Sonnenaktivitäten Live

This channel highlights the outer atmosphere of the Sun – called the corona – as well as hot flare plasma. Hot active regions, solar flares, and coronal mass ejections will appear bright here. The dark areas – called coronal holes – are places where very little radiation is emitted, yet are the main source of solar wind particles.

Where: Corona and hot flare plasma
Wavelength: 193 angstroms (0.0000000193 m) = Extreme Ultraviolet
Primary ions seen: 11 times ionized iron (Fe XII)
Characteristic temperature: 1.25 million K (2.25 million F)

Corona and hot flare plasma last 48 hr

This channel is especially good at showing coronal loops – the arcs extending off of the Sun where plasma moves along magnetic field lines. The brightest spots seen here are locations where the magnetic field near the surface is exceptionally strong.

Where: Quiet corona and upper transition region
Wavelength: 171 angstroms (0.0000000171 m) = Extreme Ultraviolet
Primary ions seen: 8 times ionized iron (Fe IX)
Characteristic temperature: 1 million K (1.8 million F)

Quiet corona and upper transition region last 48 hr

https://sdo.gsfc.nasa.gov/assets/img/latest/latest_1024_HMIIF.jpgThis channel is especially good at showing coronal loops – the arcs extending off of the Sun where plasma moves along magnetic field lines. The brightest spots seen here are locations where the magnetic field near the surface is exceptionally strong.

Where: Quiet corona and upper transition region
Wavelength: 171 angstroms (0.0000000171 m) = Extreme Ultraviolet
Primary ions seen: 8 times ionized iron (Fe IX)
Characteristic temperature: 1 million K (1.8 million F)

Quiet corona and upper transition region last 48 hr

HMI Intensitygram – Flattened

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