Solar flux variation of the electron temperature morning overshoot in the equatorial F region

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F68378289%3A_____%2F11%3A00366447" target="_blank" >RIV/68378289:_____/11:00366447 - isvavai.cz</a>

Výsledek na webu

<a href="http://www.agu.org/pubs/crossref/2011/2010JA016235.shtml" target="_blank" >http://www.agu.org/pubs/crossref/2011/2010JA016235.shtml</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1029/2010JA016235" target="_blank" >10.1029/2010JA016235</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Solar flux variation of the electron temperature morning overshoot in the equatorial F region

Popis výsledku v původním jazyce

Using 8 years of CHAMP satellite observations of the equatorial electron temperature, T(e), we investigate its behavior during the morning overshoot and at ionospheric altitudes below 450 km including its variation with solar activity. The morning T(e) has a maximum at the dip equator and decreases gradually with increasing latitude, which is due to the increasing importance of heat conduction as the dip angle becomes larger. The amplitude of the equatorial morning overshoot T(e) decreases with increasing solar flux by about -10 degrees K/solar flux unit depending on season and longitude. Trends of similar magnitude are predicted by the FLIP model. The model calculations confirm that the electron cooling due to enhanced electron-ion collisions increases faster than the heating of thermal electrons through collision with photoelectrons for increasing solar EUV. Both data and model showed that elevated electron temperatures persist to later local times during low solar activity.

Název v anglickém jazyce

Solar flux variation of the electron temperature morning overshoot in the equatorial F region

Popis výsledku anglicky

Using 8 years of CHAMP satellite observations of the equatorial electron temperature, T(e), we investigate its behavior during the morning overshoot and at ionospheric altitudes below 450 km including its variation with solar activity. The morning T(e) has a maximum at the dip equator and decreases gradually with increasing latitude, which is due to the increasing importance of heat conduction as the dip angle becomes larger. The amplitude of the equatorial morning overshoot T(e) decreases with increasing solar flux by about -10 degrees K/solar flux unit depending on season and longitude. Trends of similar magnitude are predicted by the FLIP model. The model calculations confirm that the electron cooling due to enhanced electron-ion collisions increases faster than the heating of thermal electrons through collision with photoelectrons for increasing solar EUV. Both data and model showed that elevated electron temperatures persist to later local times during low solar activity.

Druh

J_x - Nezařazeno - Článek v odborném periodiku (Jimp, Jsc a Jost)

CEP obor

DG - Vědy o atmosféře, meteorologie

OECD FORD obor

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Projekt

<a href="/cs/project/GAP209%2F10%2F2086" target="_blank" >GAP209/10/2086: Modelování variability parametrů termálního plazmatu v horní ionosféře a vnitřní magnetosféře Země</a><br>

Návaznosti

Z - Vyzkumny zamer (s odkazem do CEZ)

Rok uplatnění

2011

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Journal of Geophysical Research

ISSN

0148-0227

e-ISSN

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Svazek periodika

116

Číslo periodika v rámci svazku

—

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

13

Strana od-do

"A04308/1"-"A04308/13"

Kód UT WoS článku

000289644900005

EID výsledku v databázi Scopus

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