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Titolo:
Lasco observations of the coronal rotation
Autore:
Lewis, DJ; Simnett, GM; Brueckner, GE; Howard, RA; Lamy, PL; Schwenn, R;
Indirizzi:
Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England Univ Birmingham Birmingham W Midlands England B15 2TT W Midlands, England USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC 20375 USA USN Washington DC USA 20375 lburt Ctr Space Res, Washington, DC 20375 USA Astron Spatiale Lab, F-13376 Marseille, France Astron Spatiale Lab Marseille France F-13376 , F-13376 Marseille, France Max Planck Inst Aeron, D-37189 Katlenburg Lindau, Germany Max Planck Inst Aeron Katlenburg Lindau Germany D-37189 Lindau, Germany
Titolo Testata:
SOLAR PHYSICS
fascicolo: 2, volume: 184, anno: 1999,
pagine: 297 - 315
SICI:
0038-0938(199902)184:2<297:LOOTCR>2.0.ZU;2-Q
Fonte:
ISI
Lingua:
ENG
Soggetto:
MAGNETIC-FIELD; DIFFERENTIAL ROTATION; SOLAR CORONA; HOLES; EVOLUTION; EVENTS;
Tipo documento:
Article
Natura:
Periodico
Settore Disciplinare:
Physical, Chemical & Earth Sciences
Citazioni:
23
Recensione:
Indirizzi per estratti:
Indirizzo: Lewis, DJ Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England Univ Birmingham Birmingham W Midlands England B15 2TT , England
Citazione:
D.J. Lewis et al., "Lasco observations of the coronal rotation", SOLAR PHYS, 184(2), 1999, pp. 297-315

Abstract

The near-rigid rotation of the corona above the differential rotation of the photosphere has important implications for the form of the global coronal magnetic field. The magnetic reconfiguring associated with the shear region where the rigidly-rotating coronal field lines interface with the differentially-rotating photospheric field lines could provide an important energy source for coronal heating. We present data on coronal rotation as a function of altitude provided by the Large Angle Spectrometric Coronagraph (LASCO) instrument aboard the Solar and Heliospheric Observatory (SOHO) spacecraft. LASCO comprises of three coronagraphs (C1, C2, and C3) with nested fields of-view spanning 1.1 R. to 30 R.. An asymmetry in brightness, both of the Fe XIV emission line corona and of the broad-band electron scattered corona, has been observed to be stable over at least a one-year period spanning May 1996 to May 1997. This feature has presented a tracer for the coronalrotation and allowed period estimates to be made to beyond 15 R., up to 5 times further than previously recorded for the white-light corona. The difficulty in determining the extent of differential motion in the outer coronais demonstrated and latitudinally averaged rates formed and determined as a function of distance from the Sun. The altitude extent of the low latitude closed coronal field region is inferred from the determined rotation periods which is important to the ability of the solar atmosphere to retain energetic particles. For the inner green line corona (< 2 R.) we determine a synodic rotation period of (27.4 +/- 0.1) days, whereas, for the outer white-light corona, (> 2.5 R.) we determine a rotation period of (27.7 +/- 0.1) days.

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Documento generato il 04/12/20 alle ore 22:22:43