Solar cycle in the photosphere and corona

E. E. Benevolenskaya; A. G. Kosovichev; P. H. Scherrer

Solar cycle in the photosphere and corona

E. E. Benevolenskaya, A. G. Kosovichev, P. H. Scherrer

Research output: Contribution to journal › Conference article › peer-review

Abstract

EIT/SOHO data in four EUV lines and MDI/SOHO (1996-2002), and soft X-ray YOHKOH data (1991-2001) are analyzed in the form of coronal synoptic maps for the investigation of solar cycle variations of the corona and magnetic field. The evolution of coronal structures is closely related to sunspot activity, photospheric magnetic field, and topology of the large-scale magnetic field. The coronal structures visible in extreme ultraviolet and soft X-rays as extended bright loops, reflect the non-axisymmetrical magnetic structure of the Sun, changing with the solar cycle. The long-living coronal structures are related to complexes of solar activity and display the quasiperiodic behavior (impulses of coronal activity) with periods of 1.0-1.5 year in the axisymmetrical distribution of EUV and X-ray fluxes during the current cycle.

Original language	English (US)
Pages (from-to)	831-834
Number of pages	4
Journal	European Space Agency, (Special Publication) ESA SP
Issue number	506 II
State	Published - Dec 2002
Externally published	Yes
Event	The 10th European Solar Physics Meeting; Solar Variability: From Core to Outer Frontiers - Prague, Czech Republic Duration: Sep 9 2002 → Sep 14 2002

All Science Journal Classification (ASJC) codes

Aerospace Engineering
Space and Planetary Science

Keywords

EUV and X-ray corona
Magnetic flux
Solar cycle
Sun

Cite this

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title = "Solar cycle in the photosphere and corona",

abstract = "EIT/SOHO data in four EUV lines and MDI/SOHO (1996-2002), and soft X-ray YOHKOH data (1991-2001) are analyzed in the form of coronal synoptic maps for the investigation of solar cycle variations of the corona and magnetic field. The evolution of coronal structures is closely related to sunspot activity, photospheric magnetic field, and topology of the large-scale magnetic field. The coronal structures visible in extreme ultraviolet and soft X-rays as extended bright loops, reflect the non-axisymmetrical magnetic structure of the Sun, changing with the solar cycle. The long-living coronal structures are related to complexes of solar activity and display the quasiperiodic behavior (impulses of coronal activity) with periods of 1.0-1.5 year in the axisymmetrical distribution of EUV and X-ray fluxes during the current cycle.",

keywords = "EUV and X-ray corona, Magnetic flux, Solar cycle, Sun",

author = "Benevolenskaya, {E. E.} and Kosovichev, {A. G.} and Scherrer, {P. H.}",

year = "2002",

month = dec,

language = "English (US)",

pages = "831--834",

journal = "European Space Agency, (Special Publication) ESA SP",

issn = "0379-6566",

publisher = "European Space Agency",

number = "506 II",

note = "The 10th European Solar Physics Meeting; Solar Variability: From Core to Outer Frontiers ; Conference date: 09-09-2002 Through 14-09-2002",

}

TY - JOUR

T1 - Solar cycle in the photosphere and corona

AU - Benevolenskaya, E. E.

AU - Kosovichev, A. G.

AU - Scherrer, P. H.

PY - 2002/12

Y1 - 2002/12

N2 - EIT/SOHO data in four EUV lines and MDI/SOHO (1996-2002), and soft X-ray YOHKOH data (1991-2001) are analyzed in the form of coronal synoptic maps for the investigation of solar cycle variations of the corona and magnetic field. The evolution of coronal structures is closely related to sunspot activity, photospheric magnetic field, and topology of the large-scale magnetic field. The coronal structures visible in extreme ultraviolet and soft X-rays as extended bright loops, reflect the non-axisymmetrical magnetic structure of the Sun, changing with the solar cycle. The long-living coronal structures are related to complexes of solar activity and display the quasiperiodic behavior (impulses of coronal activity) with periods of 1.0-1.5 year in the axisymmetrical distribution of EUV and X-ray fluxes during the current cycle.

AB - EIT/SOHO data in four EUV lines and MDI/SOHO (1996-2002), and soft X-ray YOHKOH data (1991-2001) are analyzed in the form of coronal synoptic maps for the investigation of solar cycle variations of the corona and magnetic field. The evolution of coronal structures is closely related to sunspot activity, photospheric magnetic field, and topology of the large-scale magnetic field. The coronal structures visible in extreme ultraviolet and soft X-rays as extended bright loops, reflect the non-axisymmetrical magnetic structure of the Sun, changing with the solar cycle. The long-living coronal structures are related to complexes of solar activity and display the quasiperiodic behavior (impulses of coronal activity) with periods of 1.0-1.5 year in the axisymmetrical distribution of EUV and X-ray fluxes during the current cycle.

KW - EUV and X-ray corona

KW - Magnetic flux

KW - Solar cycle

KW - Sun

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M3 - Conference article

AN - SCOPUS:0036975475

SN - 0379-6566

SP - 831

EP - 834

JO - European Space Agency, (Special Publication) ESA SP

JF - European Space Agency, (Special Publication) ESA SP

IS - 506 II

T2 - The 10th European Solar Physics Meeting; Solar Variability: From Core to Outer Frontiers

Y2 - 9 September 2002 through 14 September 2002

ER -

Solar cycle in the photosphere and corona

Abstract

All Science Journal Classification (ASJC) codes

Keywords

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