SPATIAL AND TEMPORAL VARIATIONS OF K CA II LINE PROFILE SHAPES IN DIFFERENT STRUCTURES OF THE SOLAR CHROMOSPHERE. II. DETERMINATION TECHNIQUE AND CORRELATION RELATIONSHIPS BETWEEN THE K CA II LINE PARAMETERS FOR K₁ AND K₂ FEATURES

Journal Title: Solar-Terrestrial Physics - Year 2020, Vol 6, Issue 4

Abstract

We have studied two regions located at the base of a coronal hole. For the K₁ intensity minima and K₂ peaks, which form between the upper photosphere and the lower chromosphere and in the lower chromosphere respectively, a number of Ca II line parameters have been computed. We have improved the determination technique for ∆λᴋ₁ᵥ and ∆λᴋ₁ᵣ, ∆λᴋ₂ᵥ and ∆λᴋ₂ᵣ line profile shifts, including certain cases when their direct determination was complicated. We have determined Iᴋ₁ᵥ, Iᴋ₁ᵣ, Iᴋ₂ᵥ, Iᴋ₂ᵣ intensities, K₁ minima and K₂ peaks separations SEPᴋ₁ = ∆λᴋ₁ᵣ – ∆λᴋ₁ᵥ, SEPᴋ₂ = ∆λᴋ₂ᵣ – ∆λᴋ₂ᵥ, respectively. We have constructed scatter plots and have computed correlation relationships between parameters relating to different levels of atmosphere. We have obtained the following results. The intensities observed in the lower and middle chromosphere are connected closer than intensities related to the upper photosphere and middle chromosphere. The structures with a stronger magnetic field are brighter at the upper photosphere and lower chromosphere levels as compared to the structures with a weaker magnetic field. K₁ minima separations are of greater value for the structures with a stronger magnetic field relative to the structures with a weaker magnetic field, whereas K₂ peaks separations demonstrate the opposite behavior. They are lower for the structures with a stronger magnetic field. It is true not only for the chosen structures belonging to quiet regions but also for the plage, though we need additional statistics for plages. The relation between shifts of K₁ minima and K₂ peak intensities for violet and red wings appeared to be weak. This may be due to the considerable contribution of random movements to the velocity field at the upper photosphere and lower chromosphere levels or due to different forming levels for the profile violet and red wings.

Authors and Affiliations

Turova I. P. , Grigoryeva S. A. , Ozhogina O. A.

Keywords

Related Articles

DIAMAGNETIC STRUCTURES AS A BASIS OF QUASI-STATIONARY SLOW SOLAR WIND

The results presented in this review reflect the fundamentals of the modern understanding of the nature of the structure of the slow solar wind (SW) along the entire length from the Sun to the Earth's orbit. It is known...

OBSERVING THE NEUTRON COMPONENT DURING THUNDERSTORM ACTIVITY AT A MOUNTAIN CR STATION

During three summer months in 2015, the Cosmic Ray (CR) station Irkutsk-3000, located at 3000 m above sea level, measured the CR neutron component intensity with the 6NM64 neutron monitor, as well as the atmospheric elec...

RETROSPECTIVE ANALYSIS OF LONG-TERM REGIONAL FEATURES OF THE DYNAMIC REGIME OF THE IONOSPHERE OVER THE SOUTH OF EASTERN SIBERIA

We have carried out a statistical analysis of a huge array of archival experimental data on the dynamic regime of the ionosphere over Irkutsk, obtained by a radiophysical spaced-receiver method with a small base of a rad...

CALIBRATION OF SIBERIAN RADIOHELIOGRAPH IMAGES

We discuss the method for automatic calibration of solar radio images derived from the first stage of the multiwave Siberian Radioheliograph (SRH-48). SRH is a 48-element T-shaped radiointerferometer in the 4–8 GHz frequ...

SPATIAL STRUCTURE OF AZIMUTHALLY SMALL-SCALE MHD WAVES IN ONE-DIMENSIONALLY INHOMOGENEOUS FINITE PRESSURE PLASMA WITH CURVED FIELD LINES

We have studied propagation of hydromagnetic (MHD) waves in one-dimensionally inhomogeneous finite pressure plasma with curved field lines. Magnetic surfaces are considered to be concentric cylinders, where the cylinder’...

Download PDF file
  • EP ID EP700237
  • DOI 10.12737/stp-64202002
  • Views 121
  • Downloads 0

How To Cite

Turova I. P. , Grigoryeva S. A. , Ozhogina O. A. (2020). SPATIAL AND TEMPORAL VARIATIONS OF K CA II LINE PROFILE SHAPES IN DIFFERENT STRUCTURES OF THE SOLAR CHROMOSPHERE. II. DETERMINATION TECHNIQUE AND CORRELATION RELATIONSHIPS BETWEEN THE K CA II LINE PARAMETERS FOR K₁ AND K₂ FEATURES. Solar-Terrestrial Physics, 6(4), -. https://europub.co.uk/articles/-A-700237