solar radio emission - reuven ramaty high energy solar ... · • radio astronomers express flux...
TRANSCRIPT
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Solar Radio Emission
T. S. BastianNRAO
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UX Ari
18 Nov 1995
VLBA
8.4 GHz
1035 – 1036 erg
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Plan• Preliminaries• Emission mechanisms
- Gyro-emissionthermal gyroresonancenonthermal gyrosynchrotron
- Thermal free-free emission- Plasma emission
• Solar radio phenomenology
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PreliminariesNot surprisingly, the emission and absorption of EM waves is closely related to the natural frequencies of the material with which they interact.
In the case of a plasma, we encountered three frequencies:
Electron plasma frequency νpe ≈ 9 ne1/2 kHz
Electron gyrofrequency νBe ≈ 2.8 B MHz
Electron collision frequency νc « νpe, νBe
These correspond to plasma radiation, gyroemission, and “free-free” or bremsstrahlung radiation.
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2
222
ωckn = 2
pe
ω=Ω
o30=θRefractive index
Whistler
z mode
ordinary mode
extraordinary mode
Wave modes supported by a cold,magnetized plasma
2222 3 thvkp
+= ωω
2222 ckp
+= ωω
2
22 1
ωω pn −= (unmagnetized plasma)
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Charge with constant speed suddenly brought to a stop in time Δt.
tv
ΔΔ
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The radiation power is given by the Poynting Flux (power per unit area: ergs cm-2 s-1 or watts m-2)
2
44Ecc
ππ=×= HES
23
2222
2 4sinsin
4 rcvq
rcvqc
πθθ
π&&
=⎟⎠⎞
⎜⎝⎛=S
3
22
32
cvqP&
=• Proportional to charge squared
• Proportional to acceleration squared
• Dipole radiation pattern along acceleration vector
Intuitive derivation will be posted with online version of notes.
Power emitted into 4π steradians
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GyroemissionGyroemission is due to the acceleration experienced by an electron as it gyrates in a magnetic field due to the Lorentz force. The acceleration is perpendicularto the instantaneous velocity of the electron.
When the electron velocity is nonrelativisitic (v<<c or γ-1<<1) the radiation pattern is just the dipole pattern.
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Since the electron motion perpendicular to the magnetic field is circular, it experiences a constant acceleration perpendicular to its instantaneous velocity:
⊥⊥ = Va Beν
This can be substituted in to Larmor’s Eqn to obtain
223
2
32
perpBeVceP ν=
In fact, this expression must be modified in when the electron speed is relativistic (i.e., near c):
2243
2
32
perpBeVceP νγ= mc
eBBe γ
ν =
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When the electron is relativistic (v~c or γ>>1) we have, in the rest frame of the electron
'23
22
sin4'
'Θ=
Ω cvq
ddP
π&
which, when transformed into the frame of the observer
⎥⎦
⎤⎢⎣
⎡−
−−
=Ω 22
22
43
22
)1(cossin1
)1(1
4 βμγφθ
βμπcvq
ddP &
Strongly forward peaked!
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What this means is that an observer sees a signal which becomes more and more sharply pulsed as the electron increases its speed (and therefore its energy).
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For a nonrelativistic electron, a sinusoidally varying electric field is seen which has a period 2π/ΩBe,
And the power spectrum yields a single tone (corresponding to the electron gyrofrequency).
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As the electron energy increases, mild beaming begins and the observed variation of the electric field with time becomes non-sinusoidal.
The power spectrum shows power in low harmonics(integer multiples) of the electron gyrofrequency.
Gyroemission at low harmonics of the gyrofrequency is called cyclotron radiation or gyroresonance emission.
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When the electron is relativistic the time variation of E is highly non-sinusoidal…
and the power spectrum shows power in many harmonics.
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A detailed treatment of the spectral and angular characteristics of electron gyroemission requires a great deal of care.
A precise expression for the emission coefficient that is valid for all electron energies is not available. Instead, expression are derived for various electron energy regimes:
Non-relativistic: γ-1<<1 (thermal)
cyclotron or gyroresonance radiation
Mildly relativisitic: γ-1~1-5 (thermal/non-thermal)
gyrosynchrotron radiation
Ultra-relativisitic: γ-1>>1 (non-thermal)
synchrotron radiation
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Synchrotron radiation is encountered in a variety of sources. The electrons involved are generally non-thermal and can often be parameterized in terms of a power law energy distribution:
dECEdEEN δ−=)(In this case, we have
21
)(−
−∝
δ
ννP
when the source is optically thin and
2/5)( νν ∝Pwhen the source is optically thick (or self absorbed).
