This instrument has two ranges for optical imaging of the Sun’s corona: C2 (covers distance range of 1.5 to 6 solar radii) and C3 (range of 3 to 32 solar radii). The calculation shows that this formula is in good agreement with the data at distances from the lower corona to the Earth's orbit. The NASA Solar and Heliospheric Observatory (SOHO) carries a coronagraph known as the Large Angle and Spectrometric Coronagraph (LASCO). The average electron density distribution in the inner corona has been determined by using white-light observations by Saito (1970). The obtained calculation results are compared with the results of other authors and they have been found to be consistent when choosing the parameters included in the formula. In particular, using the well-known empirical formula (dν)/(dt)=-0.01ν 1.84, we can obtain (1-α)b=0.42. The outermost layer of the Sun is known as the corona. As a result of integration of equation, we obtain the electron density n e(r) in the form n e= n 0(1+y)((-1) ⁄ ((1-α)b)), y=((1-α)/(α)) b ((r)/(λ T) and the constants are determined in comparison with the empirical formulas for FDR. At that distance, the sun-facing side of the spacecraft will get roasted to over 1,300 degrees Celsius, its suite of instruments protected by an 11-centimeter-thick carbon-composite shield. The scale height is presented in a combination of two distance dependencies as H= αλ T+(1-α)f(r). We investigated the certain dependence of the scale height on the distance, which allows us to obtain different dependence of the frequency drift rate (FDR) on the frequency. However, the relationship needed to describe qualitatively the Solar corona observations, Rodrguez Gmez, 2017 19, requires 1/2, while the quiescent. In addition, solar coronal mass ejections (CMEs) sweep aside cosmic rays. It has been proven that electron density in the solar corona is determined by observing the frequency drift of type III radio bursts. With the sun, Earth, and Moon perfectly aligned, the faces of the 5-sided. Sun: corona, Sun: electron density, Sun: radio burst type III, Sun: frequency drift rate Abstract This section gives a succinct overview of the Coronal Rotational Tomography method which is used to gain the coronal electron density state of the solar corona (Section 2.1), an overview of the time-dependent Heliopsheric Upwind eXtrapolation model used to test and validate the results (Section 2.2), followed by a description of how a density. Department of Astrophysics, Institute of Astronomy & Geophysics, Mongolian Academy of Sciences, Ulaanbaatar, Mongolia

Sun corona density