Post by cinsinus1 on Feb 12, 2007 16:37:44 GMT -5
Dear friends,
I collected some natural sound fragments from our solar system. Especially Satrun represents the omega energy (gate to be a perfect human or a salvation gate. The old Egyptian were used Ankh for supplying themselves with Omega energy which is work like a spirit in its ring and provide only the useful energies.
With Love
cinsinus
*** These are the "sounds of space" collected by U Iowa instruments on various spacecraft.
www-pw.physics.uiowa.edu/space-audio/index.html
www-pw.physics.uiowa.edu/space-audio/Iowa10-2002.html
www.jpl.nasa.gov/multimedia/sounds/index-flash.html
Satrun
www-pw.physics.uiowa.edu/cassini/
www.nasa.gov/mission_pages/cassini/multimedia/pia07966.html à
www.nasa.gov/wav/123163main_cas-skr1-112203.wav
Saturn is a source of intense radio emissions, which have been monitored by the Cassini spacecraft. The radio waves are closely related to the auroras near the poles of the planet. These auroras are similar to Earth's northern and southern lights. This is an audio file of radio emissions from Saturn.
The Cassini spacecraft began detecting these radio emissions in April 2002, when Cassini was 374 million kilometers (234 million miles) from the planet, using the Cassini radio and plasma wave science instrument. The radio and plasma wave instrument has now provided the first high resolution observations of these emissions, showing an amazing array of variations in frequency and time. The complex radio spectrum with rising and falling tones, is very similar to Earth's auroral radio emissions. These structures indicate that there are numerous small radio sources moving along magnetic field lines threading the auroral region.
Time on this recording has been compressed, so that 73 seconds corresponds to 27 minutes. Since the frequencies of these emissions are well above the audio frequency range, we have shifted them downward by a factor of 44.
The Cassini-Huygens mission is a cooperative project of NASA, the European Space Agency and the Italian Space Agency. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter was designed, developed and assembled at JPL. The radio and plasma wave science team is based at the University of Iowa, Iowa City.
www.nasa.gov/mission_pages/cassini/multimedia/pia07967.html à
www.nasa.gov/wav/123160main_cas-skr2-072504.wav
Saturn is a source of intense radio emissions, which have been monitored by the Cassini spacecraft. The radio waves are closely related to the auroras near the poles of the planet. These auroras are similar to Earth's northern and southern lights. This is an audio file of Saturn's radio emissions.
The Cassini spacecraft began detecting these radio emissions in April 2002, when Cassini was 374 million kilometers (234 million miles) from the planet, using the Cassini radio and plasma wave science instrument.
The instrument has now provided the first high resolution observations of these emissions, showing that show an amazing array of variations in frequency and time. In this example, it appears as though the three rising tones are launched from the more slowly varying narrowband emission near the bottom of this display. If this is the case, it represents a very complicated interaction between waves in Saturn's radio source region, but one which has also been observed at Earth.
Time on this recording has been compressed such that 13 seconds corresponds to 27 seconds. Since the frequencies of these emissions are well above the audio frequency range, we have shifted them downward by a factor of 260.
The Cassini-Huygens mission is a cooperative project of NASA, the European Space Agency and the Italian Space Agency. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter was designed, developed and assembled at JPL. The radio and plasma wave science team is based at the University of Iowa, Iowa City.
cassini.physics.uiowa.edu/space-audio/cassini/SKR1/ à
cassini.physics.uiowa.edu/space-audio/cassini/SKR1/SKR-03-324.wav
Saturn is a source of intense radio emissions. The radio waves are closely related to the auroras near the poles of the planet. These auroras are similar to Earth's northern and southern lights. The Cassini spacecraft began detecting these radio emissions in April 2002 when Cassini was 2.5 astronomical units from the planet using the Cassini Radio and Plasma Wave Science (RPWS) instrument. The RPWS has now provided the first high resolution observations of these emissions that show an amazing array of variations in frequency and time. The complex radio spectrum with rising and falling tones is very similar to Earth's auroral radio emissions. These structures indicate that there are numerous small radio sources moving along magnetic field lines threading the auroral region.
