heated by the stellar magnetic field. While the chromosphere is marked by optical emission lines, the corona – which constitutes the atmospheric layer with the highest temperature (~ 10MK) – is dominated by emission in ultraviolet (UV), X-ray and radio bands. The radiation from these hot parts of the stellar atmosphere is collectively termed `magnetic activity'. Evidently, the observational characterization of magnetic activity requires a multi-wavelength approach. The direct aim of such studies is to understand the influence of the magnetic field on the radiative output of the star, i.e. to analyse how the stellar dynamo works and what are its dependencies on stellar parameters such as mass, effective temperature, age and rotation. Besides this, in particular the radiation emitted at high energies (UV and X-rays) is crucial for the star formation process (e.g., the composition of meteorites, the evolution of circumstellar disks and the star formation rate) and for the formation and evolution of planets around the star (e.g., evaporation and effects on chemical composition of the planet atmosphere). I review our current knowledge on the dynamic outer atmospheres of (photospherically) cool stars and the crucial role of their emissions on their environment. 

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