Variation of the Mn I 539.4 nm line with the solar cycle
- S. Danilovic
- S. K. Solanki
- W. Livingston
- N. Krivova
- I. Vince
DOIAbstract
Context. As a part of the long-term program at Kitt Peak National Observatory (KPNO), the Mn
Context. As a part of the long-term program at Kitt Peak National Observatory (KPNO), the Mn
Sunspots are a canonical marker of the Sun’s internal magnetic field which flips polarity every ∼22-...
The next generation of solar observatories aim to understand the magnetism of the solar chromosphere...
The Sun has a polar magnetic field which oscillates with the 11 yr sunspot cycle. This polar magneti...
We observed the MnI 539.47 nm and 542.04nm line profiles in the quiet photosphere and plage regions ...
Abstract. On the basis of NLTE profile calculations obtained by employing the radiative transfer cod...
The equivalent width and central depth data of Mn 539.4 nm solar spectral line, observed in the peri...
Abstract. The Mn I 5394.7 A ̊ line is the only spectral line originating in the solar photosphere fo...
We present a solution for the long standing problem concerning the "chromospheric"behaviour of the ...
There is a long-standing debate why the Mn i 5394.7 Å line in the solar irradiance spectrum brighten...
CCD observations of the MnI 539.47 nm spectral line in the solar flux made at the Astronomical Obser...
Context.We present a detailed NLTE analysis of 39 $\ion{Mn}{i}$ lines in the solar spectrum. The inf...
We present composite time series of Ca II H & K line core emission indices of up to 50 years in leng...
There is a long-standing debate why the Mn i 5394.7 Å line in the solar irradiance spectrum brighten...
The Sun has a steady 11-year cycle in magnetic activity most well-known by the rising and falling in...
Context. The solar brightness varies on timescales from minutes to decades. A clear identification o...
Sunspots are a canonical marker of the Sun’s internal magnetic field which flips polarity every ∼22-...
The next generation of solar observatories aim to understand the magnetism of the solar chromosphere...
The Sun has a polar magnetic field which oscillates with the 11 yr sunspot cycle. This polar magneti...
We observed the MnI 539.47 nm and 542.04nm line profiles in the quiet photosphere and plage regions ...
Abstract. On the basis of NLTE profile calculations obtained by employing the radiative transfer cod...
The equivalent width and central depth data of Mn 539.4 nm solar spectral line, observed in the peri...
Abstract. The Mn I 5394.7 A ̊ line is the only spectral line originating in the solar photosphere fo...
We present a solution for the long standing problem concerning the "chromospheric"behaviour of the ...
There is a long-standing debate why the Mn i 5394.7 Å line in the solar irradiance spectrum brighten...
CCD observations of the MnI 539.47 nm spectral line in the solar flux made at the Astronomical Obser...
Context.We present a detailed NLTE analysis of 39 $\ion{Mn}{i}$ lines in the solar spectrum. The inf...
We present composite time series of Ca II H & K line core emission indices of up to 50 years in leng...
There is a long-standing debate why the Mn i 5394.7 Å line in the solar irradiance spectrum brighten...
The Sun has a steady 11-year cycle in magnetic activity most well-known by the rising and falling in...
Context. The solar brightness varies on timescales from minutes to decades. A clear identification o...
Sunspots are a canonical marker of the Sun’s internal magnetic field which flips polarity every ∼22-...
The next generation of solar observatories aim to understand the magnetism of the solar chromosphere...
The Sun has a polar magnetic field which oscillates with the 11 yr sunspot cycle. This polar magneti...
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