Links to recent Solar Radio Science Highlights by Eduard Kontar

My many thanks to Dr. Eduard Kontar, University of Glasgow School of Physics and Astronomy,
and the Community of European Solar Radio Astronomers, for the following highlights.

About Dr. Eduard Kontar:
http://www.gla.ac.uk/schools/physics/staff/eduardkontar/

About CESRA:
http://www.astro.gla.ac.uk/users/eduard/cesra/?page_id=181

"The Community of European Solar Radio Astronomers (CESRA) is an informal organization of European
scientists to stimulate research of the outer solar atmosphere by means of radio waves and any
other suitable diagnostics."

"...CESRA publishes Highlights of Solar Radio Physics aka CESRA Nuggets approximately every two weeks at http://cesra.net. These short communications are written in the language accessible to a non-expert in the specific area and designed to keep solar and heliophysics communities informed and up-to-date about current research.
The highlights can be followed, discussed, commented and shared via
http://www.facebook.com/solarcesra/
http://twitter.com/CESRA_community    ..."

--------------------------------- 

An Extreme-ultraviolet Wave Generating Upward Secondary Waves in a
Streamer-like Solar Structure
by Ruisheng Zheng et al.*
http://cesra.net/?p=1925

Long-lasting injection of solar energetic electrons into the heliosphere
by N. Dresing et al.
http://cesra.net/?p=1916

Statistical Analysis of Solar Events Associated with storm sudden
commencements in the magnetosphere
by K. Bocchialini et al.*
http://www.astro.gla.ac.uk/users/eduard/cesra/?p=1895

Solar Radio Burst Associated with a Falling Bright EUV Blob
by M. Karlický et al.*
http://cesra.net/?p=1870

Properties of Decameter IIIb–III Pairs
by V. Melnik et al.*
http://cesra.net/?p=1875

Modeling of Solar Atmosphere Parameters Above Sunspots Using RATAN-600
Microwave Observations
by A.G. Stupishin et al.*
http://cesra.net/?p=1853

LOFAR observations of Fine Fundamental and Harmonic Structures in Solar
Radio Bursts
by Xingyao Chen et al*
http://cesra.net/?p=1848

Solar Type-IIIb Radio Bursts as Tracers for Electron Density
Fluctuations in the Corona
by V. Mugundhan et al.*
http://cesra.net/?p=1831

New evidence for a coronal mass ejection driven fast drifting type II
radio burst
by K. Ashnu et al.
http://cesra.net/?p=1818

Association of radio polar cap brightening with bright patches and
coronal holes
by C. L. Selhorst et al.*
http://cesra.net/?p=1807

Dressing the Coronal Magnetic Extrapolations of Active Regions with a
Parameterized Thermal Structure
by Gelu M. Nita et al.
http://cesra.net/?p=1798

Solar ALMA observations: constraining the chromosphere above sunspots
by M. Loukitcheva et al.*
http://cesra.net/?p=1777

Synergy of stochastic and systematic energization of plasmas during
turbulent reconnection
by Th. Pisokas, L. Vlahos and H. Isliker
http://cesra.net/?p=1773

The statistical relationship between global EUV waves and other solar
phenomena
by D. Long et al.*
http://cesra.net/?p=1763

Estimation of a CME magnetic field strength using observations of
gyrosynchrotron radiation
by E. P. Carley et al.*
http://cesra.net/?p=1701

Propagation and Interaction Properties of Successive Coronal Mass
Ejections in Relation to a Complex Type II Radio Burst
by Y. D. Liu et al.*
http://cesra.net/?p=1693

Observations of solar radio burst fine structures with LOFAR
by E. Kontar et al.*
http://cesra.net/?p=1675

VLA Measurements of Faraday Rotation through Coronal Mass Ejections
by Jason E. Kooi et al*
http://cesra.net/?p=1671

Solar Prominence Modelling at ALMA Wavelengths
by A. Rodger and N. Labrosse
http://cesra.net/?p=1647

Small electron acceleration episodes in the solar corona
by T. James et al.
http://cesra.net/?p=1635

Critical Fluctuations in Beam-Plasma Systems and Solar Type III Radio
Bursts
by G. Thejappa  and R. J. MacDowall
http://cesra.net/?p=1628

Acceleration and Storage of Energetic Electrons in Magnetic Loops in the
Course of Electric Current Oscillations
by V.V. Zaitsev and A.V. Stepanov
http://cesra.net/?p=1593

