M. J. ReinerM. J. ReinerM. J. Reiner, 1st STEREO Workshop, March, 2002, Paris

Radio Observations Associated Radio Observations Associated with Solar Transient Phenomenawith Solar Transient Phenomena

Dynamic Spectrum

ee-- acceleration at CME- acceleration at CME-driven shock frontsdriven shock frontsee-- beams from flare beams from flare

sitessites

OrigOriginin

intense, intense, continuouscontinuous

weak, weak, diffuse/sporadicdiffuse/sporadicwide frequency wide frequency

bandbandnarrow frequency narrow frequency bandband

fast frequency fast frequency driftdrift

slow frequency slow frequency driftdrift

Radiation Radiation CharacteristicsCharacteristics

flarflaree

CME

freq

uen

cy

time

Players in the Solar Players in the Solar Radio DramaRadio Drama

Intensity

M. J. Reiner, 1st STEREO Workshop, March, 2002, Paris

•• BothBoth generated by the plasma emission mechanism at frequency:f = fp(kHz) =

9÷n(cm-3)i.e., fundamental and/or harmonic of the plasma frequency

f = 2 fp(kHz)

or

fifi

fifi Explains the observed Explains the observed frequency driftfrequency drift

Radio emissions remotely Radio emissions remotely measuremeasureplasma density in source plasma density in source regionregion•• Plasma density decreases with increasing Plasma density decreases with increasing

heliocentric distanceheliocentric distance

M. J. Reiner, 1st STEREO Workshop, March, 2002, Paris

confined confined beam/beam/radio radio sourcesource

wide wide beam/beam/radio radio sourcesource

e-

e-

e-e-

e-flareflare

iso-density contour (iso-frequency

contour)100 kHz

shock front

M. J. Reiner, 1st STEREO Workshop, March, 2002, Paris

Study Study characteristics of characteristics of electron beams electron beams

andandtopological topological

structure of the structure of the IMFIMF

Study evolution Study evolution and dynamics of and dynamics of

CMEs,CMEs,Sun to EarthSun to Earth

M. J. Reiner, 1st STEREO Workshop, March, 2002, Paris

UlysseUlyssess Use radio Use radio

direction-finding direction-finding to get line-of-to get line-of-sight source sight source direction at each direction at each observing observing frequencyfrequencyUse density law Use density law to determine to determine radio source radio source location along location along line of site at line of site at each frequencyeach frequency

fifi Radio source centroid Radio source centroid follows Archimedean follows Archimedean spiral pathspiral path

Radio direction-Radio direction-finding from finding from

Ulysses gives 2-Ulysses gives 2-D trajectory D trajectory

without using a without using a density modeldensity model

M. J. Reiner, 1st STEREO Workshop, March, 2002, Paris

• Two s/c triangulation can give the 3-D radio source trajectory, without the need for a density model

(simultaneous radio source direction-finding from two widely separated s/c)

• plasma density profile along type III trajectory• “true” radio source intensity• radiation propagation times M. J. Reiner, 1st STEREO Workshop, March, 2002, Paris

Source region & electron beam Source region & electron beam characteristicscharacteristics

W

E

N

S

540 kHz

Wind(deg)

(deg)

Azimuth (deg)

Log(sfu)

e-

e-e-e-e-e-

e-

sourceregion

e-

e-e-e-

e-e-

e-

sourceregion

exciter longitudinal

velocity gradient

e- exciters arrive simultaneously at source region

W

E

M. J. Reiner, 1st STEREO Workshop, March, 2002, Paris

Lift off of CMEs and type II events Lift off of CMEs and type II events are usually preceded by very are usually preceded by very intense intense (violent),(violent), complex type III complex type III emissionsemissions

These complex type These complex type IIIs have unusual IIIs have unusual characteristics in characteristics in

the the 1 to 15 MHz band1 to 15 MHz band

• diminution in intensity near 7 MHz• very narrow band features below 7 MHz

10:20 10:25 10:30 10:35 10:40 10:45 10:50 10:55 11:00

1.075

3

5

7

9

11

13

Time(UT)

