Stellar prominences and coronal magnetic fields

A C  Cameron; M  Jardine; K  Wood; J F  Donati

doi:10.1051/eas:2003103

Stellar prominences and coronal magnetic fields

A C Cameron, M Jardine, K Wood, J F Donati

School of Physics and Astronomy

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution

Abstract

Rapidly rotating solar type stars display varying amounts of chromospheric emission in their Balmer lines. The profiles of these lines often display rapid variability. Since the mid-1980s, high-cadence echelle spectroscopy of numerous such stars has revealed that some of the variability is caused by concentrations of neutral hydrogen, trapped in the stellar coronal magnetic field at distances up to a few stellar radii from the rotation axis. In this paper we review the observations and the tomographic techniques that can be applied to mapping these "sling-shot prominence" systems. We discuss the possible mechanisms for formation and mechanical support of these condensations, in the light of recent efforts to map 3-dimensional stellar coronal magnetic fields and X-ray emission measure distributions, with the help of Zeeman-Doppler imaging.

Original language	English
Title of host publication	MAGNETISM AND ACTIVITY OF THE SUN AND STARS
Editors	J Arnaud, N Meunier
Place of Publication	CEDEX A
Publisher	E D P Sciences
Pages	217-226
Number of pages	10
ISBN (Print)	2-86883-646-1
DOIs	https://doi.org/10.1051/eas:2003103
Publication status	Published - 2003
Event	International Conference on Magnetism and Activity of the Sun and Stars - Toulouse Duration: 17 Sept 2002 → 21 Sept 2002

Conference

Conference	International Conference on Magnetism and Activity of the Sun and Stars
City	Toulouse
Period	17/09/02 → 21/09/02

Access to Document

10.1051/eas:2003103

Cite this

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title = "Stellar prominences and coronal magnetic fields",

abstract = "Rapidly rotating solar type stars display varying amounts of chromospheric emission in their Balmer lines. The profiles of these lines often display rapid variability. Since the mid-1980s, high-cadence echelle spectroscopy of numerous such stars has revealed that some of the variability is caused by concentrations of neutral hydrogen, trapped in the stellar coronal magnetic field at distances up to a few stellar radii from the rotation axis. In this paper we review the observations and the tomographic techniques that can be applied to mapping these {"}sling-shot prominence{"} systems. We discuss the possible mechanisms for formation and mechanical support of these condensations, in the light of recent efforts to map 3-dimensional stellar coronal magnetic fields and X-ray emission measure distributions, with the help of Zeeman-Doppler imaging.",

author = "Cameron, {A C} and M Jardine and K Wood and Donati, {J F}",

year = "2003",

doi = "10.1051/eas:2003103",

language = "English",

isbn = "2-86883-646-1",

pages = "217--226",

editor = "J Arnaud and N Meunier",

booktitle = "MAGNETISM AND ACTIVITY OF THE SUN AND STARS",

publisher = "E D P Sciences",

note = "International Conference on Magnetism and Activity of the Sun and Stars ; Conference date: 17-09-2002 Through 21-09-2002",

}

TY - GEN

T1 - Stellar prominences and coronal magnetic fields

AU - Cameron, A C

AU - Jardine, M

AU - Wood, K

AU - Donati, J F

PY - 2003

Y1 - 2003

N2 - Rapidly rotating solar type stars display varying amounts of chromospheric emission in their Balmer lines. The profiles of these lines often display rapid variability. Since the mid-1980s, high-cadence echelle spectroscopy of numerous such stars has revealed that some of the variability is caused by concentrations of neutral hydrogen, trapped in the stellar coronal magnetic field at distances up to a few stellar radii from the rotation axis. In this paper we review the observations and the tomographic techniques that can be applied to mapping these "sling-shot prominence" systems. We discuss the possible mechanisms for formation and mechanical support of these condensations, in the light of recent efforts to map 3-dimensional stellar coronal magnetic fields and X-ray emission measure distributions, with the help of Zeeman-Doppler imaging.

AB - Rapidly rotating solar type stars display varying amounts of chromospheric emission in their Balmer lines. The profiles of these lines often display rapid variability. Since the mid-1980s, high-cadence echelle spectroscopy of numerous such stars has revealed that some of the variability is caused by concentrations of neutral hydrogen, trapped in the stellar coronal magnetic field at distances up to a few stellar radii from the rotation axis. In this paper we review the observations and the tomographic techniques that can be applied to mapping these "sling-shot prominence" systems. We discuss the possible mechanisms for formation and mechanical support of these condensations, in the light of recent efforts to map 3-dimensional stellar coronal magnetic fields and X-ray emission measure distributions, with the help of Zeeman-Doppler imaging.

U2 - 10.1051/eas:2003103

DO - 10.1051/eas:2003103

M3 - Conference contribution

SN - 2-86883-646-1

SP - 217

EP - 226

BT - MAGNETISM AND ACTIVITY OF THE SUN AND STARS

A2 - Arnaud, J

A2 - Meunier, N

PB - E D P Sciences

CY - CEDEX A

T2 - International Conference on Magnetism and Activity of the Sun and Stars

Y2 - 17 September 2002 through 21 September 2002

ER -

Stellar prominences and coronal magnetic fields

Abstract

Conference

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