τ << 1
τ >> 1
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Thermal gyroresonance radiation
• Harmonics of the gyrofrequency
• Two different modes, or circular polarizations (σ=+1 o-mode, σ=-1 x-mode)
• Typically, s = 2 (o-mode), s = 3 (x-mode)
Hz 108.22
6 sBcm
eBsse
B ×===π
νν
2122
02222/5
, )cos1(2sin
!2
2θσθβ
ννπα −⎟⎟
⎠
⎞⎜⎜⎝
⎛⎟⎠⎞
⎜⎝⎛=
−sp
OXs
ss
c
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from Lee et al (1998)
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from J. Lee
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Thermal free-free radiationNow consider an electron’s interaction with an ion. The electron is accelerated by the Coulomb field and therefore radiates electromagnetic radiation.
In fact, the electron-ion collision can be approximated by a straight-line trajectory with an impact parameter b. The electron experiences an acceleration that is largely perpendicular to its straight-line trajectory.
Ze
-e
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For a thermal plasma characterized by temperature T, the absorption coefficient is
ffkTh
ieff gennZT
kmmhce )1(
32
34 322/1
2/16 ν
ν νππα−−− −⎟
⎠⎞
⎜⎝⎛=
In the Rayleigh-Jeans regime this simplifies to
ffie
ff gnnZTkmmkc
e 222/32/16
32
34 −−⎟
⎠⎞
⎜⎝⎛= νππαν
ffie
ff gnnZT 222/3 018.0 −−= ναν
where gff is the (velocity averaged) Gaunt factor.
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222/3 −−∝ ναν eff nTThen we have
and so 222/3 L)( −−∝= νατ νν effff nTL
The quantity ne2L is called the column emission measure.
Notice that the optical depth τff decreases as the temperature T increases and/or the column emission measure decreases and/or the frequency ν increases.
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A brief aside
• Radio astronomers express flux density in units of Janskys
• Solar radio physics tends to employ solar flux units (SFU)
• While specific intensity can be expressed in units of Jy/beam or SFU/beam, a simple and intuitive alternative is brightness temperature, which has units of Kelvin.
1 Jy = 10-26 W m-2 Hz-1
1 SFU = 104 Jy
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Planck function
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Note that at radio wavelengths
kTh
kThekThv kTh ννν =−+≈−→<< 111 1/ /
The Planckian then simplifies to the Rayleigh-Jeans Law.
kTcec
hTB kTh 2
2
/2
3 21
12)( νννν ≈
−=
It is useful to now introduce the concept of brightness temperature TB, which is defined by
BB kTc
TBI 2
22)( ννν ==
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Similarly, we can define an effective temperature Teff:
effkTc
jS 2
22ναν
νν ==
And rewrite the RTE in the formThe radiative transfer equation is written
νννν α jI
dsdI
+−=
which describes the change in specific intensity Iν along a ray. Emission and absorption are embodied in αν and jν, respectively. The optical depth is defined through dτν = ανds and the RTE can be written
ννν
ν
τSI
ddI
+−=
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TTT effB ==
LnTTT eff
B222/1 −−∝= ντν
1>>ντ
1<<ντ
For a homogeneous source it has the solution
)1( ντ−−= eTT effB
Recall that
effBB TT
ddT
+−=ντ
Using our definitions of brightness temperature and effective temperature, the RTE can be recast as
Brightness temperature is a simple and intuitive expression of specific intensity.
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Sun at 17 GHz
Nobeyama RH
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17 GHz
B gram
SXR
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• A magnetic field renders a plasma “birefringent”
• The absorption coefficient for the two magnetoionicmodes, x and o, is
• The x-mode has higher opacity, so becomes optically thick slightly higher in the chromosphere, while o-mode is optically thick slightly lower
• Degree of circular polarization
Λ+
⎟⎠⎞
⎜⎝⎛=
∑2/32/1
24
2
22/1
, )(
4
)cos(312
kTm
nZe
ci
ii
B
pox
π
θσννν
πα
LR
LRc TT
TT+−
=ρ
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Free-Free Opacity
No B
x-modeTx
o-mode
To
lB
C B∝= θννβρ cos
νβ
lnln
dTd
=
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Gelfriekh 2004
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Plasma radiation
Plasma oscillations (Langmuir waves) are a natural mode of a plasma and can be excited by a variety of mechanisms.
