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2 edition of Electron densities and scale heights in the topside ionosphere found in the catalog.

Electron densities and scale heights in the topside ionosphere

Kwok-Long Chan

Electron densities and scale heights in the topside ionosphere

Alouette 1, observations over the American continents.

by Kwok-Long Chan

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Published by National Aeronautics and Space Administration in Washington D.C .
Written in English


Edition Notes

StatementKwok-Long Chan, Lawrence Colin, and John O. Thomas.
SeriesNASA special publication -- 3034
ContributionsColin, Lawrence., Thomas, J. O. 1926-, United States. National Aeronautics and Space Administration. Office of Technology Utilization.
ID Numbers
Open LibraryOL13890194M

Measurement of Ionospheric Electron Density Profile The equivalent height of the ionosphere can be measured in a fairly straightforward manner, by timing how long it takes a radio pulse fired vertically upwards to return to ground level again. @article{osti_, title = {An observational study of the nightside ionospheres of Mars and Venus with radio occultation methods}, author = {Zhang, M.H.G. and Luhmann, J.G. and Kliore, A.J.}, abstractNote = {An analysis of Mars and Venus nightside electron density profiles obtained with radio occultation methods shows how the nightside ionospheres of both planets vary with solar zenith angle. Ionosphere observations indicated the emergence of a daytime super-fountain effect lifting the ionosphere to new heights and increasing its total electron content by as much as percent. Also observed were very large amplitude traveling ionospheric disturbances (Figure ), new ionosphere layers, and very different behavior in equatorial. and time dependencies of the measured electron and ion densities in the Mars ionosphere versus solar activity, heliocentric distance, and local solar time [1]. The major positive ion is O2 + and electron-ion recombination is expected to be quadratic in the electron density, i.e., in equation (12), 0 and 1 vanish, but 2 does not. Ferraro [

2-() 16 1•6 14 • 2 LOG Re Rc 10 06 04 02 0 ~. I Ll._ I: aos 2 ITTii (HI I I l 4 5 1/.


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Electron densities and scale heights in the topside ionosphere by Kwok-Long Chan Download PDF EPUB FB2

Electron densities and scale heights in the topside ionosphere: Alouette I: observations recorded at Hawaii, wintersummer [Lawrence Colin, Kwok-Long Chan] on *FREE* shipping on qualifying offers. Electron densities and scale heights in the topside ionosphere: Alouette I: observations recorded at HawaiiAuthor: Lawrence Colin, Kwok-Long Chan.

Get this from a library. Electron densities and scale heights in the topside ionosphere: Alouette I observations in midlatitudes, summerwinter.

Electron densities and scale heights in the topside ionosphere: Alouette I observations over the American continents. Washington, Scientific and Technical Information Division, National Aeronautics and Space Administration; [for sale by the Clearinghouse for Federal Scientific and Technical Information, Springfield, Va.] Alouette I measurements of electron densities and scale heights in topside ionosphere - tabular data analysis.

ELECTRON DENSITIES and SCALE HEIGHTS in the TOPSIDE IONOSPHERE: Alouette I Ovservations Over The American Continents - Volume IV (4), Summary Graphs, NASA SP [Chan, Kwok-Long; Colin, Lawrence; Thomas, John O.] on *FREE* shipping on qualifying offers.

ELECTRON DENSITIES and SCALE HEIGHTS in the TOPSIDE IONOSPHERE: Alouette I Ovservations Over The Author: John O. Chan, Kwok-Long; Colin, Lawrence; Thomas. Full text of "Electron densities and scale heights in the topside ionosphere - Alouette I observations over the American II - March and May " See other formats.

New Vary-Chap profile of the topside ionosphere electron density distribution for use with the IRI model and the GIRO real time data Patrick Nsumei,1 Bodo W.

Reinisch,1,2 Xueqin Huang,1 and Dieter Bilitza3,4 Received 26 January ; revised 30 March ; accepted 3 Cited by: The ionosphere (/ aɪ ˈ ɒ n ə ˌ s f ɪər /) is the ionized part of Earth's upper atmosphere, from about 60 km (37 mi) to 1, km ( mi) altitude, a region that includes the thermosphere and parts of the mesosphere and ionosphere is ionized by solar radiation.

It plays an important role in atmospheric electricity and forms the inner edge of the magnetosphere. Journal of Atmospheric and Tenerial Physics, Electron densities and scale heights in the topside ionosphere book, Vol. 29, pp. Pergamon Press Ltd. Printed In Northern Ireland Estimates of ionospheric composition and temperature derived from topside sounder electron scale height data P.

