| SSL Home | Solar Physics Home | NASA Home |
header bar

Multi-Spectral Solar Telescope Array

THE SUN 

Why We Study the Sun 
The Big Questions 
Magnetism - The Key 

SOLAR STRUCTURE 

The Interior 
The Photosphere 
The Chromosphere 
The Transition Region 
The Corona 
The Solar Wind 
The Heliosphere 

SOLAR FEATURES 

Photospheric Features 
Chromospheric Features 
Coronal Features 
Solar Wind Features 

THE SUN IN ACTION 

The Sunspot Cycle 
Solar Flares 
Post Flare Loops 
Coronal Mass Ejections 
Surface and Interior Flows 
Waves and Helioseismology 

RESEARCH AREAS 

Flare Mechanisms 
3D Magnetic Fields 
The Solar Dynamo 
Sunspot Cycle Predictions 
Coronal Heating 
Solar Wind Dynamics 

PREVIOUS PROJECTS 

The Skylab Mission 
The Solar Maximum Mission 
The SpaceLab 2 Mission 
MSSTA 

CURRENT PROJECTS 

MSFC TVM  
MSFC EXVM  
The Yohkoh Mission 
The Ulysses Mission 
The SOHO Mission 
The GONG Project 
The Sun in Time (EPO) 

FUTURE PROJECTS 

The Solar B Mission 
The GOES SXI Instruments 
Interstellar Probe  

Click on image for larger version.

The Multi-Spectral Solar Telescope Array, MSSTA (128 kb GIF image), is a telescope array consisting of at least fifteen different telescopes designed to observe the Sun in ultraviolet and soft x-rays. The project is part of a joint effort between Richard Hoover at MSFC and Art B. C. Walker at Stanford University. Each telescope in the array consists of mirrored optics coated with multilayers to allow for reflection at a selected wavelength. Pre-filters are used to exclude unwanted emissions so that each telescope obtains images at its prescribed wavelength.

MSSTA's first flight was on May 13th, 1991 at 19:03 UT. The payload was launched from White Sands Missile Range atop a Terrier Black Brant IX (283 kb GIF image). The telescopes were carried to an altitude of 230 km and remained out of the lower atmosphere for approximately 6 minutes. During this time photographs were taken of the Sun and its outer atmospheric layers, the chromosphere and corona.

Images obtained with MSSTA span the wavelength range from Lyman-Alpha emission at 1216 Å to a Si XII emission line at 44 Å. Among these images are:

H I 1216 Å (152 kB GIF image) Temperature = 20,000 K
He II 304 Å (134 kB GIF image) Temperature = 80,000 K
Fe XII 193 Å (88 kB GIF image) Temperature = 1,500,000 K
Fe XIV 211 Å (81 kB GIF image) Temperature = 1,800,000 K
Si XII 44 Å (94 kB GIF image) Temperature = 2,000,000 K

Ground-based images taken at nearly the same time were acquired from the Big Bear Solar Observatory (BBSO) and the National Solar Observatory (NSO). These images include:

BBSO White Light (141 kB GIF image) Temperature = 6,000 K
BBSO H I 6563 Å (76 kB GIF image) Temperature = 10,000 K
BBSO Ca II 3934 Å (79 kB GIF image) Temperature = 10,000 K
NSO Magnetogram (64 kB GIF image)

Analysis of these images is in progress. These analyses will help to determine temperatures and densities in the observed coronal structures and provide information on magnetic connections between them.

A reflight of the MSSTA payload with several new instruments took place on November 3rd, 1994.

Web Links


 

Author: David H. Hathaway, david.hathaway@msfc.nasa.gov, (256) 544-7610
Mail Code SD50, NASA/Marshall Space Flight Center, Huntsville, AL 35812

 

Responsible Official: John M. Davis, john.m.davis@msfc.nasa.gov, (256) 544-7600
Mail Code SD50, NASA/Marshall Space Flight Center, Huntsville, AL 35812

 

Last revised 2000 January 07 - D. H. Hathaway