In the Sun’s corona, the propagation of electron beams and/or shocks can excite plasma waves.
These are converted from longitudinal oscillations to transverse oscillation through nonlinear wave-wave interactions.
The resulting transverse waves have frequencies near the fundamental or harmonic of the local electron plasma frequency: i.e., νpe or 2νpe.
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Plasma radiation
Plasma radiation is therefore thought to involve several steps:
Fundamental plasma radiation
• A process must occur that is unstable to the production of Langmuir waves
• These must then scatter off of thermal ions or, more likely, low-frequency waves (e.g., ion-acoustic waves)
TSL ωωω =+
TSL ωωω += TSL kkk +=
TSL kkk =+and
or
coalescence
decay
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Plasma radiationPlasma radiation is therefore thought to involve several steps:
Harmonic plasma radiation
• A process must occur that is unstable to the production of Langmuir waves
• A secondary spectrum of Langmuir waves must be generated
• Two Langmuir waves can then coalesce
TLL ωωω =+ 21LTLL kkkk <<=+ 21and
21LL kk −≈LT ωω 2≈
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“Classical” radio bursts
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type II radio burst
SA type III radio bursts
WIND/WAVES and Culgoora
More examples: http://www.nrao.edu/astrores/gbsrbs
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Lin et al. 1981
ISEE-3 type III
1979 Feb 17IP Langmuir
waves
IP electrons
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Lin et al. 1981
ISEE-3 type III
1979 Feb 17
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Statistical study of spectral properties of dm-cm λ radio
bursts
Nita et al 2004
• Sample of 412 OVSA events (1.2-18 GHZ)
• Events are the superposition of cm-λ (>2.6 GHz) and dm-λ (<2.6 GHz) components
• Pure C: 80%; Pure D: 5%; Composite CD: 15%
• For CD events: 12% (<100 sfu); 19% (100-1000 sfu); 60% (>1000 sfu)
• No evidence for harmonic structure
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from Nita et al 2004
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from Benz, 2004
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Long duration flare observed on west limb by Yohkoh and the Nobeyamaradioheliograph on 16 March 1993.
Y. Hanaoka Aschwanden & Benz 1997
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Isliker & Benz 1994
Reverse slope type IIIdm radio bursts
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Aschwanden et al. 1992
Type U bursts observed by Phoenix/ETH and the VLA.
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Long duration flare observed on west limb by Yohkoh and the Nobeyamaradioheliograph on 16 March 1993.
Y. HanaokaAschwanden & Benz 1997
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Gyrosynchrotron Radiation
Ramaty 1969
Benka & Holman 1992
Petrosian 1981
Dulk & Marsh 1982, 1985
Klein 1987
“exact” approximate
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e.g., Klein (1987)
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A Schematic Model
Bas
tian
et a
l 199
8
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B=300 G
Nrel=107 cm-3
θ=45o
Nth=1010
δ=3
x mode
o mode
For positive magnetic polarity, x-mode radiation is RCP and o-mode is LCP
s ~ 10s – 100s νBe
νBe = 2.8 B MHz
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B=100 G
B=200 G
B=500 G
B=1000 G
Νpk ~ B 3/4
ην ~ B2.5
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Nrel=1 x 107 cm-3
Nrel=5 x 106 cm-3
Nrel=2 x 106 cm-3
Nrel=1 x 106 cm-3
νpk~ Nrel1/4
ην ~ Nrel
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θ=20o
θ=40o
θ=60o
θ=80oνpk~ θ1/2
ην ~ θ3/2
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Nth=1 x 1011 cm-3
Nth=5 x 1010 cm-3
Nth=2 x 1010 cm-3Nth=1 x 1010 cm-3
Razin suppression
νR~20 Nth/Bperp
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1993 June 3
Lee, Gary, & Shibasaki 2000Trap properties
OVSA/NoRH
A comparison of successive flares yielded trap densities of 5 x 109 cm-3 in the first, and 8 x 1010 cm-3 in the second.
Anisotropic injectionLee & Gary 2000
Showed that the electron injection in the first flare was best fit by a beamed pitch angle distribution.
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1999 August 28
Yokoyama et al 2002
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17 GHz intensity 17 GHz circ. pol. 34 GHz intensity
Magnetic field lines in the solar corona illuminated by gyrosynchrotronemission from nonthermal electrons.