The sound of the radio emissions can be heard by clicking on the button labeled "Audio" or in an animated version (which shows a cursor that indicates time on the spectrogram) by clicking on "Animate." Time on this recording has been compressed such that 73 seconds corresponds to 27 minutes, or, the recording is at 22x real time. Since the frequencies of these emissions are well above the audio frequency range, we have shifted them downward by a factor of 44.
cassini.physics.uiowa.edu/space-audio/cassini/SKR2/ à
cassini.physics.uiowa.edu/space-audio/cassini/SKR2/casskrtrig04207a.wav
Saturn is a source of intense radio emissions. The radio waves are closely related to the auroras near the poles of the planet. These auroras are similar to Earth's northern and southern lights. The Cassini spacecraft began detecting these radio emissions in April 2002 when Cassini was 2.5 astronomical units from the planet using the Cassini Radio and Plasma Wave Science (RPWS) instrument. The RPWS has now provided the first high resolution observations of these emissions that show an amazing array of variations in frequency and time. In this example, it appears as though the three rising tones are launched from the more slowly varying narrowband emission near the bottom of this display. If this is the case, it represents a very complicated interaction between waves in Saturn's radio source region, but one which has also been observed at Earth!
The sound of the radio emissions can be heard by clicking on the button labeled "Audio" or in an animated version (which shows a cursor that indicates time on the spectrogram) by clicking on "A Java animation." Time on this recording has been compressed such that 13 seconds corresponds to 27 seconds, or, about 2x real time. Since the frequencies of these emissions are well above the audio frequency range, we have shifted them downward by a factor of 260.
cassini.physics.uiowa.edu/space-audio/cassini/cas-sed-06-023-2hr/ à
cassini.physics.uiowa.edu/space-audio/cassini/cas-sed-06-023-2hr/cas-sed-06-023-twohour.wav
Saturn has lightning, apparently deep in its atmosphere, which generates strong radio emissions, similar to the cracks and pops one hears on an AM radio during a thunderstorm. First discovered by Voyager 1, these radio emissions are the only direct evidence of lightning at Saturn, so far. The Cassini Radio and Plasma Wave Science (RPWS) instrument sweeps in frequency up to 16 MHz. Since the lightning-related radio emissions are emitted over a broad range of frequencies but last only about one thirtieth of a second, a burst appears at whatever frequency the instrument happens to be tuned to at the moment of the burst. So, in this representation of the RPWS observations of a strong thunderstorm beginning on January 23, 2006, the radio emissions appear as speckles at random frequencies above about 2 MHz. These records were converted to sound by using the amplitude and duration of the bursts to create an audio signal.
The sound of the radio emissions can be heard by clicking on the button labeled "Play audio" or in an animated version (which shows a cursor that indicates time on the spectrogram) by clicking on "A Java animation." In this audio clip, time is compressed by a factor of about 260. That is, this 28 second clip represents two hours of Cassini observations. The actual occurrence rate of the flashes during the peak of this storm is about one every two seconds.
www.jpl.nasa.gov/multimedia/sounds/audio/saturn-curve.mp3
www.jpl.nasa.gov/multimedia/sounds/audio/spookysaturn.mp3
Satrun rings inbound & outbound
cassini.physics.uiowa.edu/space-audio/cassini/ring-plane/ à & à
cassini.physics.uiowa.edu/space-audio/cassini/ring-plane/first_rpxing_15_sh.wav
cassini.physics.uiowa.edu/space-audio/cassini/ring-plane/second_rpxing_8_sh.wav
Satrun satellites
Enceladus sounds from a satellite of Satrun.
photojournal.jpl.nasa.gov/catalog/PIA07869 à
photojournal.jpl.nasa.gov/animation/PIA07869 à
Cassini's magnetometer instrument detected an atmosphere around Enceladus during the Feb. 17, 2005, flyby and again during a March 9, 2005, flyby. This audio file is based on the data collected from that instrument.
Ion cyclotron waves are organized fluctuations in the magnetic field that provide information on what ions are present. Cassini's magnetometer detected the presence of these waves in the vicinity of Saturn's moon Enceladus. This audio file shows the power of these waves near Enceladus.
