CMEs in Fukuoka Workshop
EventsNat Gopalswamy1, S. Yashiro1,2, S. Akiyama1,2, H. Xie1,2, and P. Mäkelä1,2
1NASA/GSFC
2The Catholic University of America

Solar Terrestrial Environment Workshop, Fukuoka, March 4, 2015

The Fukuoka Workshop Events: Overview• 2014 August 27 moderate storm (-85 nT) due to a slow CME• 2014 September 12 moderate storm (-75 nT) due to a fast halo CME
sheath; also associated with a large SEP event and an IP type II burst• CME-poor AR 12192 with 39 M+X flares, but only 9 CMEs (all small)• Hyder flare of 2014 November 1 (spotless flare, post-eruption arcade
following filament eruption). Fast CME and SEP event
Sunspotグラフ
タイトル• Context: 14 front-side halos 6/2014 to 12/2014
number• Relatively high SSN after the 2nd peak
120
100
80
60
40
200
2008

2009

2010

2011

2012

2013

2014

2015

2016

2014 August 27 Moderate Storm• 2014 August 22 Partial Halo seems to be the solar source• C2.2 flare from N12E01 (AR 12146)• Brief DH Type II (12-7 MHz)
• No SEP event• ICME, no shock2014 August 22 CME

N12E01

Partial Halo CME, Earth-directed

C2.2Flare2014 August 22 CME• Very slow CME (338 km/s)• True speed is expected to be ~560 km/s
• Width ~210o• Transit time ~ 112 h• Cloud-like ICME with high inclination (FS)• Bz = -15 nT, V = 310 km/s at 1 AU

ICME: High Inclination
EW rotation of B
Neutral line

Two-ribbon flare

BtBy

Bz
Vertical neutral line consistent with
FS-type ICME
Dst = 0.01VBz -32 nT= -78 nT
Gopalswamy, 2010

V = 310 km/s
Bz = -15 nTFSV
Dst-85 nT

20140912 Moderate Storm• Moderate geomagnetic storm (Dst = -75 nT)• CME on 9/10 (NOT 9/9)
• Large SEP Event (30 pfu, ESP – 100 pfu)
• Fast Halo CME (V ~1425 km/s ) and X1.6
flare from AR 12150• No metric type II burst listed, but possible• Intense IP type II• ICME (Omni2)• Good Sun-to-Earth event

e-CALLISTO ROSWELL NM

2014/09/09 CME caused just a sudden
impulseEjecta mostly to the east: glancing blow

N12E29
M4.5

The Storm-causing CME Occurred on
2004/09/10

N14E02
X1.6

The CME produced a large SEP event with ESP

30 pfu

100 pfuA 4000 pfu event behind the limb from thesame region?

Wind/WAVES Type II  Shock in the IPmedium

Shock at L1

Shock at Wind (L1) identified in the TNR data

Shock at Wind (L1) identified in SOHO proton monitor data

BzS in the shock
sheath; ICME field isalso of high inclination,
but north-pointing!

Bt
By
Bz
lowBetaBeta
V
SDO/HMIS1

S2

AIA 1600 A (CaIV)

The ribbons have a complex structure,
but the overall neutral line is north-south

Dst-75 nT

AR12192: CME-poor Flares• 39 M and X flares during the disk passage (between 10/16 and 11/1):
33 M-class flares and 6 X-class flares• 3 of the X-class flares (50%) had no CMEs
• In cycle 23, the largest X-class flare without CME was X1.2
• Now this size is X2.0
• Only 6 of the 33 M-class flares (18%) had CME association• The flares are extremely CME-poor (only 9/39 or 23%) had CMEs
• The CMEs were faint and narrow (low energy)• Only one CME was slightly fast and wide (2014/10/24)

The Corona above AR 12192

GONG PFSS Line of sightNine M+X flares from AR12192 were associated with CMEs

2014/10/24 CME
V=689 km/s; W=91oMetric Type IIburst

40

Type IIII

2014/10/24 CME associated with M4.0 Flare2014/10/22 X1.6 Flare - CMElessfpk = 15.4 GHz, 3700 sfu

Radio: only noise storm – unaffected by the flare2014/10/26 X2.0 Flare - CMElessfpk = 15.4 GHz, 2400 sfu

2014/10/27 X2.0 Flare - CMElessfpk = 15.4 GHz, 760 sfu

No Radio emission at f<14 MHz  no energetic electrons propagating away from the Sun

No CMENo CMENo CMEActive Region Area: Similar to AR 10486(Halloween 2003)
Gopalswamy et al. 2005 JGRAR12192

Hyder Flare 2014/11/01

Early Phase and Location

EP & CME

Post Eruption ArcadeSolar SourceC-class Flare but fast CME as in mostenergetic filament eruptions events with SEPs

Gopalswamy et al. 2015 ApJ

SEP Event?
CME

Other CMEs: Complex Event?

A very fast CME, accelerating….
Width = 150o