Selling an Idea or a Product

1
Photospheric Sources of Very Fast (gt1000km/s)
Coronal Mass Ejections
Vasyl Yurchyshyn, Big Bear Solar Observatory,
40386 North Shore Lane, Big Bear City, CA 92314
email vayur_at_bbso.njit.edu, http//www.bbso.njit.
edu/vayur
SHINE
We identified photospheric sources of 39 very
fast CMEs and we distinguished three different
groups of active regions with specific magnetic
configurations i) complex delta spots ii)
simple tadpole-shaped delta spots and iii)
magnetic complexes.
1. CME projection speed seem to be related to
the Bz in IMF
1. Complex Delta Spots (11 - X, 8 - M 2 C
flare)
Is magnetic complexity crucial for production of
a fast CME? Yes Is reconnection required to
produce a fast CME? Yes
Date Speed Coord NOAA
Area Length Flare
Pre-flare Configuration
F1
The M7.9 Flare in NOAA AR 9415 on April 9th, 2001
PFL
The hourly averaged Bz at the front of an ejecta
(ACE, GSM) vs the projected speed of CMEs. Solid
line is an exponential fit (F1)
BznT12.30.7exp(V/404). (r.m.s7nT)
MC at 1AU
CME near the Sun
CME
Post-flare Configuration
2. In turn, the Bz in IMF defines the intensity
(the Dst Index) of a storm
2. Tadpole-Shaped ARs (2 - X, 5 - M 1 C
flare)
Reconnection of many twisted magnetic field loops?
Date Speed Coord NOAA
Area Length Flare
3. Magnetic Complex (1- X, 8 - M 1 C flare)
Date Speed Coord NOAA
Area Length Flare
The Dst index plotted vs the hourly averaged Bz.
The solid line is a 3rd degree polinominal fit,
F2, and the dashed lines show r.m.s33nT.
It seems that only fast CMEs capable of
producing strong geomagnetic storms. If so, where
these fast CMEs originate?
Interaction of two (or more) active regions?