Title: Wilcox Solar Observatory, Stanford
1- Wilcox Solar Observatory, Stanford
2Solar eclipse HawaiiJuly 1989
3The Sun!
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13Coronal Mass Ejections
14Coronal Mass Ejections
White light (SOHO/LASCO) solar limb coronagraph
image of CME. Inner corona and solar disk seen
in extreme ultraviolet (SOHO/EIT).
15The view from Earth
163D and twisted.
17CME Onset Due to Loss of Confinement of Twisted
Magnetic Flux Ropes
- What triggers coronal mass ejections (CMEs)?
This is a fundamental question in solar
astrophysics that must be answered for space
weather prediction. - Magnetic twist can drive eruption. A 3D
numerical simulation demonstrates that given
enough twist, a magnetic flux rope can no longer
be confined by the surrounding coronal magnetic
field and will erupt in a CME. - Twist in eruptions is observed. Twisted
internal structure and motion consistent with the
model has been observed in CMEs.
Observation of a CME by HAO Mauna Loa Solar
Observatory Mk4 white-light coronagraph
MHD Simulation from Fan (2005)
18Soft-X ray sigmoid brightening and associated
dimming
Fan and Gibson (in preparation)
Line-of-sight column integration of
Line-of-sight
- Looking down on flux rope we see it as it would
appear on the solar disk - Model predicts current sheets forming forward or
backwards S shapes (depending on direction of
flux rope twist) - X-ray observations show such S shapes
- Model predicts twin density depletions within
the S-shape (owl-eyes) - Observations sometimes show such twin dimmings
during eruptions
Line-of-sight column integration of
Soft-X ray image from Yohkoh satellite during the
onset of a CME
19Sigmoids
Sigmoids are generally visible in three ways
(Pevtsov, 2002)
persistent (long-lived)
transient (short-lived)
eruptive (transient sigmoid --gt cusp)
(Gibson et al., 2002)
20Magnetic flux rope observables X-ray sigmoids
- Sigmoid evolution -- evidence for flux rope
before, during and after eruption (Gibson et al.,
2004 2005)
eruptive (transient sigmoid --gt cusp)
persistent (long-lived)
transient (short-lived)
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