Flare SOL2012-07-06: on the origin of the circular polarization reversal
between 17 GHz and 34 GHz
by Altyntsev et al.*
http://cesra.net/?p=1578

Observations of a radio-quiet solar preflare
by A. Benz et al.*
http://cesra.net/?p=1562

Predicting Flares and Solar Energetic Particle Events: The FORSPEF Tool
by A. Anastasiadis et al.*
http://cesra.net/?p=1551

Exploring the potential of microwave diagnostics in SEP forecasting
by P. Zucca et al.
http://cesra.net/?p=1540

Solar plasma radio emission and inertial Alfven turbulence
by O. Lyubchyk et al.
http://cesra.net/?p=1525

EUV-invisible reservoir of solar energetic particles
by G. Fleishman et al..
http://cesra.net/?p=1499

Traveling Ionospheric Disturbances as Huge Natural Lenses: Solar Radio Emission Focusing Effect
by A. Koval et al.
http://cesra.net/?p=1480

Wavelet-based characterization of small-scale solar emission features at low radio frequencies
by A. Suresh et al.
http://cesra.net/?p=1473

Probing the Temperature Structure of the Solar Chromosphere with ALMA
by C. Alissandrakis et al.
http://cesra.net/?p=1457

Oscillation of solar radio emission at coronal acoustic cut-off frequency
by T. Zaqarashvili et al.
http://cesra.net/?p=1450

Siberian Radioheliograph: First Results
by S.V. Lesovoi et al.
http://cesra.net/?p=1426

The 30 cm solar radio flux: a new proxy for upper atmosphere specification
by Thierry Dudok de Wit and Sean Bruinsma
http://cesra.net/?p=1423

Particle acceleration and turbulence during a solar flare
by E.P. Kontar et al.
http://cesra.net/?p=1409

Solar wind density turbulence from 10 to 45 solar radii
by K. Sasikumar Raja et al.
http://cesra.net/?p=1385

Multi-Loop Structure of Nonthermal Microwave Sources in a Major Long-Duration Flare
by V. Grechnev et al.
http://cesra.net/?p=1375

Comparison of alternative zebra-structure models in solar radio emission
by G.P. Chernov et al.*
http://cesra.net/?p=1341

Microwave emission as a proxy of CME speed in ICME forecasting
by Carolina Salas Matamoros, Ludwig Klein and Gerard Trottet
http://cesra.net/?p=1336

The Brightness Temperature of the Quiet Solar Chromosphere at 2.6 mm
by Kazumasa Iwai et al
http://cesra.net/?p=1325

How Electron Beams Produce Continuous Coherent Plasma Emission
by H. Che, M. Goldstein, P. Diamond, and R. Sagdeev
http://cesra.net/?p=1310

Radio Diagnostics of Electron Acceleration Sites During the Eruption of a Flux Rope in the Solar Corona
by Eoin Carley et al.
http://cesra.net/?p=1188

Solar Science with the Atacama Large Millimeter/Submillimeter Array — A New View of Our Sun
by S. Wedemeyer
http://cesra.net/?p=1221

Quasi-periodic acceleration of electrons in the flare on 2012 July 19
by Jing Huang et al.
http://cesra.net/?p=1214

Large-scale simulations of Langmuir Wave Distributions Induced by Electron Beams
by H. Reid and E. Kontar
http://cesra.net/?p=1209

Full paper at:
"Langmuir Wave Electric Fields Induced by Electron Beams in the Heliosphere"
http://adsabs.harvard.edu/abs/2016arXiv161107901R
https://arxiv.org/pdf/1611.07901

Emission of radiation by plasmas with counter-streaming electron beams
by L. F. Ziebell et al.
http://cesra.net/?p=1200

Simultaneous near-Sun observations of a moving type IV radio burst
and the associated white-light CME
by K. Hariharan et al.
http://cesra.net/?p=1169

Observation of quasi-periodic solar radio bursts associated with propagating fast-mode waves
by C. R. Goddard et al.
http://cesra.net/?p=1159

Diagnosing the Source Region of a Solar Burst on 26 September 2011 by Using Microwave Type-III Pairs
by Tan B. L. et al.
http://cesra.net/?p=1138

Acceleration of electrons in the solar wind by Langmuir waves produced by a decay cascade
by Catherine Krafft and Alexander Volokitin
http://cesra.net/?p=1072

Source regions of the type II radio burst observed during a CME–CME interaction on 2013 May 22
by P. Mäkelä et al.
http://cesra.net/?p=1042

...

