Mercury sodium exospheric emission as a proxy for solar perturbations transit

Review of the present problems of relativistic celestial mechanics. Advantage is taken of the method suggested earlier by the author and based on using quasi-Galilean coordinates with arbitrary coordinate functions or parameters. As compared with the previous papers the new elements are post-post-Newtonian approximation for the circular motion in the Schwarzschild problem and reduction of the artificial satellite problem including the main solar perturbations to the Schwarzschild problem. Some current questions of time scales definitions, reference frames and reduction of observations are briefly discussed.

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Lifetime Estimation of the Upper Stage of GSAT-14 in Geostationary Transfer Orbit

International Scholarly Research Notices ◽

10.1155/2014/864953 ◽

2014 ◽

Vol 2014 ◽

pp. 1-8 ◽

Cited By ~ 1

Author(s):

Jim Fletcher Jeyakodi David ◽

Ram Krishan Sharma

Keyword(s):

Initial Conditions ◽

Lifetime Estimation ◽

Eccentric Orbits ◽

Solar Perturbations ◽

Transfer Orbit ◽

Upper Stage ◽

Optimal Values ◽

The Mean ◽

Satellite Launch Vehicle ◽

Earth’S Oblateness

The combination of atmospheric drag and lunar and solar perturbations in addition to Earth’s oblateness influences the orbital lifetime of an upper stage in geostationary transfer orbit (GTO). These high eccentric orbits undergo fluctuations in both perturbations and velocity and are very sensitive to the initial conditions. The main objective of this paper is to predict the reentry time of the upper stage of the Indian geosynchronous satellite launch vehicle, GSLV-D5, which inserted the satellite GSAT-14 into a GTO on January 05, 2014, with mean perigee and apogee altitudes of 170 km and 35975 km. Four intervals of near linear variation of the mean apogee altitude observed were used in predicting the orbital lifetime. For these four intervals, optimal values of the initial osculating eccentricity and ballistic coefficient for matching the mean apogee altitudes were estimated with the response surface methodology using a genetic algorithm. It was found that the orbital lifetime from these four time spans was between 144 and 148 days.

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On the analytic lunar and solar perturbations of a near Earth satellite

Celestial Mechanics ◽

10.1007/bf01586857 ◽

1974 ◽

Vol 10 (3) ◽

pp. 253-276 ◽

Cited By ~ 3

Author(s):

Ronald H. Estes

Keyword(s):

Earth Satellite ◽

Solar Perturbations

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INCREASES IN SCR ENERGETIC PROTON FLUXES ON EARTH AND THEIR RELATION TO SOLAR SOURCES

Solar-Terrestrial Physics ◽

10.12737/stp-64202006 ◽

2020 ◽

Vol 6 (4) ◽

pp. 40-43

Author(s):

Leonid Lazutin

Keyword(s):

Solar Flare ◽

Solar Proton ◽

Maximum Energy ◽

Solar Cosmic Rays ◽

Proton Acceleration ◽

Flux Intensity ◽

Solar Perturbations ◽

No Scr ◽

Galactic Background ◽

Accelerated Particles

Logachev catalog data for solar cycle 23 has been used to study the dependence of measured increases in solar cosmic rays (SCRs) on solar perturbations. The efficiency of recording the SCR increases, driven by proton acceleration in the corona, on Earth and in its vicinity is shown to depend on power of a solar flare that created a shock wave and on position of the flare on the solar disk. As the particle flux moves along the heliolongitude away from the parent flare, the acceleration efficiency decreases, i.e. the maximum energy of the accelerated particles and their intensity at equal energy decrease. As a result, at a certain distance along a heliolongitude from the parent solar flare, the solar proton flux intensity decreases to the galactic background, and there is no SCR increase detected.

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INCREASES IN SCR ENERGETIC PROTON FLUXES ON EARTH AND THEIR RELATION TO SOLAR SOURCES

Solnechno-Zemnaya Fizika ◽

10.12737/szf-64202006 ◽

2020 ◽

Vol 6 (4) ◽

pp. 46-50

Author(s):

Leonid Lazutin

Keyword(s):

Solar Flare ◽

Solar Proton ◽

Maximum Energy ◽

Solar Cosmic Rays ◽

Proton Acceleration ◽

Flux Intensity ◽

Solar Perturbations ◽

No Scr ◽

Galactic Background ◽

Accelerated Particles

Logachev catalog data for solar cycle 23 has been used to study the dependence of measured increases in solar cosmic rays (SCRs) on solar perturbations. The efficiency of recording the SCR increases, driven by proton acceleration in the corona, on Earth and in its vicinity is shown to depend on power of a solar flare that created a shock wave and on position of the flare on the solar disk. As the particle flux moves along the heliolongitude away from the parent flare, the acceleration efficiency decreases, i.e. the maximum energy of the accelerated particles and their intensity at equal energy decrease. As a result, at a certain distance along a heliolongitude from the parent solar flare, the solar proton flux intensity decreases to the galactic background, and there is no SCR increase detected.

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