The Cassini-Huygens mission is a cooperative project of NASA, the European Space Agency and the Italian Space Agency. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The magnetometer team is based at Imperial College in London, working with team members from the United States and Germany.
Titan / Satrun
www.jpl.nasa.gov/multimedia/sounds/audio/titan-come.mp3
www.jpl.nasa.gov/multimedia/sounds/audio/titan-echo.mp3
Ganymede / Satrun
Bow-Shcok. Satrun
cassini.physics.uiowa.edu/space-audio/cassini/bow-shock/ à
cassini.physics.uiowa.edu/space-audio/cassini/bow-shock/t2004_179_oneshock.wav
The Cassini spacecraft crossed the bow shock of Saturn at 09 hr 45 min Universal Time on June 27, 2004, at a radial distance of 49.2 RS (Saturn Radii) from Saturn. The bow shock is a discontinuity that forms in the solar wind when the supersonic solar wind encounters the magnetic field of a planet, very similar to the shock wave that forms upstream of an aircraft moving at a supersonic speed. The color frequency-time spectrogram in the above illustration shows the electric field intensities detected by the Cassini Radio and Plasma Wave Science (RPWS) instrument. The bow shock crossing is indicated by the abrupt burst of electric field noise at the time marked by the arrow. The electric field noise is caused by electrical currents that flow in the shock.
The sound of the bow shock crossing can be heard by clicking on the button labeled "Audio" or in an animated version (which shows a cursor that indicates time on the spectrogram) by clicking on "Animate." Time on this recording has been compressed such that 10 seconds corresponds to 28 minutes.
Radio Rotation Period of Saturn from Cassini RPWS Measurements
cassini.physics.uiowa.edu/space-audio/cassini/sat-rotation/ à
cassini.physics.uiowa.edu/space-audio/cassini/sat-rotation/sat-rotation-04-154-159.wav
The above diagram illustrates the method used by the Cassini Radio and Plasma Wave Science (RPWS) instrument to study the rotation rate of Saturn. Since giant gas planets such as Saturn have no surface and are shrouded by clouds it is not possible to obtain an accurate rotation rate from visual observations. The rotation rate most commonly quoted is obtained by analyzing the periodic rotational modulation of radio emissions. These radio emissions are generated by charged particles whose motions are controlled by the planetary magnetic field. Since the magnetic field is linked to the deep interior of the planet this technique is believed to give the best indication of the average rotation rate of the planet. At Saturn the radio emission that is used to determine the radio rotation rate occurs in the frequency range from about 50 to 500 kHz and is called Saturn Kilometric Radiation (SKR). The color frequency-time spectrogram in the diagram shows the SKR intensity detected over a five day interval, from June 2 to June 7, 2004. The audio sounds of these radio emissions have been generated by shifting the radio frequency range from 100 to 300 kHz down to the frequency range from 0 to 3 kHz and speeding up the recording so that 1 second corresponds to one rotation. The average rotation period obtained over an approximate one year interval, from April 29, 2003, to June 10, 2004, during the Cassini approach to Saturn, is 10 hr 45 min 45 ± 36 sec. This period differs significantly from the rotation period obtained during the 1980-81 Voyager flybys of Saturn which was 10 hr 39 min 24 ± 7 sec [see Desch and Kaiser, Geophys. Res. Lett., 8, 253-256, 1981]. The Cassini observations confirm a result first reported by Lecacheux [Radio Emissions IV, ed. by H. O. Rucker, S. J. Bauer, and A. Lecacheux, Austrian Academy of Sciences Press, Vienna, pp. 313-325, 1977; also see Galopeau and Lecacheux, Geophys. Res. Lett., 105, 13,089-13,101, 2000] using the Ulysses spacecraft that Saturn's radio period often deviates substantially from the Voyager value. A comparison of the power spectrums for the Voyager and Cassini measurements is shown in the Figure below. The reason for the long term variations in Saturn's radio rotation period is poorly understood and will require further study.
Jupiter
galileo.jpl.nasa.gov/sounds.cfm#bowshock
galileo.jpl.nasa.gov/multimedia/v1-jup-bowshock.wav
galileo.jpl.nasa.gov/multimedia/jovefuh-dag.wav
galileo.jpl.nasa.gov/multimedia/jwhist-dag-short.wav
I collected some natural sound fragments from our solar system. Especially Satrun represents the omega energy (gate to be a perfect human or a salvation gate. The old Egyptian were used Ankh for supplying themselves with Omega energy which is work like a spirit in its ring and provide only the useful energies.