SMITH and B. KAISER S.R.C., Radio and Space Research Station, Ditton Park, Slough, by:   Anthony J. Mannucci, Bruce T. Tsurutani, in Extreme Events in Geospace, 5 Conclusions and Future Outlook. The largest increases in ionospheric electron density and total electron content during intense geomagnetic storms are due to prompt penetration electric fields (PPEF), that tend to occur during the storm main phase, and can last for several hours.

et al. (), who made a comparison between electron density values in the topside part of the ionosphere measured by Swarm satellites and calculated by IRI.

The need to mathematically model the topside ionosphere led many scientists to apply several analyticalCited by: 3. Plasma scale height is an important parameter of topside ionosphere and contains information about ionospheric physics and dynamic.

We investigated the seasonal features of vertical scale height. For example, the International Reference Ionosphere (IRI) model 6 is not able to represent properly the real features of the topside ionosphere [7] [8][9].

One of the topside options proposed by. Note that in this work, we used data from DEMETER at almost a fixed orbit height of ~ km. Thus, the satellite sampled the topside ionosphere where electron density decreases with plasma scale height and electron temperature increases with height [e.g., Schunk and Nagy, ].

Earth Planets Space, 55, –, Equivalent electron densities at reflection heights of tweek atmospherics in the low-middle latitude Electron densities and scale heights in the topside ionosphere book ionosphere H. Ohya1, M. Nishino2, Y. Murayama3, and K. Igarashi3 1Department of Electronics and Mechanical Engineering, Chiba University, ChibaJapan 2Solar-Terrestrial Environment Laboratory, Nagoya University, ToyokawaJapanCited by: compares NeQuick and IRI models with the topside electron density profiles available in the databases of the ISIS2, IK19 and Cosmos satellites.

Experimental electron content from the F2 peak up to satellite height and electron densities at fixed heights above the peak have been compared under a wide range of different con-ditions. Electron densities in the upper ionosphere of Mars from the excitation of electron plasma oscillations F.

Duru,1 D. Gurnett,1 D. Morgan,1 R. Modolo,1 A. Nagy,2 and D. Najib2 Received 1 February ; revised 20 February ; accepted 28 February ; published 9 July Topside O+ H+ O+ O2 + NO Density: Altitude in km Hmax Nmax Figure 2. Various layers of the ionospher e and their predominant ion populations ar e listed at their respective heights above gr ound.

The density in the ionosphere varies considerably, as shown. F2 Layer D Region Electrons/cm3 lowest is the D-region, covering altitudes be-File Size: KB. ELECTRON TEMPERATURE AND DENSITY OF THE TOPSIDE EQUATORIAL IONOSPHERE AS OBTAINED FROM A THEORETICAL MODEL K.K.

Chetia(1), A. Borgohain(2) around F peak heights, exhibited a minimum around pre-sunrise hours and a maximum during daytime.

On the other temperature is due to low electron densities and photoelectron heating. In the evening. ionospheric scale heights, as well as the shape of the topside electron density profiles. Over Millstone Hill, the diurnal be-haviors of the median VSH and Hm are very similar to each other and are not so tightly correlated with that of the plasma scale height Hp or the plasma temperature.

The present study confirms the sensitivity of the. Electron densities and scale heights in the topside ionosphere: Alouette I observations over the America International reference ionosphere [microform] / Dieter Bilitza; Space physics investigator semiannual report for NASA research grant NAG5 [microform] / principal i.

[1] A simple model for the topside ionosphere region is introduced and applied to fit radio‐occultation‐retrieved electron density profiles for altitudes above the F2 peak. The model considers two isothermal components representing the population of the O + (ionosphere component) and the H + (protonosphere component) ions.

The purpose of the model is to achieve an accurate fit of the. Electron Densities and Scale Heights in the Topside Ionosphere, a Data Publication in a series of volumes by AMES Research Center, Clearinghouse for Federal Scientific and Technical Information, Springfield, Virginia, by: 9.

> and ionospheric scale heights H at altitudes between the F-layer peak and km. Data acquired during eight COSMIC-C/NOFS-DMSP conjunctions on 24 – 25 October are used to demonstrate the proposed method’s feasibility then outline our plan to apply it to large databases. Our ultimate goal is to specify topside EDP taxonomies.

If the address matches an existing account you will receive an email with instructions to reset your password. Indian Journal of Radio & Space Physics Vol.

10, Junepp. Electron Temperature Models for the F-Region & Topside Ionosphere V K PANDEY & K K MAHAJAN Radio Science Division, National Physical Laboratory, New Delhi 'Author: V.

Pandey, K. Mahajan. The formulation of the topside electron density in NeQuick model has been analysed looking at possible improvements of the model performance. The present topside formulation is based on a semi-Epstein layer with a height-dependent thickness parameter, which allows to take into account in a simplified way the electron content up to.

