J/ApJ/891/79 Single storms and the related ICMEs from 1998-2011 (Li+, 2020)
Stronger southward magnetic field and geoeffectiveness of ICMEs containing
prominence materials measured from 1998 to 2011.
Li D., Yao S.
<Astrophys. J., 891, 79 (2020)>
=2020ApJ...891...79L 2020ApJ...891...79L
ADC_Keywords: Sun; Magnetic fields
Keywords: Solar coronal mass ejections ; Solar prominences ; Space weather ;
Geomagnetic fields
Abstract:
Interplanetary coronal mass ejections (ICMEs) could be classified into
magnetic clouds (MCs) and non-MCs according to their magnetic field
signatures, and into prominence-inside ICMEs (PIs) and non-PIs based
on whether they contain colder and higher helium abundance plasmas
than the solar wind. It is known that the MCs often lead to magnetic
storms. However, whether or not the PIs have significant
geoeffectiveness is unclear. This statistical work studies the
southward interplanetary magnetic field (IMF) magnitude of the PIs,
and the related magnetic storms' level. The data include the IMF and
plasma moments measured by ACE and WIND, and the Dst index from 1998
to 2011. The hypothesis test based on the proportions of two groups is
used to analyze 95 ICMEs related to single storms (SSs). The results
show that the magnetic storms caused by the PIs mostly distribute at a
strong level, while that caused by the non-PIs and by all the 95 ICMEs
mostly distribute at a moderate level. The PIs have a significantly
higher probability of generating SSs than the non-PIs. Moreover, the
MCs containing carbon-cold and helium-enhanced materials (MC&PIs) have
the highest fraction of minimum Bz, less than -11 nT. Since the MC&PIs
have large-scale magnetic flux rope and prominence material, the
stronger southward IMF is probably provided by the prominence. It is
in accordance with the observed injection of enhanced twisted flux
ropes to prominence. Therefore, the detailed eruption and propagation
processes of the three-part coronal mass ejections deserve more
concern from a space weather perspective.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 89 95 Single storms and the related interplanetary
coronal mass ejections (ICMEs) selected
from Feng+ 2018, J/ApJ/868/124
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See also:
J/A+A/440/373 : Earthbound interplanetary shocks (Howard+, 2005)
J/ApJ/709/1238 : Solar Coronal Mass Ejection (Yeates+, 2010)
J/ApJ/737/L35 : Pulsed Alfven waves in the solar wind (Gosling+, 2011)
J/ApJ/759/69 : Solar electron events, 1995-2005 with WIND/3DP (Wang+, 2012)
J/MNRAS/456/1542 : Predicting CMEs transit times (Sudar+, 2016)
J/ApJ/831/105 : Global energetics of solar flares. IV. CME (Aschwanden, 2016)
J/ApJ/868/124 : ICMEs events from 1998 to 2011 with ACE and WIND (Feng+, 2018)
J/ApJS/239/12 : Small-scale magnetic flux ropes in the solar wind (Hu+, 2018)
J/ApJ/871/93 : Solar wind speed from ACE spacecraft (Wang+, 2019)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Seq [2/219] The ICME sequence number
from Feng+, 2018, J/ApJ/868/124
5- 14 A10 "Y/M/D" St.date ICME start date (UT)
16- 20 A5 "h:m" St.time ICME start time
22 A1 --- MC Magnetic clouds? (Y)es or (N)o
24 A1 --- CC Carbon Cold? (Y)es or (N)o
26 A1 --- HE Helium enhanced? (Y)es or (N)o
28- 33 F6.2 nT BzMin [-45.6/-3.11] Magnetic field z component minimum
35- 44 A10 "Y/M/D" Main.date Main phase start date (UT)
46- 50 A5 "h:m" Main.time Main phase start time
52- 61 A10 "Y/M/D" Min.date Dst index minimum date (UT)
63- 67 A5 "h:m" Min.time Dst index minimum time
69- 78 A10 "Y/M/D" Rec.date Recovery phase end date (UT)
80- 84 A5 "h:m" Rec.time Recovery phase end time
86- 89 I4 nT DstMin [-422/-30] Dst index minimum value (1)
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Note (1): The Dst index represents the horizontal magnetic field variation
caused by an enhanced ring current during the storm
(Sugiura 1964nepb.conf...49S). And its minimum value is used to
estimate the storm intensity. See Section 1.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 06-Aug-2021