Type III solar radio bursts in inhomogeneous interplanetary space observed by Geotail

Kasahara, Yoshiya; Matsumoto, Hiroshi; Kojima, Hirotsugu

doi:10.1029/2000rs002456

Cited by 3 publications

(2 citation statements)

References 12 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Type III SRBs are common radio transient emissions, which have been studied for more than 70 years. They are observed by instruments at frequencies ranging from kHz (Kasahara et al 2001) up to 7.6 GHz (Ma et al 2012). They are characterized by a fast drift from higher to lower frequencies over time .…”

Section: Type III Solar Radio Burstsmentioning

confidence: 99%

CALLISTO facilities in Peru: spectrometer commissioning and observations of type III solar radio bursts

Rengifo

Loaiza-Tacuri

Bazo

et al. 2021

Res. Astron. Astrophys.

View full text Add to dashboard Cite

The Astrophysics Directorate of CONIDA has installed two radio spectrometer stations belonging to the e-CALLISTO network in Lima, Peru. Given their strategic location near the Equator, it is possible to observe the Sun evenly throughout the whole year. The receiver located at Pucusana, nearby the capital city of Lima, took data from October 2014 until August 2016 in the metric and decimetric bands looking for radio bursts. During this period, this e-CALLISTO detector was unique in its time-zone coverage. To asses the suitability of the sites and the performance of the antennas, we analyzed the radio ambient background and measured their radiation pattern and beamwidth. To demonstrate the capabilities of the facilities for studying solar dynamics in these radio frequencies, we have selected and analyzed type III Solar Radio Bursts. The study of this kind of burst helps to understand the electron beams traversing the solar corona and the solar atmospheric density. We have characterized the most common radio bursts with the following mean values: a negative drift rate of –25.8 ± 3.7 MHz s−1, a duration of 2.6 ± 0.3 s and 35 MHz bandwidth in the frequency range of 114 to 174 MHz. In addition, for some events, it was possible to calculate a global frequency drift which on average was 0.4 ± 0.1 MHz s−1.

show abstract

Section: Type III Solar Radio Burstsmentioning

confidence: 99%

CALLISTO facilities in Peru: spectrometer commissioning and observations of type III solar radio bursts

Rengifo

Loaiza-Tacuri

Bazo

et al. 2021

Res. Astron. Astrophys.

View full text Add to dashboard Cite

show abstract

“…In the history of Japanese scientific spacecraft, the GEOTAIL mission is one of the most important projects investigating the phenomena in the earth's magnetosphere, by which so many new findings and paradigms were introduced by combining observation, computer simulations and theoretical studies. The WFC onboard SELENE is expected to clarify the detailed features of the wave phenomena observed by PWI instruments (Matsumoto et al, 1994a) on board the GEOTAIL spacecraft, such as Auroral Kilometric Radiation (AKR) (Murata et al, 1997;, nonthermal continuum and kilometric continuum (KC) (Hashimoto et al, 1999(Hashimoto et al, , 2005(Hashimoto et al, , 2006, continuum enhancement , low-frequency bursts (Anderson et al, 1997), electrostatic solitary wave (ESW) (Matsumoto et al, 1994b), narrowband electrostatic noise (NEN) , f p and 2 f p emissions (Kasaba et al, 2000), and solar radio emissions (Kasahara et al, 2001), among others. Emissions with frequencies higher than the maximum plasma frequency of the magnetosheath (about 30 kHz), such as AKR, KC, and continuum enhancement, and type II and III solar bursts are observed both inside and outside the magnetosphere.…”

Section: Scientific Objectivesmentioning

confidence: 99%

Plasma wave observation using waveform capture in the Lunar Radar Sounder on board the SELENE spacecraft

et al. 2008

Self Cite

View full text Add to dashboard Cite

The waveform capture (WFC) instrument is one of the subsystems of the Lunar Radar Sounder (LRS) on board the SELENE spacecraft. By taking advantage of a moon orbiter, the WFC is expected to measure plasma waves and radio emissions that are generated around the moon and/or that originated from the sun and from the earth and other planets. It is a high-performance and multifunctional software receiver in which most functions are realized by the onboard software implemented in a digital signal processor (DSP). The WFC consists of a fastsweep frequency analyzer (WFC-H) covering the frequency range from 1 kHz to 1 MHz and a waveform receiver (WFC-L) in the frequency range from 10 Hz to 100 kHz. By introducing the hybrid IC called PDC in the WFC-H, we created a spectral analyzer with a very high time and frequency resolution. In addition, new techniques such as digital filtering, automatic filter selection, and data compression are implemented for data processing of the WFC-L to extract the important data adequately under the severe restriction of total amount of telemetry data. Because of the flexibility of the instruments, various kinds of observation modes can be achieved, and we expect the WFC to generate many interesting data.

show abstract

Geotail Observations of Solar Wind and Interplanetary Phenomena

Terasawa

2005

Frontiers in Magnetospheric Plasma Physics - Celebrating 10 Years of Geotail Operation, Proceedings of the 16th COSPAR Colloqui

View full text Add to dashboard Cite

Type III solar radio bursts in inhomogeneous interplanetary space observed by Geotail

Cited by 3 publications

References 12 publications

CALLISTO facilities in Peru: spectrometer commissioning and observations of type III solar radio bursts

CALLISTO facilities in Peru: spectrometer commissioning and observations of type III solar radio bursts

Plasma wave observation using waveform capture in the Lunar Radar Sounder on board the SELENE spacecraft

Geotail Observations of Solar Wind and Interplanetary Phenomena

Contact Info

Product

Resources

About