Multi-Wavelength Eclipse Observations of a Quiescent Prominence Multi-Wavelength Eclipse Observations of a Quiescent Prominence Multi-Wavelength Eclipse Observations of a Quiescent Prominence

Multi-Wavelength Eclipse Observations of a Quiescent Prominence Multi-Wavelength Eclipse Observations of a Quiescent Prominence Multi-Wavelength Eclipse Observations of a Quiescent Prominence

Článek WoS

We construct the maps of temperatures, geometrical thicknesses, electron densities and gas pressures in a quiescent prominence. For this we use the RGB signal of the prominence visible-light emission detected during the total solar eclipse of 1 August 2008 in Mongolia and quasi-simultaneous H alpha spectra taken at OndA (TM) ejov Observatory. The method of disentangling the electron density and geometrical (effective) thickness was described by Jeji and Heinzel (Solar Phys. 254, 89 -aEuro parts per thousand 100, 2009) and is used here for the first time to analyse the spatial variations of prominence parameters. For the studied prominence we obtained the following range of parameters: temperature 6000 -aEuro parts per thousand 15 000 K, effective thickness 200 -aEuro parts per thousand 15000 km, electron density 5x10(9) -aEuro parts per thousand 10(11) cm(-3) and gas pressure 0.02 -aEuro parts per thousand 0.2 dyn cm(-2) (assuming a fixed ionisation degree n (p)/n (H)=0.5). The electron density increases towards the bottom of the prominence, which we explain by an enhanced photoionisation due to the incident solar radiation. To confirm this, we construct a two-dimensional radiative-transfer model with realistic prominence illumination.

We construct the maps of temperatures, geometrical thicknesses, electron densities and gas pressures in a quiescent prominence. For this we use the RGB signal of the prominence visible-light emission detected during the total solar eclipse of 1 August 2008 in Mongolia and quasi-simultaneous H alpha spectra taken at OndA (TM) ejov Observatory. The method of disentangling the electron density and geometrical (effective) thickness was described by Jeji and Heinzel (Solar Phys. 254, 89 -aEuro parts per thousand 100, 2009) and is used here for the first time to analyse the spatial variations of prominence parameters. For the studied prominence we obtained the following range of parameters: temperature 6000 -aEuro parts per thousand 15 000 K, effective thickness 200 -aEuro parts per thousand 15000 km, electron density 5x10(9) -aEuro parts per thousand 10(11) cm(-3) and gas pressure 0.02 -aEuro parts per thousand 0.2 dyn cm(-2) (assuming a fixed ionisation degree n (p)/n (H)=0.5). The electron density increases towards the bottom of the prominence, which we explain by an enhanced photoionisation due to the incident solar radiation. To confirm this, we construct a two-dimensional radiative-transfer model with realistic prominence illumination.

Sun, prominence

Sun, prominence

JEJCIC, S.; PETR HEINZEL, P.; ZAPIOR, M.; DRUCKMÜLLER, M.; STANISLAV, G.; KOTRČ, P.

2015

01.07.2014

0038-0938

SOLAR PHYSICS

2014 (289)

7

Nizozemsko

2487

2501

14