α-Chapman topside analytical formulation performs better than the other topside formulations, and the IRI model, for both Swarm A&C and Swarm B databases; The working hypothesis related to the plasma scale height constancy for the lower topside part of the ionospheric vertical electron density profile has been found reasonable.

density unless the 0 + scale height is very observed in the topside ionosphere, with cone large. The outflow decreases with decreasing angles close to 90 ø and only small upward field-aligned current density and, to a lesser field-aligned velocity components. largely able to reproduce the observed high topside ionosphere electron temperatures (e.g., K at km altitude) without using a topside heat flux when magnetic field topologies consistent with the measured magnetic field were adopted.

Magnetic topology affects both suprathermal electron transport and thermal electron heat Size: 2MB. 1 High-Latitude Topside Ionospheric Vertical Electron-Density-Profile Changes in Response to Large Magnetic Storms Robert F.

Benson 1, Joseph Fainberg, Vladimir A. Osherovich2, Vladimir Truhlik3, Yongli Wang4, Dieter Bilitza5, and Shing F. Fung1 1NASA/Goddard Space Flight Center, Geospace Physics Laboratory, CodeHeliophysics Science Division, Greenbelt, MD USA.

In this study, we estimated the topside scale height of plasma density (Hm) using the Swarm constellation and ionosondes in Korea. The Hm above Korean Peninsula is generally around 50 km.

Statistical distributions of the topside scale height exhibited a complex dependence upon local time and season. The International Reference Ionosphere (IRI) a joint project of URSI and COSPAR is the defacto standard for overestimation of electron densities in the upper topside (from about km above the F-peak upward) that scale height) parameter that provides a smooth transition from an atomic oxygen ionosphere to a light ion ionosphere.

The model. Sibanda and L. McKinnell: Topside ionospheric vertical electron density profile reconstruction the section that follows resulting in a profile that is unique to a specific set of geophysical conditions.

Therefore, the focus of the present study is on the ability to construct the shape of. independent scale height cannot reproduce the topside Ne profile exactly. Therefore a further investigation on the shape of the topside profile is indeed important.

[4] In the present study, we hope to answer what the shape factors should be in the topside ionosphere if we take the scale height from an atmospheric model as Ezquer et al.

[ How the ionosphere varies. Plasma densities in the ionosphere are characterized by strong day-night variability. The maximum ionospheric plasma density (approximately one million electrons per cubic centimeter) occurs in the noon F region, at an altitude of km. Superthermal electron energy interchange in the ionosphere-plasmasphere system G.

Khazanov,1 A. Glocer,1 M. Liemohn,2 and E. Himwich1 Received 10 September ; revised 10 January ; accepted 12 January File Size: 1MB. of superthermal electron transport calculates the distri-bution on a global scale throughout the subauroral magnetosphere (Khazanov et al., a, ).

Here, this model is used to determine the energy flux into the upper ionosphere from the calculated photoelectron and plasma sheet electron distribution functions in the midlatitude region.

The only in situ measurements of the thermal plasma composition, density, and temperature in the ionosphere of Mars were obtained by the retarding potential analyzers carried aboard the two Viking landers 11 and by the mass spectrometers mentioned above.

The retarding potential analyzers provided two vertical profiles of the densities of the three most abundant ions (O 2 +, O +, and CO 2 +) in. TISH - Topside Ionosphere Scale Height.

Looking for abbreviations of TISH. It is Topside Ionosphere Scale Height. Topside Ionosphere Scale Height listed as TISH. Topside Ionosphere Scale Height - How is Topside Ionosphere Scale Height abbreviated.

Topside Electromagnetic Aperture Management System; Topside Fabrication and Installation. @article{osti_, title = {Storm-induced changes of the topside ionosphere as deduced from incoherent-scatter radars. Master's thesis}, author = {Lunn, K.J.}, abstractNote = {Incoherent scatter radar observations from Millstone Hill, Saint Santin, and Arecibo are used to illustrate changes of the topside ionosphere during a geomagnetic storm.Ionosphere and magnetosphere, regions of Earth’s atmosphere in which the number of electrically charged particles— ions and electrons—are large enough to affect the propagation of radio charged particles are created by the action of extraterrestrial radiation (mainly from the Sun) on neutral atoms and molecules of ionosphere begins at a height of about 50 km (30 miles.The ionosphere is the region from about 60 km to km altitude, where the solar irradiance produces a partially ionized plasma of mostly H+ and He+ above km, O+ from to km and molecular ion (NO+, O2+, N2+) below km.

Total ion densities (= electron density) range from 10^8 to 10^13 m