Magnetic structure and reconnection of X-ray bright points in the solar corona

D S  Brown; C E  Parnell; E E  DeLuca; R A  McMullen; L  Golub; E R  Priest

Magnetic structure and reconnection of X-ray bright points in the solar corona

D S Brown
, C E Parnell
, E E DeLuca
, R A McMullen
, L Golub
, E R Priest

Applied Mathematics

Research output: Contribution to journal › Article › peer-review

Abstract

The three-dimensional magnetic topology of the solar corona is incredibly complex and its effect on the nature of 3D reconnection is profound. We study the supposedly simple topology of a small scale X-ray bright point observed by TRACE and SOHO/MDl, and how it is driven by reconnection when it forms and during the early stages of its lifetime. (C) 2002 COSPAR. Published by Elsevier Science Ltd. All rights reserved.

Original language	English
Pages (from-to)	1093-1099
Number of pages	7
Journal	Comparative Reconnection Studies at the Sun and in Planetary Magnetospheres
Volume	29
Publication status	Published - 2002

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MODEL

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abstract = "The three-dimensional magnetic topology of the solar corona is incredibly complex and its effect on the nature of 3D reconnection is profound. We study the supposedly simple topology of a small scale X-ray bright point observed by TRACE and SOHO/MDl, and how it is driven by reconnection when it forms and during the early stages of its lifetime. (C) 2002 COSPAR. Published by Elsevier Science Ltd. All rights reserved.",

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AU - Brown, D S

AU - Parnell, C E

AU - DeLuca, E E

AU - McMullen, R A

AU - Golub, L

AU - Priest, E R

PY - 2002

Y1 - 2002

N2 - The three-dimensional magnetic topology of the solar corona is incredibly complex and its effect on the nature of 3D reconnection is profound. We study the supposedly simple topology of a small scale X-ray bright point observed by TRACE and SOHO/MDl, and how it is driven by reconnection when it forms and during the early stages of its lifetime. (C) 2002 COSPAR. Published by Elsevier Science Ltd. All rights reserved.

AB - The three-dimensional magnetic topology of the solar corona is incredibly complex and its effect on the nature of 3D reconnection is profound. We study the supposedly simple topology of a small scale X-ray bright point observed by TRACE and SOHO/MDl, and how it is driven by reconnection when it forms and during the early stages of its lifetime. (C) 2002 COSPAR. Published by Elsevier Science Ltd. All rights reserved.

KW - FIELDS

KW - MODEL

UR - https://www.scopus.com/pages/publications/0036541955

M3 - Article

VL - 29

SP - 1093

EP - 1099

JO - Comparative Reconnection Studies at the Sun and in Planetary Magnetospheres

JF - Comparative Reconnection Studies at the Sun and in Planetary Magnetospheres

ER -

Magnetic structure and reconnection of X-ray bright points in the solar corona

Abstract

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