Nobeyama RH
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2/3−∝∝ EED νν
TPP/DP Model
from Aschwanden 1998
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Kundu et al. 2001
1998 June 13
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Bastian et al 1998
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White et al 20021999 May 29
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1993 June 3 OVSA
Lee & Gary 2000
μo=0
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Melnikov et al 2002
beam
isotropic
pancake
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Gyrosynchrotronradiation from
anisotropic electrons
Fleishman & Melnikov 2003a,b
Properties of the emitted radiation – e.g., intensity, optically thin spectral index, degree of polarization –depend sensitively on the type and degree of electron anisotropy
η = cos θ
QT QP
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“Collapsing trap”Karlický & Kosugi 2004
Model electron properties near “footpoint”
• Analysis of betatron acceleration of electrons due to relaxation of post-reconnection magnetic field lines.
• Energies electrons and producers highly anisotropic distribution
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Observations of Radio emission from flares
• Access to nonthermal electrons throughout flaring volume: magnetic connectivity
• Sensitive to electron distribution function and magnetic vector, ambient density and temperature
• Observations over past decade have clarified relation of microwave-emitting electrons to HXR-emitting electrons: FP, LT, spectral properties
• Recent work has emphasized importance of particle anisotropies
Need an instrument capable of time-resolved broadband imaging spectroscopy to fully exploit radio diagnostics!
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20 April 1998
C2 C2
C3
C3
10:04:51 UT 10:31:20 UT
10:45:22 UT
11:49:14 UT
SOHO/LASCO
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Bastian et al. (2001)
Noise storm
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Bastian et al. (2001)
300.335 x 1052212.8-1.074
1900.696.5 x 106219.52.40.033
2651.031.35 x 107218.52.050.542
3301.472.5 x 1072341.451.811
LoS α Rsun φ (deg) ne (cm-3) B(G) νRT (MHz)
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2465 km/s
Core1635 km/s
1925 km/s
see Hudson et al. 2001 Gopalswamy et al 2004
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Ionosphericcutoff
Spa
ce b
ased
Gro
und
base
d type IV
type III
type II
Dulk et al. 2001
Culgoora
WIND/WAVES
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Observations of Radio emission from CMEs
• Unique access to the nascent stages of CMEs
• Sensitive to both gyrosynchrotron (leading edge) and thermal (core) emission
• Provides means of measuring speed, acceleration, width etc.
• Can also measure B (CME), nth (CME), nrel (CME), nth (core), T (core)
Need an instrument capable of time-resolved broadband imaging spectroscopy to fully exploit radio diagnostics!
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Larmor FormulaFor the time being, we are going to consider continuum emission mechanisms, deferring emission and absorption in spectral lines until later.
We are therefore going to ignore radiation processes involving atomic and molecular transitions and instead think about radiation from free charges.
A derivation of radiation from free charges is somewhat involved. I’m just going to sketch out the underlying physical ideas using a simple derivation due to J.J Thomson.
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First, consider a charged particle q moving at some velocity v from left to right. It is suddenly brought to a stop at point x at time t=0; I.e., it is decelerated.
Alternatively, a charge can be accelerated. We’ll analyze this case…
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θΔv t Δv
Δvt sin θ
r=ct
cΔt
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The ratio of the perpendicular component of the electric field to the radial component is
tctv
EE
r ΔΔ
=θθ sin
from Coulomb’s Law. Since r=ct, we can substitute and rearrange terms to get
2rqEr =and
2sinsin rc
vqc
ttv
rctqE θθ
θ&
=ΔΔ
=
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Note that Er is proportional to 1/r2, while Eθ is proportional to 1/r, so Eθ>> Er far from the charge q.
The radiation power is given by the Poynting Flux (power per unit area: ergs cm-2 s-1 or watts m-2)
2
44Ecc
ππ=×= HES
Substituting our expression for Eθ for E, we obtain
23
2222
2 4sinsin
4 rcvq
rcvqc
πθθ
π&&
=⎟⎠⎞
⎜⎝⎛=S
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The power pattern is determined by the factor sin2θ, which yields a “donut” (dipole pattern) whose axis is coincident with the vector along which the charge was accelerated.
To compute the total radiation power P produced by the accelerated charge, we integrate over the sphere of radius r:
θθθθπ
π
θ
π
φ
d sinr r sin4
0
2
2
03
22
drc
vqdASP ∫∫∫∫==
==&
3
22
0
33
22
32d sin
2 cvq
cvqP
&&== ∫
=
θθπ
θ
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The last expression is called Larmor’s Equation. Note that the power is proportional to the square of the charge and the square of the acceleration.