The source region of an interplanetary type II radio burst

Bale, S. D.; Reiner, M. J.; Bougeret, Jean‐Louis; Kaiser, M. L.; Krucker, S.; Larson, D. E.; Lin, R. P.

doi:10.1029/1999gl900293

Cited by 204 publications

(230 citation statements)

References 13 publications

(15 reference statements)

Supporting

Mentioning

211

Contrasting

Unclassified

Order By: Relevance

“…Reiner et al (1998a) has suggested that the intermittent nature of type II emissions implies multiple, distinct emission regions. It has also been shown with both remote sensing (Reiner et al 1998a(Reiner et al , 1998b and in situ observations (Bale et al 1999) that the source region of type II emission lies upstream of CME-driven shock fronts. Taken together, these observations suggest that type II emission is generated in multiple foreshock regions upstream of IP shocks.…”

Section: Introductionmentioning

confidence: 99%

“…The in situ terrestrial foreshock has been extensively studied by many spacecraft. In contrast, only one in situ IP foreshock region has been described in the literature (Bale et al 1999). In this section, we will review the basic characteristics of electron acceleration and Langmuir wave generation at the terrestrial foreshock, and outline our analogous measurements upstream of IP shocks.…”

Section: Introductionmentioning

confidence: 99%

“…The event described by Bale et al (1999) was the first observed in situ measurement of a type II radio burst. We have examined the data set of IP shocks observed by the Wind spacecraft, searching for additional events.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Structure on Interplanetary Shock Fronts: Type II Radio Burst Source Regions

Pulupa

Bale

2008

ApJ

Self Cite

View full text Add to dashboard Cite

We present in situ observations of the source regions of interplanetary ( IP) type II radio bursts, using data from the Wind spacecraft during the period 1996-2002. We show the results of this survey, as well as in-depth analysis of several individual events. Each event analyzed in detail is associated with an interplanetary coronal mass ejection (ICME ) and an IP shock driven by the ICME. Immediately prior to the arrival of each shock, electron beams along the interplanetary magnetic field (IMF ) and associated Langmuir waves are detected, implying magnetic connection to a quasi-perpendicular shock front acceleration site. These observations are analogous to those made in the terrestrial foreshock region, indicating that a similar foreshock region exists on IP shock fronts. The analogy suggests that the electron acceleration process is a fast Fermi process, and this suggestion is borne out by loss cone features in the electron distribution functions. The presence of a foreshock region requires nonplanar structure on the shock front. Using Wind burst mode data, the foreshock electrons are analyzed to estimate the dimensions of the curved region. We present the first measurement of the lateral, shock-parallel scale size of IP foreshock regions. The presence of these regions on IP shock fronts can explain the fine structure often seen in the spectra of type II bursts. Subject headingg s: interplanetary medium -solar-terrestrial relations -Sun: coronal mass ejections (CMEs) -Sun: radio radiation

show abstract

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Structure on Interplanetary Shock Fronts: Type II Radio Burst Source Regions

Pulupa

Bale

2008

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

“…ripples in the shock surface [Bale et al, 1999], in which case, parts of the shock magnetically connected to the upstream region need not have the same 0B,• as at the shock crossing. This is also likely due to the shock being curved (even without ripples) or to B varying in space.…”

Section: B• ~ 860 At the Crossing) These Observations Implymentioning

confidence: 99%

Theory of type II radio emission from the foreshock of an interplanetary shock

Knock¹,

Cairns²,

Robinson³

et al. 2001

J. Geophys. Res.

148

View full text Add to dashboard Cite

“…Of particular interest are observations of radio events that follow solar flares and coronal mass ejections (CMEs). Type II solar radio bursts, for example, are associated with radio emission produced near the local plasma frequency (f p ) and its harmonic (2f p ) upstream of a traveling shock wave, itself often driven ahead of a CME [Wild et al, 1963;Cane et al, 1981Cane et al, , 1987Reiner et al, 1998;Bale et al, 1999;Knock et al, 2001].…”

Section: Introductionmentioning

confidence: 99%

Prediction of background levels for the Wind WAVES instrument and implications for the galactic background radiation

et al. 2010

View full text Add to dashboard Cite

[1] We investigate and predict the observed background levels for the TNR, RAD1, and RAD2 receivers when connected to the X, Y, and Z antennas of the WAVES instrument on the spacecraft Wind. The receivers are connected to either a single antenna, in "SEP" mode, or a combination of antennas, in "SUM" mode. With the TNR receiver in SEP (X) mode, the predicted backgrounds agree to within 20% when modeled using a two component model for the quasi-thermal plasma noise (QTN). Calibrating the RAD1 in SEP (X) mode observations against TNR allows us to calculate the relative receiver gain G R1 = 1.43 ± 0.18. Using the RAD1 data in SUM (X+Z) mode, the ratio of antenna gains is found to be R = 6.5, in agreement with preflight measurements. Observed differences between the SEP (X) and SUM (X+Z) modes are explained for the first time, and the predicted levels of QTN and galactic background are found to agree to within 20%. RAD2 is also calibrated against RAD1 and TNR, yielding a total gain G R2 G y = 2.5 ± 0.3. Differences between the predicted and observed galactic background spectra are used to estimate the effective antenna lengths for the X and Y antennas, which are found to be between the physical monopole antenna length L and the Hansen (1981) prediction of ffiffiffiffiffiffiffiffiffiffiffi ð2=3Þ p L. The analyses are consistent with the Novaco and Brown (1978) galactic background model, which decreases much faster than that of Cane (1979). Our model background spectrum is useful for theory-data comparisons of type II and III bursts.

show abstract

The source region of an interplanetary type II radio burst

Cited by 204 publications

References 13 publications

Structure on Interplanetary Shock Fronts: Type II Radio Burst Source Regions

Structure on Interplanetary Shock Fronts: Type II Radio Burst Source Regions

Theory of type II radio emission from the foreshock of an interplanetary shock

Prediction of background levels for the Wind WAVES instrument and implications for the galactic background radiation

Contact Info

Product

Resources

About