With Love
cinsinus
*** These are the "sounds of space" collected by U Iowa instruments on various spacecraft.
www-pw.physics.uiowa.edu/space-audio/index.html
www-pw.physics.uiowa.edu/space-audio/Iowa10-2002.html
www.jpl.nasa.gov/multimedia/sounds/index-flash.html
Satrun
www-pw.physics.uiowa.edu/cassini/
www.nasa.gov/mission_pages/cassini/multimedia/pia07966.html à
www.nasa.gov/wav/123163main_cas-skr1-112203.wav
Saturn is a source of intense radio emissions, which have been monitored by the Cassini spacecraft. The radio waves are closely related to the auroras near the poles of the planet. These auroras are similar to Earth's northern and southern lights. This is an audio file of radio emissions from Saturn.
The Cassini spacecraft began detecting these radio emissions in April 2002, when Cassini was 374 million kilometers (234 million miles) from the planet, using the Cassini radio and plasma wave science instrument. The radio and plasma wave instrument has now provided the first high resolution observations of these emissions, showing an amazing array of variations in frequency and time. The complex radio spectrum with rising and falling tones, is very similar to Earth's auroral radio emissions. These structures indicate that there are numerous small radio sources moving along magnetic field lines threading the auroral region.
Time on this recording has been compressed, so that 73 seconds corresponds to 27 minutes. Since the frequencies of these emissions are well above the audio frequency range, we have shifted them downward by a factor of 44.
The Cassini-Huygens mission is a cooperative project of NASA, the European Space Agency and the Italian Space Agency. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter was designed, developed and assembled at JPL. The radio and plasma wave science team is based at the University of Iowa, Iowa City.
www.nasa.gov/mission_pages/cassini/multimedia/pia07967.html à
www.nasa.gov/wav/123160main_cas-skr2-072504.wav
Saturn is a source of intense radio emissions, which have been monitored by the Cassini spacecraft. The radio waves are closely related to the auroras near the poles of the planet. These auroras are similar to Earth's northern and southern lights. This is an audio file of Saturn's radio emissions.
The Cassini spacecraft began detecting these radio emissions in April 2002, when Cassini was 374 million kilometers (234 million miles) from the planet, using the Cassini radio and plasma wave science instrument.
The instrument has now provided the first high resolution observations of these emissions, showing that show an amazing array of variations in frequency and time. In this example, it appears as though the three rising tones are launched from the more slowly varying narrowband emission near the bottom of this display. If this is the case, it represents a very complicated interaction between waves in Saturn's radio source region, but one which has also been observed at Earth.
Time on this recording has been compressed such that 13 seconds corresponds to 27 seconds. Since the frequencies of these emissions are well above the audio frequency range, we have shifted them downward by a factor of 260.
The Cassini-Huygens mission is a cooperative project of NASA, the European Space Agency and the Italian Space Agency. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter was designed, developed and assembled at JPL. The radio and plasma wave science team is based at the University of Iowa, Iowa City.
cassini.physics.uiowa.edu/space-audio/cassini/SKR1/ à
cassini.physics.uiowa.edu/space-audio/cassini/SKR1/SKR-03-324.wav
Saturn is a source of intense radio emissions. The radio waves are closely related to the auroras near the poles of the planet. These auroras are similar to Earth's northern and southern lights. The Cassini spacecraft began detecting these radio emissions in April 2002 when Cassini was 2.5 astronomical units from the planet using the Cassini Radio and Plasma Wave Science (RPWS) instrument. The RPWS has now provided the first high resolution observations of these emissions that show an amazing array of variations in frequency and time. The complex radio spectrum with rising and falling tones is very similar to Earth's auroral radio emissions. These structures indicate that there are numerous small radio sources moving along magnetic field lines threading the auroral region.
