Field line distribution of mass density at geostationary orbit. Issue 6 (4th June 2015)

• Record Type: Journal Article
• Authors: Denton, R. E.; Takahashi, Kazue; Lee, Jinmyoung; Zeitler, C. K.; Wimer, N. T.; Litscher, L. E.; Singer, H. J.; Min, Kyungguk
• Is Part Of: Journal of geophysical research. Volume 120:Issue 6(2015:Jun.)
• Page Start: 4409
• Page End: 4422
• Publication Date: 2015-06-04
• Subjects: mass density -- field line distribution -- geostationary orbit -- Alfven waves; Magnetospheric physics -- Periodicals; Space environment -- Periodicals; Cosmic physics -- Periodicals; Planets -- Atmospheres -- Periodicals; Heliosphere (Astrophysics) -- Periodicals; Geophysics -- Periodicals; 523.01
• DOI: 10.1002/2014JA020810
• Languages: English
• ISSNs: 2169-9380

Abstract

Abstract: The distribution of mass density along the field lines affects the ratios of toroidal (azimuthally oscillating) Alfvén frequencies, and given the ratios of these frequencies, we can get information about that distribution. Here we assume the commonly used power law form for the field line distribution, ρ m = ρ m, eq ( L R E / R ) α, where ρ m, eq is the value of the mass density ρ m at the magnetic equator, L is the L shell, R E is the Earth's radius, R is the geocentric distance to a point on the field line, and α is the power law coefficient. Positive values of α indicate that ρ m increases away from the magnetic equator, zero value indicates that ρ m is constant along the magnetic field line, and negative α indicates that there is a local peak in ρ m at the magnetic equator. Using 12 years of observations of toroidal Alfvén frequencies by the Geostationary Operational Environmental Satellites, we study the typical dependence of inferred values of α on the magnetic local time (MLT), the phase of the solar cycle as specified by the F 10.7 extreme ultraviolet solar flux, and geomagnetic activity as specified by the auroral electrojet ( AE ) index. Over the mostly dayside range of the observations, we find that α decreases with respect to increasing MLT and F 10.7, but increases with respect to increasing AE . We develop a formula that depends on all three parameters, α 3Dmodel = 2 . 2 + 1 . 3 · cos MLT · 1 5 ∘ + 0 . 0026 · AE · cos ( MLT − 0 . 8 ) · 1 5 ∘ + 2 . 1 · 1 0 − 5 · AE · F 10 . 7 − 0 . 010 · F 10 . 7, that models the binned values of α within a standard deviation of 0.3. While we do not yet have a complete theoretical understanding of why α should depend on these parameters in such a way, we do make some observations and speculations about the causes. At least part of the dependence is related to that of ρ m, eq ; higher α, corresponding to steeper variation with respect to magnetic latitude, occurs when ρ m, eq is lower. Key Points: The typical field line distribution of mass density can be well modeled The mass density field line distribution depends on MLT, F 10.7, and A E