4.00

6.25

8.50

M. J. Reiner, 1st STEREO Workshop, March, 2002, Paris

f = 9÷nn ~ 1/R2 f ~

1/R

1/f

time

1/f ~ R = (v1/f ~ R = (vss /9 /9 ÷nnoo)(t - )(t - ttoo))

CMEs propagate at ~ CMEs propagate at ~ constant speed through constant speed through IPMIPM

(CME) liftoff(CME) liftofftime,ttime,too

CME Dynamics & Evolution: 1/f trackingCME Dynamics & Evolution: 1/f tracking

harmonic emissionfundamental emission

Dynamic SpectrumDynamic Spectrum

fifi

Radio emissions Radio emissions organized along straight organized along straight lines from solar originlines from solar origin

vvss = shock = shock speedspeedttoo = liftoff = liftoff timetime

M. J. Reiner, 1st STEREO Workshop, March, 2002, Paris

Knowing the shock speed at 1 AU and by Knowing the shock speed at 1 AU and by fitting the radio frequency drift, we get the fitting the radio frequency drift, we get the

“true” height & speed profile of the CME “true” height & speed profile of the CME from Sun to 1 AUfrom Sun to 1 AU

R

M. J. Reiner, 1st STEREO Workshop, March, 2002, Paris

White-light images at White-light images at consecutive timesconsecutive times Type II radio emissions at Type II radio emissions at

decreasing frequencydecreasing frequency

Measure height Measure height vs. timevs. time

Measure frequency Measure frequency driftdrift

€€

€€

Plane-of-sky Plane-of-sky height & speed height & speed of CMEof CME

Coronal Coronal density density profile can profile can be measuredbe measured

““true” (radial) true” (radial) height & speed of height & speed of radio sourceradio source

Coronal density Coronal density profile “unkown”profile “unkown”

€€

€€

M. J. Reiner, 1st STEREO Workshop, March, 2002, Paris

20 January 200120 January 2001

Consistency between White-Light & Radio ObservationsConsistency between White-Light & Radio Observations

E90o

Flare site ≈ N7Flare site ≈ N7ooE46E46oo

E47o

Radial propagation from 47Radial propagation from 47oo ±± 3 3ooE (“launch angle”) E (“launch angle”)

flare

fifiM. J. Reiner, 1st STEREO Workshop, March, 2002, Paris

Radio Measurements•• Radio dynamic spectra (intensities) from two Radio dynamic spectra (intensities) from two

viewpointsviewpoints•• 3-D radio source location routinely deduced 3-D radio source location routinely deduced by triangulationby triangulation•• In-situ e- beams, Langmuir waves and Local In-situ e- beams, Langmuir waves and Local radiationradiation New and unique

physics•• Intrinsic nature & characteristics of type II & III Intrinsic nature & characteristics of type II & III sourcesource•• Evolution & dynamics of solar transient Evolution & dynamics of solar transient phenomenaphenomena

•• Characteristics of e- beams related to radio Characteristics of e- beams related to radio emissionsemissions

•• Remote radio probing of interplanetary plasma Remote radio probing of interplanetary plasma propertiesproperties

•• true source true source intensitiesintensities

•• propagation time & propagation time & effectseffects

•• beaming beaming effectseffects

•• direct 3-D tracking of radio sources from direct 3-D tracking of radio sources from Sun to EarthSun to Earth•• relationship of radio sources to white-relationship of radio sources to white-light featureslight features

•• plasma density profiles along radio source plasma density profiles along radio source trajectoriestrajectories•• global 3-D reconstruction of IMF from global 3-D reconstruction of IMF from active regionsactive regions

•• exciter speed exciter speed profilesprofiles•• relation to Langmuir waves & relation to Langmuir waves & local radiationlocal radiation

•• injection times & path injection times & path lengthslengths

•• relationship of radio source region to relationship of radio source region to interplanetary structuresinterplanetary structures

M. J. Reiner, 1st STEREO Workshop, March, 2002, Paris