The sound of the radio emissions can be heard by clicking on the button labeled "Audio" or in an animated version (which shows a cursor that indicates time on the spectrogram) by clicking on "Animate." Time on this recording has been compressed such that 73 seconds corresponds to 27 minutes, or, the recording is at 22x real time. Since the frequencies of these emissions are well above the audio frequency range, we have shifted them downward by a factor of 44.
cassini.physics.uiowa.edu/space-audio/cassini/SKR2/ à
cassini.physics.uiowa.edu/space-audio/cassini/SKR2/casskrtrig04207a.wav
Saturn is a source of intense radio emissions. The radio waves are closely related to the auroras near the poles of the planet. These auroras are similar to Earth's northern and southern lights. The Cassini spacecraft began detecting these radio emissions in April 2002 when Cassini was 2.5 astronomical units from the planet using the Cassini Radio and Plasma Wave Science (RPWS) instrument. The RPWS has now provided the first high resolution observations of these emissions that show an amazing array of variations in frequency and time. In this example, it appears as though the three rising tones are launched from the more slowly varying narrowband emission near the bottom of this display. If this is the case, it represents a very complicated interaction between waves in Saturn's radio source region, but one which has also been observed at Earth!
The sound of the radio emissions can be heard by clicking on the button labeled "Audio" or in an animated version (which shows a cursor that indicates time on the spectrogram) by clicking on "A Java animation." Time on this recording has been compressed such that 13 seconds corresponds to 27 seconds, or, about 2x real time. Since the frequencies of these emissions are well above the audio frequency range, we have shifted them downward by a factor of 260.
cassini.physics.uiowa.edu/space-audio/cassini/cas-sed-06-023-2hr/ à
cassini.physics.uiowa.edu/space-audio/cassini/cas-sed-06-023-2hr/cas-sed-06-023-twohour.wav
Saturn has lightning, apparently deep in its atmosphere, which generates strong radio emissions, similar to the cracks and pops one hears on an AM radio during a thunderstorm. First discovered by Voyager 1, these radio emissions are the only direct evidence of lightning at Saturn, so far. The Cassini Radio and Plasma Wave Science (RPWS) instrument sweeps in frequency up to 16 MHz. Since the lightning-related radio emissions are emitted over a broad range of frequencies but last only about one thirtieth of a second, a burst appears at whatever frequency the instrument happens to be tuned to at the moment of the burst. So, in this representation of the RPWS observations of a strong thunderstorm beginning on January 23, 2006, the radio emissions appear as speckles at random frequencies above about 2 MHz. These records were converted to sound by using the amplitude and duration of the bursts to create an audio signal.
The sound of the radio emissions can be heard by clicking on the button labeled "Play audio" or in an animated version (which shows a cursor that indicates time on the spectrogram) by clicking on "A Java animation." In this audio clip, time is compressed by a factor of about 260. That is, this 28 second clip represents two hours of Cassini observations. The actual occurrence rate of the flashes during the peak of this storm is about one every two seconds.
www.jpl.nasa.gov/multimedia/sounds/audio/saturn-curve.mp3
www.jpl.nasa.gov/multimedia/sounds/audio/spookysaturn.mp3
Satrun rings inbound & outbound
cassini.physics.uiowa.edu/space-audio/cassini/ring-plane/ à & à
cassini.physics.uiowa.edu/space-audio/cassini/ring-plane/first_rpxing_15_sh.wav
cassini.physics.uiowa.edu/space-audio/cassini/ring-plane/second_rpxing_8_sh.wav
Satrun satellites
Enceladus sounds from a satellite of Satrun.
photojournal.jpl.nasa.gov/catalog/PIA07869 à
photojournal.jpl.nasa.gov/animation/PIA07869 à
Cassini's magnetometer instrument detected an atmosphere around Enceladus during the Feb. 17, 2005, flyby and again during a March 9, 2005, flyby. This audio file is based on the data collected from that instrument.
Ion cyclotron waves are organized fluctuations in the magnetic field that provide information on what ions are present. Cassini's magnetometer detected the presence of these waves in the vicinity of Saturn's moon Enceladus. This audio file shows the power of these waves near Enceladus.
The Cassini-Huygens mission is a cooperative project of NASA, the European Space Agency and the Italian Space Agency. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The magnetometer team is based at Imperial College in London, working with team members from the United States and Germany.
