[radioastro] Solar wind control of Jovian hectometric radiation

From: Victor Herrero <hubbleed@xxxxxxxxx>
To: Marco Nicolini <heygio@xxxxxxxx>, Juan Fernando Tonatiuh Hernández Escobar <cecilixz@xxxxxxxxxxx>, Peter Hughes <PHughes@xxxxxxxxxx>, David Fields <fieldsde@xxxxxxx>, Steve McCauley <esmac@xxxxxxxxxx>, Dave Typinski <davetyp@xxxxxxxxxx>, "Whitham D. Reeve" <whitreeve@xxxxxxxxx>, Terrence Flower <tfflower@xxxxxxxxxx>, Jim Thieman <james.r.thieman@xxxxxxxx>, Divyadarshan Purohit <divyadarshan63@xxxxxxxxx>, Ramón Menéndez-Manjón <ramon.ramon.astronomers@xxxxxxxxx>, Tushar Sharma <sharma.tushar17@xxxxxxxxx>, "military.radioman" <samhevener@xxxxxxxxx>, Myamiphil <myamiphil@xxxxxxxxx>, danny garvin <grailknight_2@xxxxxxxxx>, Alfonso CastilloAbrego <cendap@xxxxxxxxxxx>, Thomas Ashcraft <ashcraft@xxxxxxxxxxxxx>, John Avellone <JGAVELLONE@xxxxxxx>, Arturo Garcia Cole <cole@xxxxxxxxxxxxxxxx>, Dalila Martinez <dmarti@xxxxxxxxxxxxxxxxx>, FRANCISCO BERSUNSES <siriober@xxxxxxxxxxx>, Steve Arnold <steve_arnold@xxxxxxxxxx>, Sajjad Mahdizadeh <sajjadea@xxxxxxxxx>, James H Van Prooyen <grro@xxxxxxxxxxxxx>, Cristian Leon Irribarra <celeon2@xxxxxxxxx>, "Karen & Jim Carson" <kjcarson@xxxxxxxxx>, Pablo Gonzalez <pablomgonzalez@xxxxxxxxxxxxx>, Clint Jeffrey <clintonjeffrey1@xxxxxxxxxxx>, Wanda Diaz <wanda@xxxxxxxxxxxxx>, Michael Rudolph <mrudolph@xxxxxxxxxxxxxxxxxxxxx>, Sead Kulenov <skulenov@xxxxxxxxx>, Neil Maron <neil.maron@xxxxxxxxx>, Wesley Greenman <greenman@xxxxxxxxxxxxx>, Jim Sky <radiosky@xxxxxxxxxxxx>, Salvador Aguirre <drsaguirre@xxxxxxxxx>, Abebe Kebede <abkebede@xxxxxxxxx>, Martin Wright <ducksuit@xxxxxxxxxxxxx>, Kibrom Yeibyo <kibromyeibyo@xxxxxxxxx>, Richard Flagg <rf@xxxxxxxxxxxxx>, _gloom_ gloom <_gloom_@xxxxxxx>
Date: Fri, 29 Oct 2010 23:36:48 -0700

Solar wind control of Jovian hectometric radiation

Hello Radio Astronomers,

I have read:
Galopeau and Boudjada 2005 "Solar wind control of Jovian auroral emissions"
:
http://adsabs.harvard.edu/abs/2005JGRA..11009221G
and following are some notes:

The study was based on data recorded in 1996 by WIND WAVES (near the Earth)
and Galileo PWS (orbiting the Jovian magnetosphere).

The highest probability regions are near CML 120 and 300 degrees (the B and
C regions, in the northern and southern magnetic hemispheres), with a peak
in intensity at about 1 MHz.
The morphology of the emission depends on the Jovicentric latitude of the
spacecraft.
The radiation is beamed in hollow cones.

HOM events are observed in sets, during periods of a few days, averaging
about 4 Jovian rotations.

The solar wind parameters were recorded by the WIND SWE Solar Wind
Experiment: flow speed, ion density, and temperature.

The best correlation index (60 %) is between the HOM radiation intensity and
the Solar wind flow speed, with a delay of 153 days.

"Further investigations must be made to understand, and possibly to predict,
how the solar particles can generate, directly or indirectly, such
disturbances and how they power the inner magnetosphere and also the
planetary equatorial regions."

Best regards,

Victor Herrero

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[radioastro] Solar wind control of Jovian hectometric radiation

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