Titles of some Juno related papers submitted to Geophysical Research Letters

Selected from :

http://www-pw.physics.uiowa.edu/plasma-wave/juno/publications.html

Direction Finding Measurements of Jovian Broadband and Narrowband Kilometric Radiation From the Juno Waves Instrument Near Perijove 1

Latitudinal Beaming of Jovian Decametric Radio Emissions as Viewed From Juno and the Nançay Decameter Array

A New View of Jupiter's Auroral Radio Spectrum

Generation of the jovian hectometric radiation: first lessons from Juno

Electron butterfly distributions at particular magnetic latitudes observed during Juno’s perijove pass

Io-Jupiter decametric arcs observed by Juno/Waves compared to ExPRES simulations

Plasma waves in Jupiter's high latitude regions: Observations from the Juno spacecraft

Statistical study of latitudinal beaming of Jupiter's decametric radio emissions using Juno

Electron beams and loss cones in the auroral regions of Jupiter

-----------------------
Introductory Radio Astronomy references
http://herrero-radio-astronomy.blogspot.com/2015/06/introductory-radio-astronomy-references.html?m=1
Jupiter events at STEREO A for correlation with Juno Waves
http://herrero-radio-astronomy.blogspot.com/2016/12/jupiter-events-at-stereo-for.html
Links to Juno related posts
http://herrero-radio-astronomy.blogspot.com/2016/01/links-to-juno-related-posts.html?m=1
Sun Earth Jupiter event posts:
http://herrero-radio-astronomy.blogspot.com/2017/02/sun-earth-jupiter-20170223.html
http://herrero-radio-astronomy.blogspot.com/2015/08/links-to-monthly-sun-earth-jupiter-posts.html?m=1
Solar Cycle 24
https://en.wikipedia.org/wiki/Solar_cycle_24
"The Solar Cycle" by David Hathaway 2015, 81 pages
http://arxiv.org/pdf/1502.07020v1
Driel-Gesztelyi and Green 2015 "Evolution of Active Regions" 98 pages, 11 MB:
http://link.springer.com/content/pdf/10.1007%2Flrsp-2015-1.pdf
Links to recent Solar Radio Science Highlights by Eduard Kontar
http://herrero-radio-astronomy.blogspot.com/2017/02/links-to-recent-solar-radio-science.html
Solar Type Examples
http://herrero-radio-astronomy.blogspot.com/2015/07/solar-type-examples.html
Solar Dynamics Observatory - Now and Daily - Images Movies
http://sdo.gsfc.nasa.gov/data/
NOAA SWPC Solar Event reports with README description of their format
ftp://ftp.swpc.noaa.gov/pub/indices/events/
Preparation for Eclipse 170821
http://herrero-victor.blogspot.com/2016/10/preparation-for-eclipse-170821.html
-----------------------------

"Radio Emission from Red-Giant Hot Jupiters" Fujii et al. 2016

I refer to:

http://arxiv.org/abs/1601.05428

http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1601.05428

90 references in the paper :
http://adsabs.harvard.edu/cgi-bin/nph-ref_query?bibcode=2016ApJ...820..122F&refs=REFERENCES&db_key=AST

Abstract: "When planet-hosting stars evolve off the main sequence and go through the red-giant branch, the stars become orders of magnitudes more luminous and, at the same time, lose mass at much higher rates than their main-sequence counterparts. Accordingly, if planetary companions exist around these stars at orbital distances of a few au, they will be heated up to the level of canonical hot Jupiters and also be subjected to a dense stellar wind. Given that magnetized planets interacting with stellar winds emit radio waves, such “Red-Giant Hot Jupiters” (RGHJs) may also be candidate radio emitters. We estimate the spectral auroral radio intensity of RGHJs based on the empirical relation with the stellar wind as well as a proposed scaling for planetary magnetic fields. RGHJs might be intrinsically as bright as or brighter than canonical hot Jupiters and about 100 times brighter than equivalent objects around main-sequence stars. We examine the capabilities of low-frequency radio observatories to detect this emission and find that the signal from an RGHJ may be detectable at distances up to a few hundred parsecs with the Square Kilometer Array."

