Download - Presented by: Kyle Thompson and Ginny Connor
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Presented by:Kyle Thompson and Ginny Connor
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The abundance of M Dwarfs
A solar flare’s impact on atmospheric ozone
Two distinct tests With charged
particles With uncharged (UV
radiation only) particles
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Abundant Long living 70% of all stars in
our galaxy Infrared radiation Low luminosity
stars Closer habitable
zone
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Charged particles vs. uncharged (UV radiation only) particles
Ionizing particles emitted during a flare may be more dangerous depending on how much of the particle flux strikes the planet
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No significant temperature change for either test
Final temperature difference was 0.1 K
Greatest difference was observed in the Mesosphere
Ozone variations cause temperature fluctuations in the upper atmosphere, but these fluctuations are small, and the climate at the surface is unaffected
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Depleted in the Stratosphere
30 ppmv – 0.3 ppmv
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Noticeable decrease in the Stratosphere during the impulsive phase
Continued to increase until the flare ended
Much of the potentially life-damaging UV radiation goes into photolyzing ozone in the Stratosphere, which prevents it from reaching the planetary surface
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UV radiation only: 1,000 seconds after the flare, depletion was only 1%
With charged photons: large effect but stabilizes after 4 months
Given that M Dwarfs can be active on timescales of days to weeks, the atmosphere may not return to equilibrium before another flare occurs
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For an oxygen-rich, Earth-like planet in the habitable zone of an active M Dwarf, stellar flares do not necessarily affect habitability
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Segura, Antigona, Lucianne M. Walkowicz, Victoria Meadows, James Kasting, and Suzanne Hawley. "The Effect of a Strong Stellar Flare on the Atmospheric Chemistry of an Earth-like Planet Orbiting an M Dwarf." Astrobiology 10.7 (2010): 751-71. Web.