Catalogo Articoli (Spogli Riviste)

OPAC HELP

Titolo:
Coronal mass ejections (CMEs) and their geoeffectiveness
Autore:
Plunkett, SP; Wu, ST;
Indirizzi:
USN, Res Lab, Univ Space Res Assoc, Washington, DC 20375 USA USN Washington DC USA 20375 niv Space Res Assoc, Washington, DC 20375 USA Univ Alabama, Ctr Space Plasma & Aeronom Res, Huntsville, AL 35899 USA Univ Alabama Huntsville AL USA 35899 eronom Res, Huntsville, AL 35899 USA Univ Alabama, Dept Mech Engn, Huntsville, AL 35899 USA Univ Alabama Huntsville AL USA 35899 Mech Engn, Huntsville, AL 35899 USA
Titolo Testata:
IEEE TRANSACTIONS ON PLASMA SCIENCE
fascicolo: 6, volume: 28, anno: 2000,
pagine: 1807 - 1817
SICI:
0093-3813(200012)28:6<1807:CME(AT>2.0.ZU;2-X
Fonte:
ISI
Lingua:
ENG
Soggetto:
MAGNETIC-FIELD; JANUARY 1997; GEOMAGNETIC-ACTIVITY; SMM OBSERVATIONS; SOLAR CORONA; FLUX ROPE; EVOLUTION; ENERGY; STORMS; LASCO;
Keywords:
coronal ejection; MHD modeling; solar activity; sun-earth connection;
Tipo documento:
Article
Natura:
Periodico
Settore Disciplinare:
Physical, Chemical & Earth Sciences
Citazioni:
66
Recensione:
Indirizzi per estratti:
Indirizzo: Plunkett, SP USN, Res Lab, Univ Space Res Assoc, Code 7667, Washington, DC20375 USA USN Code 7667 Washington DC USA 20375 ashington, DC 20375 USA
Citazione:
S.P. Plunkett e S.T. Wu, "Coronal mass ejections (CMEs) and their geoeffectiveness", IEEE PLAS S, 28(6), 2000, pp. 1807-1817

Abstract

The Sun's activity drives the variability of geospace (i.e., near-earth environment). Observations show that the ejection of plasma from the sun, called coronal mass ejections (CMEs), are the major cause of geomagnetic storms. This global-scale solar dynamical feature of coronal mass ejection was discovered almost three decades ago by the use of space-borne coronagraphs (OSO-7, Skylab/ATM and P78-1). Significant progress has been made in understanding the physical nature of the CMEs. Observations show that these global-scale CMEs have size in the order of a solar radius (similar to6.7 x 10(5)km) near the sun, and each el ent involves a mass of about 10(15) g and anenergy comparable to that of a large flare on the order of 10(32) ergs, The radial propagation speeds of CMEs have a wide range from tens to thousands of kilometers per second. Thus, the transit time to near earth's environment [i.e., 1 AU (astronomical unit)] can be as fast as 40 hours to 100 hours. The typical transit time for geoeffective events is similar to 60-80 h [1],This paper consists of two parts. 1) A summary of the observed CMEs from Skylab to the present SOHO will be presented. Special attention will be madeto SOHO/LASCO/EIT observations and their characteristics lending to a geoeffective CME. 2) The chronological development of theory and models to interpret the physical nature of this fascinating phenomenon will be reviewed. Finally, an example will be presented to illustrate the geoeffectiveness ofthe CMEs by using both observation and model.

ASDD Area Sistemi Dipartimentali e Documentali, Università di Bologna, Catalogo delle riviste ed altri periodici
Documento generato il 18/09/20 alle ore 16:40:42