Coronal mass ejection triggering Jupiter X-ray aurora and non Io decametric radio emission, 2011 October 2-4

With many thanks, I refer to:

"The impact of an ICME on the Jovian X-ray aurora" Dunn et al. 2016:

http://onlinelibrary.wiley.com/doi/10.1002/2015JA021888/full

https://www.ucl.ac.uk/news/news-articles/0316/220316-Solar-storms-trigger-Jupiters-Northern-Lights

Abstract: "We report the first Jupiter X-ray observations planned to coincide with an interplanetary coronal mass ejection (ICME). At the predicted ICME arrival time, we observed a factor of ∼8 enhancement in Jupiter's X-ray aurora. Within 1.5 h of this enhancement, intense bursts of non-Io decametric radio emission occurred. Spatial, spectral, and temporal characteristics also varied between ICME arrival and another X-ray observation two days later. Gladstone et al. (2002) discovered the polar X-ray hot spot and found it pulsed with 45 min quasiperiodicity. During the ICME arrival, the hot spot expanded and exhibited two periods: 26 min periodicity from sulfur ions and 12 min periodicity from a mixture of carbon/sulfur and oxygen ions. After the ICME, the dominant period became 42 min. By comparing Vogt et al. (2011) Jovian mapping models with spectral analysis, we found that during ICME arrival at least two distinct ion populations, from Jupiter's dayside, produced the X-ray aurora. Auroras mapping to magnetospheric field lines between 50 and 70 RJ were dominated by emission from precipitating sulfur ions (S7+,…,14+). Emissions mapping to closed field lines between 70 and 120 RJ and to open field lines were generated by a mixture of precipitating oxygen (O7+,8+) and sulfur/carbon ions, possibly implying some solar wind precipitation. We suggest that the best explanation for the X-ray hot spot is pulsed dayside reconnection perturbing magnetospheric downward currents, as proposed by Bunce et al. (2004). The auroral enhancement has different spectral, spatial, and temporal characteristics to the hot spot. By analyzing these characteristics and coincident radio emissions, we propose that the enhancement is driven directly by the ICME through Jovian magnetosphere compression and/or a large-scale dayside reconnection event."

Temporal Evolution of the Vela Pulsar's Pulse Profile - Palfreyman et al.

I take note of this very interesting study:
   
Palfreyman, J. L.; Dickey, J. M.; Ellingsen, S. P.; Jones, I. R.; Hotan, A. W.,  February 2016 :

http://arxiv.org/abs/1602.01899

http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1602.01899

23 references at:
http://adsabs.harvard.edu/cgi-bin/nph-ref_query?bibcode=2016arXiv160201899P&refs=REFERENCES&db_key=PRE

 Abstract: "The mechanisms of emission and changes in rotation frequency ('glitching') of the Vela pulsar (J0835-4510) are not well understood. Further insight into these mechanisms can be achieved by long-term studies of integrated pulse width, timing residuals, and bright pulse rates. We have undertaken an intensive observing campaign of Vela and collected over 6000 hours of single pulse data. The data shows that the pulse width changes with time, including marked jumps in width after micro-glitches (frequency changes). The abundance of bright pulses also changes after some micro-glitches, but not all. The secular changes in pulse width have three possible cyclic periods, that match with X-ray periodicities of a helical jet that are interpreted as free precession." 

Detection possibilities of "Hot Jupiter" planets orbiting red giant stars, with very large radio telescope arrays

With many thanks, I refer to Fujii at al., 2016:

"Radio Emission from Red-Giant Hot Jupiters"

http://arxiv.org/abs/1601.05428

http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1601.05428

Abstract: "When planet-hosting stars evolve off the main sequence and go through the red-giant branch, the stars become orders of magnitudes more luminous and at the same time lose mass at much higher rates than their main-sequence counterparts. Accordingly, planetary companions around them at orbital distances of a few AU, if they exist, will be heated up to the level of canonical hot Jupiters and also subjected to a dense stellar wind. Given that magnetized planets interacting with stellar winds emit radio waves, such "Red-Giant Hot Jupiters" (RGHJs) may also be candidate radio emitters. We estimate the spectral auroral radio intensity of RGHJs based on the empirical relation with the stellar wind as well as a proposed scaling for planetary magnetic fields. RGHJs might be intrinsically as bright as or brighter than canonical hot Jupiters, and about 100 times brighter than equivalent objects around main-sequence stars. We examine the capabilities of low-frequency radio observatories to detect this emission and find that the signal from a RGHJ may be detectable at distances up to a few hundred parsecs with the Square Kilometer Array."

.
 

..
..

About the evolution of the Sun active regions

As the days go by, I frequently show details of active region magnetograms images and charts, and other data, for active regions I think may be suspect of initiating the radio events we study.

