TY - JOUR

T1 - On the relation between photospheric magnetic field and chromospheric emis-sion in the quiet Sun

AU - Loukitcheva, M.A.

AU - Solanki, S.K.

AU - White, S.

N1 - Loukitcheva, M., Solanki, S., & White, S. (2008). On the relation between photospheric magnetic field and chromospheric emission in the quiet Sun. Proceedings of the International Astronomical Union, 4(S259), 185-190. doi:10.1017/S1743921309030439

PY - 2009

Y1 - 2009

N2 - In this contribution we present an observational study of the interaction of the photosphere with different chromospheric layers. We study the correlations between emissions at varying temperature from the temperature minimum region (UV continuum at 1600 Å from TRACE) through the low chromosphere (CaII K-line from BBSO) to the middle chromosphere (continuum at 3.5 mm from BIMA) and photospheric magnetic field from MDI/SOHO. For the first time millimeter observational data are included in such analysis. We report a high degree of correlation between considered emissions formed at different heights in the chromosphere. A power law is found to be a good representation for the relationship between photospheric magnetic field and chromospheric emissions at all considered wavelengths. Our analysis shows that the dependence of chromospheric intensities on magnetic field is different for the network and internetwork regions. In the network a power law provides the best fit with the exponent being close to 0.5-0.6, w

AB - In this contribution we present an observational study of the interaction of the photosphere with different chromospheric layers. We study the correlations between emissions at varying temperature from the temperature minimum region (UV continuum at 1600 Å from TRACE) through the low chromosphere (CaII K-line from BBSO) to the middle chromosphere (continuum at 3.5 mm from BIMA) and photospheric magnetic field from MDI/SOHO. For the first time millimeter observational data are included in such analysis. We report a high degree of correlation between considered emissions formed at different heights in the chromosphere. A power law is found to be a good representation for the relationship between photospheric magnetic field and chromospheric emissions at all considered wavelengths. Our analysis shows that the dependence of chromospheric intensities on magnetic field is different for the network and internetwork regions. In the network a power law provides the best fit with the exponent being close to 0.5-0.6, w

KW - Sun: magnetic fields

KW - Sun: chromosphere

KW - Sun: radio radiation

KW - Sun: photosphere

U2 - http://dx.doi.org/10.1017/S1743921309030439

DO - http://dx.doi.org/10.1017/S1743921309030439

M3 - Article

VL - 4

SP - 185

EP - 190

JO - Proceedings of the International Astronomical Union

JF - Proceedings of the International Astronomical Union

SN - 1743-9213

IS - S259

ER -