Titan / Satrun
www.jpl.nasa.gov/multimedia/sounds/audio/titan-come.mp3
www.jpl.nasa.gov/multimedia/sounds/audio/titan-echo.mp3
Ganymede / Satrun
Bow-Shcok. Satrun
cassini.physics.uiowa.edu/space-audio/cassini/bow-shock/ à
cassini.physics.uiowa.edu/space-audio/cassini/bow-shock/t2004_179_oneshock.wav
The Cassini spacecraft crossed the bow shock of Saturn at 09 hr 45 min Universal Time on June 27, 2004, at a radial distance of 49.2 RS (Saturn Radii) from Saturn. The bow shock is a discontinuity that forms in the solar wind when the supersonic solar wind encounters the magnetic field of a planet, very similar to the shock wave that forms upstream of an aircraft moving at a supersonic speed. The color frequency-time spectrogram in the above illustration shows the electric field intensities detected by the Cassini Radio and Plasma Wave Science (RPWS) instrument. The bow shock crossing is indicated by the abrupt burst of electric field noise at the time marked by the arrow. The electric field noise is caused by electrical currents that flow in the shock.
The sound of the bow shock crossing can be heard by clicking on the button labeled "Audio" or in an animated version (which shows a cursor that indicates time on the spectrogram) by clicking on "Animate." Time on this recording has been compressed such that 10 seconds corresponds to 28 minutes.
Radio Rotation Period of Saturn from Cassini RPWS Measurements
cassini.physics.uiowa.edu/space-audio/cassini/sat-rotation/ à
cassini.physics.uiowa.edu/space-audio/cassini/sat-rotation/sat-rotation-04-154-159.wav
The above diagram illustrates the method used by the Cassini Radio and Plasma Wave Science (RPWS) instrument to study the rotation rate of Saturn. Since giant gas planets such as Saturn have no surface and are shrouded by clouds it is not possible to obtain an accurate rotation rate from visual observations. The rotation rate most commonly quoted is obtained by analyzing the periodic rotational modulation of radio emissions. These radio emissions are generated by charged particles whose motions are controlled by the planetary magnetic field. Since the magnetic field is linked to the deep interior of the planet this technique is believed to give the best indication of the average rotation rate of the planet. At Saturn the radio emission that is used to determine the radio rotation rate occurs in the frequency range from about 50 to 500 kHz and is called Saturn Kilometric Radiation (SKR). The color frequency-time spectrogram in the diagram shows the SKR intensity detected over a five day interval, from June 2 to June 7, 2004. The audio sounds of these radio emissions have been generated by shifting the radio frequency range from 100 to 300 kHz down to the frequency range from 0 to 3 kHz and speeding up the recording so that 1 second corresponds to one rotation. The average rotation period obtained over an approximate one year interval, from April 29, 2003, to June 10, 2004, during the Cassini approach to Saturn, is 10 hr 45 min 45 ± 36 sec. This period differs significantly from the rotation period obtained during the 1980-81 Voyager flybys of Saturn which was 10 hr 39 min 24 ± 7 sec [see Desch and Kaiser, Geophys. Res. Lett., 8, 253-256, 1981]. The Cassini observations confirm a result first reported by Lecacheux [Radio Emissions IV, ed. by H. O. Rucker, S. J. Bauer, and A. Lecacheux, Austrian Academy of Sciences Press, Vienna, pp. 313-325, 1977; also see Galopeau and Lecacheux, Geophys. Res. Lett., 105, 13,089-13,101, 2000] using the Ulysses spacecraft that Saturn's radio period often deviates substantially from the Voyager value. A comparison of the power spectrums for the Voyager and Cassini measurements is shown in the Figure below. The reason for the long term variations in Saturn's radio rotation period is poorly understood and will require further study.
Jupiter
galileo.jpl.nasa.gov/sounds.cfm#bowshock
galileo.jpl.nasa.gov/multimedia/v1-jup-bowshock.wav
galileo.jpl.nasa.gov/multimedia/jovefuh-dag.wav
galileo.jpl.nasa.gov/multimedia/jwhist-dag-short.wav
))) Yes MirRA, Right, It was a long time we missed the beautiful communication between us 