I started studying solar radio emission in 1966, I am not finished yet :)

The degree of activity frequently varies much from day to day and is a complex subject studied for many decades.

Lidia van Driel-Gesztelyi and Lucie May Green have published last month a "Living Review of Solar Physics" titled:

"Evolution of Active Regions" , 98 pages, including 17 pages of references, free to download at:

http://solarphysics.livingreviews.org/Articles/lrsp-2015-1/

http://solarphysics.livingreviews.org/Articles/lrsp-2015-1/download/lrsp-2015-1Color.pdf

Section 6 studies the case of AR 7978, "...subjected to the most comprehensive analysis of any AR..." as it evolved over a 6 month period.

Appendix A is a very good summary of Sunspot classifications, including the McIntosh and Hale methods.

I leave you repeating their quote from a poem by Laszlo Detre :

“  A Solar Physicist’s Lament  ....

It looks as if many a sunny day
Will pass along on its way
Before we solve it all...  "

My ignorance is vast
Have a wonderful day
Victor :)

--------------------------------
Solar Dynamics Observatory - Now and Daily - Images Movies
http://sdo.gsfc.nasa.gov/data/
Solar Type Examples
http://herrero-radio-astronomy.blogspot.com/2015/07/solar-type-examples.html
Comparison of Cycles 23 and 24 sunspot and coronal mass ejection numbers
http://3.bp.blogspot.com/-MxC1nf6CLuU/VcD2X3QT_kI/AAAAAAAALyg/n15qgyvN81g/s1600/W150804%2B50.png
http://sidc.oma.be/cactus/ CACTUS page
Introductory Radio Astronomy references
http://herrero-radio-astronomy.blogspot.com/2015/06/introductory-radio-astronomy-references.html?m=1
My recent event posts by month:
http://herrero-radio-astronomy.blogspot.com/2015/10/sun-earth-jupiter-20151001.html
http://herrero-radio-astronomy.blogspot.com/2015/09/sun-earth-jupiter-20150916.html
http://herrero-radio-astronomy.blogspot.com/2015/09/sun-earth-jupiter-2015-september.html
http://herrero-radio-astronomy.blogspot.com/2015/08/sun-earth-jupiter-2015-august.html
http://herrero-radio-astronomy.blogspot.com/2015/07/sun-earth-jupiter-2015-july.html
http://herrero-radio-astronomy.blogspot.com/2015/06/sun-earth-jupiter-2015-june.html
Links to earlier posts by month:
http://herrero-radio-astronomy.blogspot.com/2015/08/links-to-monthly-sun-earth-jupiter-posts.html?m=1
---------------------------------

Reference to a study of herringbones in Type II event on 2011 September 22 related to an X1.4 flare

With many thanks I refer to :

Carley Reid Vilmer Gallagher 2015, "Low frequency radio observations of bi-directional electron beams in the solar corona"

http://arxiv.org/abs/1508.01065

http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1508.01065

66 references at:
http://adsabs.harvard.edu/cgi-bin/nph-ref_query?bibcode=2015A%26A...581A.100C&refs=REFERENCES&db_key=AST
......

High Time and Frequency Resolution Capabilities of the Murchison Widefield Array - Pulsar observations

Dear Lovers of The Neutron Stars,

Thank you for your FUN work, it keeps me busy when the Sun and Jupiter do not keep me very busy :)

I sometimes wonder what happens at their very center, where temperatures and pressures are truly MONUMENTAL !!

Pulsars were discovered at 81.5 MHz about 50 years ago and I have been studying them since then.

Professor Tremblay at Curtin University in Perth Western Australia, and about 20 of his collaborators around the world, have been doing wonderful things working with the Murchison Widefield Array, a precursor of the Square Kilometer Array.

They have installed equipment to collect time domain data for a total of ~ 31 MHz bandwidth in ~ 1.3 MHz subbands, spread as desired, between 80 and 300 MHz, and observed 10 pulsars.

