Sun ID: 4164

A Multi-Mission View of a Solar Flare: Optical to Gamma-rays

Visualizations by Tom Bridgman Released on May 7, 2014

To improve our understanding of complex phenomena such as solar flares, a wide variety of tools are needed. In the case of astronomy, those tools enable us to analyze the light in many different wavelengths and many different ways.

Many different instruments are observing the Sun almost continuously, both from space and on the surface of the Earth. On March 29, 2014, the Dunn Solar Telescope at Sacramento Peak, New Mexico was observing a solar active region and requested other observatories to watch as well. As a result of this coordination, the region was being observed by a large number of different instruments, ground and space-based, when it subsequently erupted with an X-class flare.

This visualization presents various combinations of the datasets collected during this effort. The color text represents the dominant color of the dataset in the imagery.

Solar Dynamics Observatory (SDO): HMI (617.1nm). This data represents the Sun is visible light similar to how we see it from the ground.

Solar Dynamics Observatory (SDO): AIA (17.1nm). Solar ultraviolet emission, which can only be seen from space, reveals plasma flowing, and escaping, along magnetic fields.

IRIS Slit-Jaw Imager: 140.0nm. This high-resolution imager also contains a slit (the dark vertical line in the center of the field) which directs the light to an ultraviolet spectrometer which is used to extract even more information about the light. The imager slews back-and-forth across the region, providing spectra over a larger area of the Sun.

Hinode/X-ray Telescope: x-ray band. Indicates very hot plasma.

RHESSI: 50-100 keV. High-energy gamma-ray emission. Emission from these locations represent the very highest energy photons from the flare event.

Dunn Solar Telescope: G-band filter. This filter, showing much of the solar surface (photosphere) in visible light, provides a detailed view of the sunspots and convection cells. The view moves because the instrument was repointed several times during the observation.

Dunn Solar Telescope: IBIS ( Hydrogen alpha, 656.3nm; Calcium 854.2 nm; Iron 630.15nm). This is the small rectangular view within the Dunn Solar Telescope G-band view. This instrument can tune the wavelength during the observation, which provides views of the solar atmosphere at different depths.

Visualization Credits

Tom Bridgman (Global Science and Technology, Inc.): Lead Animator
Genna Duberstein (USRA): Producer
William D. Pesnell (NASA/GSFC): Scientist
Lucia Kleint (BAER Institute): Scientist
Albert Shih (NASA/GSFC): Scientist
Adrian Daw (NASA/GSFC): Scientist
Laurence Schuler (ADNET Systems, Inc.): Project Support
Ian Jones (ADNET Systems, Inc.): Project Support

Please give credit for this item to:
NASA's Scientific Visualization Studio, the SDO Science Team, the Virtual Solar Observatory and the BAER Institute.

Short URL to share this page:
https://svs.gsfc.nasa.gov/4164

Missions:
IRIS: Interface Region Imaging Spectrograph
RHESSI
SDO

Data Used:

Sacramento Peak Observatory/NSO

Observed Data - National Solar Observatory

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SDO/HMI/Continuum also referred to as: SDO Continuum

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RHESSI/X-ray Imaging Spectrometer

The RHESSI instrument is an imaging spectrometer observing the Sun at X-ray to gamma-rays (photon energies of 3 keV to 17 MeV) at time resolutions of a few seconds. (eV stands for "electron volt" and is a unit of energy. Note that photons of visible light have energies of 2-3 eV. 1 keV is a thousand electron volts and 1 MeV is a million electron volts.

http://hesperia.gsfc.nasa.gov/hessi/

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