Magnetic Clouds
A magnetic cloud is a transient ejection in the solar wind defined by relatively strong magnetic fields, a large and smooth
rotation of the magnetic field direction over approximately 0.25AU at 1AU, and a low proton temperature [Burlaga et al., 1981].
Magnetic clouds are ideal objects for solar-terrestrial studies because of their simplicity and their extended intervals of southward
and northward magnetic fields [Burlaga et al., 1990].
The figure summarizes the following:
- A flux rope magnetic cloud model, in which it was assumed that the internal magnetic tension and compression forces
were in balance, was successfully applied to the October 1995 WIND event to obtain the size and orientation of a large local volume
of the cloud from observations along only a single path through it; see Burlaga et al., 1996.
- The model and related analyses confirmed that a cloud had a dominant magnetic field which acted like a huge
magnetosphere departing the Sun, stretched out in the ecliptic plane, and having its own 'bow shock' ('driven' shock).
- The cloud's front and rear boundaries and the driven shock were locally analyzed and shown to be strongly related
geometrically to the estimated cloud-axis.
- The internal 'shock' may be due to a stream ramming into the rear of the cloud, but the orientation of the shock is
unexpected.
- A magnetic storm occurred in the Earth's magnetosphere due to the passage of the strong southward fields in the
early part of the magnetic cloud.
Interval #1 of the First Inter Agency Consultative Group Science Campaign was October 18-21, 1995, which foruitously
encompasses this October 1995 magnetic cloud and related events observed by WIND. Many space science teams are working
on various aspects of this magnetic cloud, its possible solar origin, and its effects on the Earth's magnetosphere, e.g., see Lepping et al., 1997.
Magnetic Cloud Table
MAGNETIC CLOUDS AS DETERMINED BY MFI DATA - PRELIMINARY
The table consists of estimated start and end times, as designated,
and physical quantities that were estimated by a magnetic field model
[Lepping et al., 1990] that assumes that the
field within the magnetic cloud is force free, i.e., so that the electrical
current and the magnetic field are parallel and proportional in strength
everywhere within its volume. The angles PHI and THETA refer to the
estimated direction of the cloud's axis, where PHI is a longitude and
THETA is a latitude in GSE coordinates. Dia. is the diameter (in AU) of the
magnetic cloud, assumed circular in cross-section, based on model results and
the radial speed of the solar wind provided by the WIND SWE instrument
(K. W. Ogilvie, PI). B is the model-estimated magnetic field for the axis
of the cloud. We point out that the spacecraft rarely encounters the actual
axis, but passes above or below at various closest approach (CA) distances
that are also estimated by the model (not shown explicitly here - but see
CA% below.) |CHI| is actually chi/(3N-5), based on the reduced chi-squared value, which is the usual
chi-squared divided by (3N-n), where N is the number of points (usually hour averages) used in
the model fitting and n is fixed at 5 which is the number of parameters
fitted up to this time; two other parameters are fitted later in the process, making
it a 7 parameter model. H represents helical field handedness, right- or
left-handed. CA% means the ratio of CA distance of the spacecraft to the
cloud's axis to the cloud's radius, expressed in percentage. F is the
magnetic flux along the axis of the magnetic cloud estimated by the flux
rope model of Lepping et al.(1990), where F = 1.36 BR**2, and where R = Dia/2.
Version date: 04/23/03
----|----START--TIME----|------END--TIME----|-------------------ESTIMATED(MODEL)---------------------------------------------
| | | |
| | | |
YR | MON Day(DOY) HR | MON Day(DOY) HR | DT* PHI THETA V** Dia | B H |CHI| asf% [QUAL+] CA%& F# Figures Ref
| | | (deg)(deg) (km/s) (AU) | (nT)
| | | |
95 | Feb 8 (039) 03 | Feb 8 (039) 22 | 20 92 6 410 0.224 | 14.2 L .0167 25.0 [1] 34 5.5 f1 f2
| | | |
95 | Mar 4 (063) 11 | Mar 5 (064) 04 | 18 205 -82 443 0.190 | 14.4 L .0296 12.2 [2] 52 3.9 f1 f2
| | | |
95 | Apr 6 (096) 07 | Apr 6 (096) 18 | 12 147 65 334 0.096 | 14.7 L .0194 11.7 [2] 76 1.0 f1 f2
| | | |
95 | May 13 (133) 10.1 | May 13 (133) 15.8 | 5.7 107 -3 331 0.165 | 20.5 L .0088 3.2 [3] 98 4.3 f1 f2
| | | |
95 | Aug 22 (234) 22 | Aug 23 (235) 19 | 22 268 4 360 0.233 | 11.8 R .0137 14.5 [1] 35 4.9 f1 f2
| | | |
95 | Oct 18 (291) 19 | Oct 20 (293) 00 | 30 289 -10 404 0.249 | 25.6 R .0141 3.3 [1] 8 12.7 f1 f2