Read more about it here:

http://arxiv.org/abs/1501.05723

32 references at:
http://adsabs.harvard.edu/cgi-bin/nph-ref_query?bibcode=2015PASA...32....5T&refs=REFERENCES&db_key=AST


Abstract: "The science cases for incorporating high time resolution capabilities into modern radio telescopes are as numerous as they are compelling. Science targets range from exotic sources such as pulsars, to our Sun, to recently detected possible extragalactic bursts of radio emission, the so-called fast radio bursts (FRBs). Originally conceived purely as an imaging telescope, the initial design of the Murchison Widefield Array (MWA) did not include the ability to access high time and frequency resolution voltage data. However, the flexibility of the MWA's software correlator allowed an off-the-shelf solution for adding this capability. This paper describes the system that records the 100 micro-second and 10 kHz resolution voltage data from the MWA. Example science applications, where this capability is critical, are presented, as well as accompanying commissioning results from this mode to demonstrate verification."
....

A LOFAR Census of Millisecond Pulsars

With many thanks I refer to:

Kondratiev et al. 2015, "A LOFAR Census of Millisecond Pulsars"

http://arxiv.org/abs/1508.02948

http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1508.02948

Abstract: "We report the detection of 48 millisecond pulsars (MSPs) out of 75 observed thus far using the LOFAR in the frequency range 110-188 MHz. We have also detected three MSPs out of nine observed in the frequency range 38-77 MHz. This is the largest sample of MSPs ever observed at these low frequencies, and half of the detected MSPs were observed for the first time at frequencies below 200 MHz. We present the average pulse profiles of the detected MSPs, their effective pulse widths and flux densities, and compare these with higher observing frequencies. The LOFAR pulse profiles will be publicly available via the EPN Database of Pulsar Profiles. We also present average values of dispersion measures (DM) and discuss DM and profile variations. About 35% of the MSPs show strong narrow profiles, another 25% exhibit scattered profiles, and the rest are only weakly detected. A qualitative comparison of the LOFAR MSP profiles with those at higher radio frequencies shows constant separation between profile components. Similarly, the profile widths are consistent with those observed at higher frequencies, unless scattering dominates at the lowest frequencies. This is very different from what is observed for normal pulsars and suggests a compact emission region in the MSP magnetosphere. The amplitude ratio of the profile components, on the other hand, can dramatically change towards low frequencies, often with the trailing component becoming dominant. As demonstrated by Dyks et al. (2010) this can be caused by aberration and retardation. This data set enables high-precision studies of pulse profile evolution with frequency, dispersion, Faraday rotation, and scattering in the interstellar medium. Characterizing and correcting these systematic effects may improve pulsar-timing precision at higher observing frequencies, where pulsar timing array projects aim to directly detect gravitational waves."

Observations of Crab Giant Pulses in 20-84 MHz using LWA1

With many thanks, I refer to

Ellingson, S. W.; Clarke, T. E.; Craig, J.; Hicks, B. C.; Lazio, T. J. W.; Taylor, G. B.; Wilson, T. L.; Wolfe, C. N.  2013

http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1304.0812

33 references at:
http://adsabs.harvard.edu/cgi-bin/nph-ref_query?bibcode=2013ApJ...768..136E&refs=REFERENCES&db_key=AST

4 citations at:
http://adsabs.harvard.edu/cgi-bin/nph-ref_query?bibcode=2013ApJ...768..136E&refs=CITATIONS&db_key=AST

Abstract: "We report the detection and observed characteristics of giant pulses from the Crab Nebula pulsar (B0531+21) in four frequency bands covering 20-84 MHz using the recently completed Long Wavelength Array Station 1 (LWA1) radio telescope. In 10 hr of observations distributed over a 72 day period in fall of 2012, 33 giant pulses having peak flux densities between 400 Jy and 2000 Jy were detected. Twenty-two of these pulses were detected simultaneously in channels of 16 MHz bandwidth centered at 44 MHz, 60 MHz, and 76 MHz, including one pulse which was also detected in a channel centered at 28 MHz. We quantify statistics of pulse amplitude and pulse shape characteristics, including pulse broadening. Amplitude statistics are consistent with expectations based on extrapolations from previous work at higher and lower frequencies. Pulse broadening is found to be relatively high, but not significantly greater than expected. We present procedures that have been found to be effective for observing giant pulses in this frequency range."

.....

The decametric radio telescopes of Ukraine

With many thanks, I refer to Konovalenko et al. 2015 :

State-of-the-art of Low Frequency Radio Astronomy, Relevant Antenna Systems and International Cooperation in Ukraine

International Conference on Antenna Theory and Techniques, 21-24 April, 2015, Kharkiv, Ukraine

http://www.researchgate.net/publication/276273697_State-of-the-art_of_Low_Frequency_Radio_Astronomy_Relevant_Antenna_Systems_and_International_Cooperation_in_Ukraine

....