coronal mass ejections: from the sun to the earth
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Coronal Mass Ejections: from the Sun to the Earth. Consuelo Cid Space Research Group-Space Weather University of Alcala. Monthly Notices of the Royal Astronomical Society, Vol. 20, November 11, 1859. Magnetic Observations at Kew . - PowerPoint PPT PresentationTRANSCRIPT
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Coronal Mass Ejections: from the Sun to the Earth
Consuelo CidSpace Research Group-Space Weather
University of Alcala
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Interdisciplinary Workshop on Plasma Physics, Madrid (Spain), June 6-7 2011
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Monthly Notices of the Royal Astronomical Society, Vol. 20, November 11, 1859
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Magnetic Observations at Kew
Two responses seen in the new photographic recordings of magnetic variations being made at Kew (London)• Prompt response (due to X-rays increasing ionospheric ionization)• Great Magnetic Storm begins 18 hours later (due to associated emission reaching Earth)
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Solar mass ejections• Unmagnetized material
(Lindenmann, 1919)• A plasma cloud including
frozen-in magnetic field loops• Plasma including turbulent
magnetic fields• A “tongue” of magnetic field
loops rooted at the Sun• A disconnected “plasmoid” or
“bubble”• Shock wave ahead of a region
of enhanced turbulence ….• Flux rope (Burlaga, 1988)
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CMES AT THE SUNCoronal Mass Ejections: from the Sun to the Earth
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The first CME observed in 1860?
This early observation was not confirmed convincingly. However...
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The first CMEs observed in modern times: OSO 7 (1971) and Skylab (1973)
...the similarity with Skylab images obtained 113 years later is striking!
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This was the first published
‘modern‘ CME event,
observed 1971 from OSO 7
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CME? ...can’t tell what it is, but if I see it I know it...
What, actually, is a CME?Definition of terms: “A coronal mass ejection (CME) is … an observable change in coronal
structure that 1) occurs on a time scale of a few minutes and several hours and 2) involves the appearance (and outward motion) of a new, discrete, bright, white-light feature in the coronagraph field of view." (Hundhausen et al., 1984)
This definition is very fortunate in that• it emphasizes the observational aspect,• it stresses the transient event character,• it does not infer an interpretation of the "feature" and its potential origin,• in particular, it does NOT infer any conjunction with "coronal mass", • it restricts the applicability of the term to the Sun's proximity
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Just an example of what a CME is
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Some CMEs are spectacular, indeed!
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Properties of CMEs
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A unique observation by LASCO-C2.Note the helical structure of the prominence and filaments!
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The most popular astronomical picture in history: a huge prominence seen in the He+ line (30.4 nm), from Skylab (1973)
From that time in 1973 on, CMEs were an issue!
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The helical structure could just disappear because of 2D-projection on the plane of sky
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Full halo CMEs: ejections towards or away the Earth
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X-Ray or EUV images show coronal loops anchored in the photosfere
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Reconnection and CMEs
• Above CME• Release mechanism in
“breakout” model • Fast CMEs
• Below CME• Release mechanism in
“emerging flux” model• Slow CMEs
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Hight helicity: one of the clues for the “emerging flux” model
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Checking the “breakout model”: dimming at solar disk
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CMEs AT INTERPLANETARY MEDIUMCoronal Mass Ejections: from the Sun to the Earth
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Solar wind …and solar wind transients
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ICME signatures in solar wind
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The first ‘magnetic cloud’Burlaga et al., 1991
… and the topology proposed
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Note the 180º rotation of the
magnetic field direction through
the cloud!
Minimum Variance Analysis
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Are all ICME MCs?...
…the answer is still on debate
Today: Magnetic cloud = flux rope
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From 1D to 3D
… well, just 2D+1/2 D
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Force-free model (Burlaga, 98)
a=cte Lundquist (1950)
BB
a
0 0
0 1
( )( )
0
axial
azth
r
B B J rB B HJ rB
aa
ar
0
B0
Baz
Beje
2.4 0
Boundary: Baxial=0 aR=2.4
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MCs expand!Force-free?
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First non-force free MC modelPlasma and magnetic field inside magnetic clouds: a global study (Cid et al., 2001)
• The starting point:(0, , ), with , cte
0y y
r
j j j j r j
B a
• Analytical expressions:
2 20
2yB R r
a
0
2 yB j r
0rB
022224
20
24Pr jRrP
aa
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XGSE
YGSE
ZGSEXGSE
ZGSE
YGSE
y0
90ºq
f
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The model reproduced properly experimental data…
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.. but not for all MCs. Elliptical MCs
Elliptical cross-section model for the magnetic topology of magnetic clouds (Hidalgo, Nieves-Chinchilla and Cid, 2002)
It fits well... but many parameters need to be controlled
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Reconstruction of the cross section using Grad-Safranov equation
But MC boundaries are
difficult to be established
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Numerical simulations
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From the Sun to L1
• Experimental data and models do not agree systematicaly: only a few cases have been reproduced nowadays
• Where is the problem to be solved?…In the magnetic topology?…In the propagation through the solar wind?
… more work needed!
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The problem is still harder!
Complex ejecta,
multiMC…
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CMEs AT TERRESTRIAL ENVIRONMENT
Coronal Mass Ejections: from the Sun to the Earth
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At solar wind (L1)
At the terrestrial surface
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day of November 2003
1 6 11 16 21 26 31
Dst
(nT)
-500
-400
-300
-200
-100
0
100
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Energy injected from solar wind (Dungey, 1961): proportional to convective electric field (Ey=VBz)
ICMEs present large
values of V and B z
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* *( )dDst DstQ tdt
( ) 5.4t
Dst Q t dt Ey t
DPS relation: The decrease of the horizontal component of the geomagnetic field is proportional to the energy content of the ring current
From the energy balance in the ring current, it is possible to get the Dst index as a function of time
Neglecting losses (main phase):
Theoretical scenario
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t (h)
0 5 10 15 20 25 30
Ey (m
V/m
)
0
200
400
600
800
1000
I (nT
)
-400
-300
-200
-100
0
t (h)
0 5 10 15 20 25 30
(B z
) (nT
)
0
5
10
15
20
25
Cumulated Ey is not enought to explain the terrestrial disturbance for small t
… but theoretical expectations do not fit properly experimental data
Soon appearing in GRL…
Bz standard deviation is large for those events
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BE v B
t
Both, E convective and B/t, are related to the appearance of an induced E
Ey
Our results agree with Faraday law!
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The phenomena are complicated and without limit as we look to finer and finer detail. It is not our goal to pursue the endless detail; instead, we are interested in understanding what we observe in terms of the basic laws of physics. We want to know how the observed effects follow from Newton, Maxwell, Lorentz, Schorödinger, etc. We construct idealized and simplified theoretical models for the purpose of demonstrating how the basic laws of physics lead to a certain observed effect. We pursue detail only insofar as it leads to novel effects, in which the basic laws of physics interact in some new and hitherto unknown combination.”
Eugene N. Parker