Abstract
| Language | English |
|---|---|
| Pages | 102-108 |
| Number of pages | 7 |
| Journal | Monthly Notices of the Royal Astronomical Society |
| Volume | 329 |
| Issue number | 1 |
| Early online date | 1 Jan 2002 |
| DOIs | |
| Publication status | Published - 2002 |
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Keywords
- stars activity
- late type stars
- magnetic fields
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Can late-type active stars be explained by a dipole magnetic trap? / Kellett, B.J.; Bingham, R.; Cairns, R.A.; Tsikoudi, V.
In: Monthly Notices of the Royal Astronomical Society, Vol. 329, No. 1, 2002, p. 102-108.Research output: Contribution to journal › Article
TY - JOUR
T1 - Can late-type active stars be explained by a dipole magnetic trap?
AU - Kellett, B.J.
AU - Bingham, R.
AU - Cairns, R.A.
AU - Tsikoudi, V.
PY - 2002
Y1 - 2002
N2 - In this paper we review four different types of X-ray and/or radio observations of active late-type stars. We then consider if a single magnetic source configuration – a toroidal dipole magnetic trap – can possibly explain these various different observations. We conclude that, indeed, dipole magnetic confinement (similar to the magnetic configurations of the Earth's radiation belts and the case of Jupiter and the Io torus) can explain all the diverse observational data. We take this to be very strong observational support for this type of magnetic confinement scheme. We also consider that this magnetic configuration is only likely to be established and maintained in the most active stars.
AB - In this paper we review four different types of X-ray and/or radio observations of active late-type stars. We then consider if a single magnetic source configuration – a toroidal dipole magnetic trap – can possibly explain these various different observations. We conclude that, indeed, dipole magnetic confinement (similar to the magnetic configurations of the Earth's radiation belts and the case of Jupiter and the Io torus) can explain all the diverse observational data. We take this to be very strong observational support for this type of magnetic confinement scheme. We also consider that this magnetic configuration is only likely to be established and maintained in the most active stars.
KW - stars activity
KW - late type stars
KW - magnetic fields
U2 - 10.1046/j.1365-8711.2002.04972.x
DO - 10.1046/j.1365-8711.2002.04972.x
M3 - Article
VL - 329
SP - 102
EP - 108
JO - Monthly Notices of the Royal Astronomical Society
T2 - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
SN - 0035-8711
IS - 1
ER -