# Presentation: 830277

## M. J. Reiner

**M. J. Reiner**

- Solar Radio Observations

- Relationships to:

- White-Light Observations

- In-Situ Plasma Data

- Evolutionary
- and
- Source Region Models

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

## Dynamic Spectrum

**Radio Observations Associated with Solar Transient Phenomena**

- e- acceleration at CME-driven shock fronts

- e- beams from flare sites

- Type III radio emissions

- Type II radio emissions

**Origin**

**intense, continuous**

**weak, diffuse/sporadic**

**wide frequency band**

**narrow frequency band**

**fast frequency drift**

**slow frequency drift**

**Radiation Characteristics**

**flare**

**CME**

**frequency**

**time**

**Players in the Solar Radio Drama**

**Intensity**

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

## fi

**•**** ****Both**** ****generated by the plasma emission mechanism at frequency:**

***f  =  f******p******(kHz)  =  9******÷******n(cm******-3******)***

***i.e., fundamental and/or harmonic of the plasma frequency***

***f  =  2  f******p******(kHz)***

***or***

***fi***

***fi***

**Explains the observed frequency drift**

**Radio emissions remotely measure**
**plasma density in source region**

**•**** ****Plasma density decreases with increasing heliocentric distance**

- Type III radio emissions                     Type II radio emissions

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

## confined beam/

- Type III radio emissions

- Type II radio emissions

**confined beam/**
**radio source**

**wide beam/**
**radio source**

***flare***

***iso-density contour***

***(iso-frequency contour)***
***100 kHz***

***shock front***

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

## Type III radio emissions

- Type II radio emissions

***Study characteristics of electron beams ***
***and***
***topological structure of the IMF***

***Study evolution and dynamics of CMEs,***
***Sun to Earth***

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

## Ulysses

**Ulysses**

**Use radio direction-finding to get line-of-sight source direction at each observing frequency**

**Use density law to determine radio source location along line of site at each frequency**

***fi***

**Radio source centroid follows Archimedean spiral path**

***Radio direction-finding from Ulysses gives 2-D trajectory without using a density model***

- IMF Topology

- Remote Type III Observations

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

## Wind/Ulysses (Stereo) Triangulation

***•****** ******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, 1****st**** STEREO Workshop, March, 2002, Paris**

## Source region & electron beam characteristics

***Source region & electron beam characteristics***

***exciter longitudinal velocity gradient***

***e******-****** exciters arrive simultaneously at source region***

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

## Bastille Day Event 2000

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

***These complex type IIIs have unusual characteristics in the ***
***1 to 15 MHz band***

***•****** ****** ******diminution in intensity near 7 MHz***

***•******  ******very narrow band features below 7 MHz***

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

## fi

***f   =  9******÷******n***

***n  ~  1/R******2***

***f  ~  1/R***

**1/f**

**time**

***1/f  ~  R = (v******s****** /9 ******÷******n******o******)(t - t******o******)***

***CMEs propagate at ~ constant speed through IPM***

**(CME) liftoff**
**time,t****o**

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

***harmonic emission***

***fundamental emission***

**Dynamic Spectrum**

***fi***

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

***v******s****** = shock speed***

***t******o****** = liftoff time***

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

## Knowing the shock speed at 1 AU and by fitting the radio frequency drift, we get the “true” height & speed profile of the CME from Sun to 1 AU

- Constraints on CME Dynamics & Evolution by
-  Simultaneous In-situ and Radio Observations

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

## White-light images at consecutive times

***Type II radio emissions at decreasing frequency***

- white-light

- Radio

**Measure height vs. time**

***Measure frequency drift***

- Comparison of Radio/White-Light Observations

**€**

**€**

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

**Coronal density profile can be measured**

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

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

**€**

**€**

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

## fi

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

**E90****o**

**Flare site ≈ N7****o****E46****o**

**E47****o**

**Radial propagation from 47****o**** ****±**** 3****o****E (“launch angle”) **

- Constraints Imposed on CME Dynamics by
-  Simultaneous White-Light and Radio Observations

***flare***

***fi***

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

## • Intrinsic nature & characteristics of type II & III source

- Radio Measurements

**•**** ****Radio dynamic spectra (intensities) from two viewpoints**

**•**** ****3-D radio source location routinely deduced by triangulation**

**•**** ****In-situ e- beams, Langmuir waves and Local radiation**

- New and unique physics

**•**** *****Intrinsic nature & characteristics of type II & III source***

**•**** *****Evolution & dynamics of solar transient phenomena***

**•**** *****Characteristics of e- beams related to radio emissions***

**•**** *****Remote radio probing of interplanetary plasma properties***

**•**** ****true source intensities**

**•**** ****propagation time & effects**

**•**** ****beaming effects**

**•**** ****direct 3-D tracking of radio sources from Sun to Earth**

**•**** ****relationship of radio sources to white-light features**

**•**** ****plasma density profiles along radio source trajectories**

**•**** ****global 3-D reconstruction of IMF from active regions**

**•**** ****exciter speed profiles**

**•**** ****relation to Langmuir waves & local radiation**

**•**** ****injection times & path lengths**

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

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