Pregled bibliografske jedinice broj: 1027959
Morphology of coronal hole based on SDO/AIA data in May 2010 - December 2013
Morphology of coronal hole based on SDO/AIA data in May 2010 - December 2013 // Book of Proceedings, Workshop "Solar Influences on the Magnetosphere, Ionosphere and Atmosphere" / Georgieva, Katya ; Kirov, Boian ; Danov, Dimitar (ur.).
Sofija: Space Research and Technologies Institute ; Bugarska akademija znanosti, 2019. str. 50-56 doi:10.31401/WS.2019.proc (predavanje, međunarodna recenzija, cjeloviti rad (in extenso), znanstveni)
CROSBI ID: 1027959 Za ispravke kontaktirajte CROSBI podršku putem web obrasca
Naslov
Morphology of coronal hole based on SDO/AIA data in May 2010 - December 2013
Autori
Šterc, Filip ; Maričić, Darije ; Roša, Dragan
Vrsta, podvrsta i kategorija rada
Radovi u zbornicima skupova, cjeloviti rad (in extenso), znanstveni
Izvornik
Book of Proceedings, Workshop "Solar Influences on the Magnetosphere, Ionosphere and Atmosphere"
/ Georgieva, Katya ; Kirov, Boian ; Danov, Dimitar - Sofija : Space Research and Technologies Institute ; Bugarska akademija znanosti, 2019, 50-56
Skup
11th Workshop “Solar Influences on the Magnetosphere, Ionosphere and Atmosphere”
Mjesto i datum
Primorsko, Bugarska, 03.06.2019. - 07.06.2019
Vrsta sudjelovanja
Predavanje
Vrsta recenzije
Međunarodna recenzija
Ključne riječi
solar wind disturbance, stream interface, high speed stream
Sažetak
We present an analysis of the high speed streams (HSSs) parameters, using in situ WIND data recorded from May 2010 to December 2012. For this purpose we made a list of 202 solar wind disturbances incorporated into an online catalogue for general use. Separating the solar wind signatures on: high speed streams, interplanetary coronal mass ejections (ICMEs), complex signatures ; we focused our attention on 102 HSSs (52% of all SW signatures) which can be clearly associated with particular stream interface (SI). Furthermore, we analyzed in detail the correlation of solar wind parameters in different parts of HSSs, particularly in front and behind of SI. We found the best correlation between maximum of the magnetic field strength Bvs proton density Np and proton thermal speed vth, 0.65 and 0.62, respectively. As well as between flow speed v and proton thermal speed vth, cc = 0.64. While the correlation is significantly lower (cc = 0.38) between magnetic field B and flow speed v. Also, the correlation between maximum of the magnetic field B, flow speed v and proton thermal speed vth, in the regions of HSS before and after SI are: cc = 0.84, 0.66 and 0.79, respectively. Correlations for the maximum of the proton density Np between these two HSS regions is significantly lower (cc = 0.39) and points out to the possibility of two different HSS families.
Izvorni jezik
Engleski
Znanstvena područja
Fizika
