OSO 8 observations of wave propagation in the solar chromosphere and transition region

1978 ◽  
Vol 224 ◽  
pp. 671 ◽  
Author(s):  
E. G. Chipman
Keyword(s):  
Wave Propagation ◽  
Transition Region ◽  
Solar Chromosphere

scholarly journals Experiment to Determine the Temperature Structure in the Solar Chromosphere and Corona

1972 ◽  
Vol 14 ◽  
pp. 668-669
Author(s):  
C. R. Negus
Keyword(s):  
Transition Region ◽  
Extreme Ultraviolet ◽  
Normal Incidence ◽  
Research Unit ◽  
Emission Lines ◽  
Solar Chromosphere ◽  
Temperature Structure ◽  
Ultraviolet Emission ◽  
Ionization Temperature ◽  
Intensity Ratios

An experiment is in course of preparation at the Astrophysics Research Unit at Culham for flight on a Sun-pointing rocket. It is designed to determine the ionization temperature and electron density as a function of height in the temperature range of about 8 × 104 K to 3 × 106 K by measuring limb to disk intensity ratios of extreme ultraviolet emission lines in the 170 to 850 Å region. The work is an extension of current experiments in which normal-incidence spectrographs are used to determine the structure lower in the chromosphere-corona transition region.

Plasma flows in the quiet solar chromosphere-corona transition region

2015 ◽  
Vol 70 (2) ◽  
pp. 153-159 ◽  
Author(s):  
O. V. Dunin-Barkovskaya ◽  
B. V. Somov
Keyword(s):  
Transition Region ◽  
Solar Chromosphere ◽  
Plasma Flows

scholarly journals Characterization of shock wave signatures at millimetre wavelengths from Bifrost simulations

2020 ◽  
Vol 379 (2190) ◽  
pp. 20200185 ◽  
Author(s):  
Henrik Eklund ◽  
Sven Wedemeyer ◽  
Ben Snow ◽  
David B. Jess ◽  
Shahin Jafarzadeh ◽  
...  
Keyword(s):  
Shock Wave ◽  
Wave Propagation ◽  
Brightness Temperature ◽  
Spectral Band ◽  
Three Dimensional ◽  
Strong Shock ◽  
Shock Wave Propagation ◽  
Small Scale ◽  
Solar Chromosphere ◽  
Brightness Temperatures

Observations at millimetre wavelengths provide a valuable tool to study the small-scale dynamics in the solar chromosphere. We evaluate the physical conditions of the atmosphere in the presence of a propagating shock wave and link that to the observable signatures in mm-wavelength radiation, providing valuable insights into the underlying physics of mm-wavelength observations. A realistic numerical simulation from the three-dimensional radiative magnetohydrodynamic code Bifrost is used to interpret changes in the atmosphere caused by shock wave propagation. High-cadence (1 s) time series of brightness temperature ( T b ) maps are calculated with the Advanced Radiative Transfer code at the wavelengths 1.309 mm and 1.204 mm, which represents opposite sides of spectral band 6 of the Atacama Large Millimeter/submillimeter Array (ALMA). An example of shock wave propagation is presented. The brightness temperatures show a strong shock wave signature with large variation in formation height between approximately 0.7 and 1.4 Mm. The results demonstrate that millimetre brightness temperatures efficiently track upwardly propagating shock waves in the middle chromosphere. In addition, we show that the gradient of the brightness temperature between wavelengths within ALMA band 6 can potentially be used as a diagnostics tool in understanding the small-scale dynamics at the sampled layers. This article is part of the Theo Murphy meeting issue ‘High-resolution wave dynamics in the lower solar atmosphere’.

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