Basic magnetic configuration and energy supply processes for an interacting flux model of eruptive solar flares

Priest, E. R.

doi:10.1007/3-540-55246-4_71

Cited by 7 publications

(3 citation statements)

References 37 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…In the case of CMEs associated with solar flares, such an association is not unexpected since it has already been shown that solar flares are often associated with new emerging flux regions [Rust, 1976;Martin et at., 1983, 1984, Rust and Cauzzi, 1992, and flare models based on this observation have been developed (c.f. Heyvaerts and Priest, [1976] and references in the recent review by Priest [1992]). In much of the work described below we are particularly interested in CMEs associated with quiescent filament disappearances.…”

mentioning

confidence: 99%

The initiation of coronal mass ejections by newly emerging magnetic flux

Feynman¹,

Martin²

1995

J. Geophys. Res.

281

200

View full text Add to dashboard Cite

We present observational evidence that eruptions of quiescent filaments and associated coronal mass ejections (CMEs) occur as a consequence of the destabilization of large‐scale coronal arcades due to interactions between these structures and new and growing active regions. Both statistical and case studies have been carried out. In a case study of a “bugle” observed by the High‐Altitude Observatory Solar Maximum Mission coronagraph, the high‐resolution magnetograms from the Big Bear Solar Observatory show newly emerging and rapidly changing flux in the magnetic fields that apparently underlie the bugle. For other case studies and in the statistical work the eruption of major quiescent filaments was taken as a proxy for CME eruption. We have found that two thirds of the quiescent‐filament‐associated CMEs occurred after substantial amounts of new magnetic flux emerged in the vicinity of the filament. In addition, in a study of all major quiescent filaments and active regions appearing in a 2‐month period we found that 17 of the 22 filaments that were associated with new active regions erupted and 26 of the 31 filaments that were not associated with new flux did not erupt. In all cases in which the new flux was oriented favorably for reconnection with the preexisting large‐scale coronal arcades; the filament was observed to erupt. The appearance of the new flux in the form of new active regions begins a few days before the eruption and typically is still occurring at the time of the eruption. A CME initiation scenario taking account of these observational results is proposed.

show abstract

mentioning

confidence: 99%

The initiation of coronal mass ejections by newly emerging magnetic flux

Feynman¹,

Martin²

1995

J. Geophys. Res.

281

200

View full text Add to dashboard Cite

show abstract

“…During the solar flares, magnetic energy of 10 29 to 10 33 ergs is released by means of magnetic reconnection (Anastasiadis, 1999). The energy released during solar flare is used in intense localized heating, particle acceleration and in mass flows (Priest, 1992).…”

Section: Introductionmentioning

confidence: 99%

Enhancement in electron and ion temperatures due to solar flares as measured by SROSS-C2 satellite

et al. 2004

View full text Add to dashboard Cite

Abstract. The observations on the ionospheric electron and ion temperatures (T e and T i ) measured by the RPA payload aboard the SROSS-C2 satellite have been used to study the effect of solar flares on ionospheric heating. The data on solar flare has been obtained from the National Geophysical Data Center (NGDC) Boulder, Colorado (USA). It has been found that the electron and ion temperatures have a consistent enhancement during the solar flares on the dayside Earth's ionosphere. The estimated enhancement for the average electron temperature is from 1.3 to 1.9 times whereas for ion temperature it is from 1.2 to 1.4 times to the normal days average temperature. The enhancement of ionospheric temperatures due to solar flares is correlated with the diurnal variation of normal days' ionospheric temperatures. The solar flare does not have any significant effect on the nightside ionosphere. A comparison with the temperature obtained from the IRI-95 model also shows a similar enhancement.

show abstract

“…Επιτάχυνση σε κέντρα όρασης 1993). Παράλληλα νέες μελέτες πραγματοποιήθηκαν τα τελευταία χρό νια, αναφορικά με τον τρόπο εξέλιξης των δυναμικών μαγνητικών γραμ μών επάνω από την τυρβώδη φωτόσφαιρα του Ηλιου, με σκοπό τη δη μιουργία πιο ρεαλιστικών τοπολογιών για το μαγνητικό πεδίο ( Parker 1983;Van Ballegooijen 1986;Low k Wolfson 1988;Mikic, Barnes L• Schnack 1988;Priest 1992;Low 1992). Η ανάπτυξη αυτή είχε ως απο τέλεσμα τη δημιουργία και μελέτη ορισμένων ποιοτικών μοντέλων για την έκλυση της ενέργειας στις ηλιακές εκλάμψεις (για επισκόπηση βλέπε 1993a;1993b).…”

Section: μηχανισμοί επιτάχυνσηςunclassified

Επιταχυνση Φορτιων Απο Τυχαιως Κινουμενα Κρουστικα Κυματα

Αναστασιου¹

View full text Add to dashboard Cite

In this thesis the problem of energetic particle (electrons and ions) acceleration by an ensemble of shock waves is addressed. Shock waves are generated, moving randomly, inside a turbulent flow (e.g. jets and hot spots of extragalactic radio sources) or in an involving and constantly changing active region on the Sun. The acceleration is based on the 'shock drift mechanism' using the adiabatic treatment. The transport and the radiation of the particles in stochastic magnetic fields is also studied.The resulting energy distribution of the energetic particles is calculated analytically and numerically, after their interaction with a number of shock waves. Two models are presented, the first one is an application to the solar flare problem (see Anastasiadis A.

show abstract

Basic magnetic configuration and energy supply processes for an interacting flux model of eruptive solar flares

Cited by 7 publications

References 37 publications

The initiation of coronal mass ejections by newly emerging magnetic flux

The initiation of coronal mass ejections by newly emerging magnetic flux

Enhancement in electron and ion temperatures due to solar flares as measured by SROSS-C2 satellite

Επιταχυνση Φορτιων Απο Τυχαιως Κινουμενα Κρουστικα Κυματα

Contact Info

Product

Resources

About