The Sun - SOS Playlist


Note  This playlist is currently under development by DMNS staff.

Sun_Solar_Dynamics_Observatory_-_20100801.jpgSun Playlist Training Information
The Sun.ppt
The Sun Playlist Companion Document

SOS User Group Meeting with Mark Miesch (video)

Slideshow used during Mark's User Group Lecture
Miesch Stellar Mag_Pt1.pdf
Miesch Stellar Mag_Pt2.pdf

nasa_stereo.jpgSTEREO/SDO Sun Observations (real time)

In this real-time dataset, imagery from the satellites named "STEREO Ahead" and "STEREO Behind" are morphed together to provide near full coverage of the sun. The images for this dataset were taken with the EUVI telescope in the extreme ultraviolet wavelength. In order to keep all of the various wavelengths straight, scientists color the different wavelengths. The 195A wavelength used here is arbitrarily colored green. In this wavelength, the brighter areas are hotter and the darker areas are cooler.

(Dataset 277 -

CaseF_Vr.pngCaseF_Vr - A Peek into the Turbulent Solar Interior

Convection near the surface of the Sun occurs when hot plasma rises and cooler, denser plasma sinks. Convection also takes place far beneath the Sun's surface, where scientists suspect there are churning masses of plasma up to 10 times larger than the size of Earth. These masses, known as giant cells, may hold the key to the movement of sunspots and the behavior of solar storms, which can buffet Earth's atmosphere and affect satellites as well as power and communications systems.
The simulations indicate that, at low solar latitudes, cooler and denser plasma sinks along north-south corridors, with the corridors moving eastward relative to hotter plasma that rises. But at higher latitudes, rising and falling areas of plasma meet and create solar cyclones that last for several days.
The model also can help scientists understand how giant cells induce a global circulation. The circulation, acting like a conveyor belt, moves plasma from the solar equator toward the poles just beneath the surface of the Sun and then back toward the equator at a greater depth. This circulation, working with convection and rotation, generates and organizes magnetic fields, giving rise to patterns of magnetic activity such as the 11-year sunspot cycle.

Dataset: Solar magnetism animation (CaseF-VR)

Introduction to images below
bilby1_Br, bilby1_Vr, bilby1_Bphi  - Vibrant Magnetism in a Young Sun
Stars like the Sun bristle with magnetic energy. Solar and stellar obervations reveal diverse and vibrant manifestations of magnetic activity, including the dramatic eruptions known as flares and coronal mass ejections. Yet, understanding the origins of solar and stellar magnetism is a formidable task, requiring the use of sophisticated supercomputer simulations. These movies show one such simulation of a star like the Sun but younger, and spinning five times faster.

Additional info on the "bilby" movies can be found here: 
Tying the Sun Together
There's a Little Black Spot on the Sun Today

Bibly1-Br.png1) bilby1_Br

The first movie of the sequence shows the vertical magnetic field at the stellar surface; red is where the magnetic field is poking out and blue is where it's poking in. Notice that the polar field changes direction as the movie proceeds; this simulated star has a magnetic cycle much like the Sun!

Solar magnetism animation (Bilby1-Br)

Bibly1_Vr.png2) bilby1_Vr

The second movie shows the convection that is responsible for the magnetism; swirling columns of plasma that wrap up and amplify magnetic fields (yellow is plasma flowing up, blue/black is plasma flowing down).

Solar magnetism animation (Bilby1-Vr)

Bibly1-Bphi.png3) bilby1_Bphi

The third and final movie of the sequence shows the horizontal magnetic field (blue is westward, red eastward) deep below the surface where telescopes can't see.

Solar magnetism animation (Bilby1-Bphi)

Related Resources
Space Weather Media Viewer - real-time
Space Weather


Further information on "Case F" can be found here:
Sun's Deep Interior Revealed by New Computer Model
Long-Term Solar Variability (LSV)




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