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

MODERN HEATING FACILITY FOR RESEARCH INTO THE MID-LATITUDE IONOSPHERE

The development of new devices for research in physics of the upper atmosphere and near-Earth space, which can be used to carry out controlled experiments on the modification of the ionosphere by powerful short-wave radi...

DETERMINATION OF ELF WAVE CHARACTERISTICS MOST STRONGLY REACTING TO MINOR CHANGES OF IONOSPHERIC ELECTRON DENSITY IN A HIGH-LATITUDE REGION

In this paper, we use numerical experiment methods to address the problem of determining characteristics of ELF (0.3–3 kHz) electromagnetic waves recorded in the surface layer and providing the maximum amount of informat...

Conditions for the occurrence of intense fluxes of energetic electrons at L<1.2 associated with solar activity and solar wind parameters

We present the results of a statistical study of transient enhancements of electrons with energies >30 keV at low drift shells in the quasi-trapped region (forbidden zone) at the geomagnetic equator. Using data from low-...

OPTICAL OBSERVATIONS OF SMALL SPACECRAFT AND SPACE DEBRIS AT ISTP SB RAS SAYAN OBSERVATORY

Launch of several thousands of small spacecraft as part of satellite groups of various companies (OneWeb, SpaceX, etc.) is expected in the coming years. They will significantly increase the “population” in the low-orbit...

HEURISTIC MODEL OF SOLAR X-RAY SPECTRUM ACCORDING TO SATELLITE DATA FOR GEOPHYSICAL APPLICATIONS

Model and computational algorithm for recovering the X-ray component of the solar spectrum based on GOES XL (0.1–0.8 nm), XS (0.05–0.4 nm or 0.05–0.3 nm) and SDO QD (0.1–7 nm) channels data are presented. The model based...

Download PDF file
  • EP ID EP700237
  • DOI 10.12737/stp-64202002
  • Views 125
  • 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