scholarly journals Cassini plasma spectrometer measurements of Jovian bow shock structure

2003 ◽  
Vol 108 (A7) ◽  
Author(s):  
Karoly Szego
Keyword(s):  
Shock Structure ◽  
Bow Shock ◽  
Plasma Spectrometer

The bow shock structure of IRS 7 - Wind-wind collision near the Galactic center

1992 ◽  
Vol 385 ◽  
pp. L41 ◽  
Author(s):  
Farhad Yusef-Zadeh ◽  
Fulvio Melia
Keyword(s):  
Galactic Center ◽  
Shock Structure ◽  
Bow Shock

Observations of Short Large Amplitude Magnetic Structures at the Kronian bow shock

2020 ◽  
Author(s):  
Zsofia Bebesi ◽  
Geza Erdos ◽  
Melinda Dosa ◽  
Antal Juhasz ◽  
Karoly Szego
Keyword(s):  
Large Amplitude ◽  
Ion Beam ◽  
Plasma Heating ◽  
Bow Shock ◽  
Time Interval ◽  
Magnetic Structures ◽  
Earth Observations ◽  
Multiple Beams ◽  
Plasma Spectrometer ◽  
Beam Reflection

<p>We observed Short Large Amplitude Magnetic Structures (SLAMS) at Saturn upstream of the quasi-parallel bow shock. Cassini surveyed the quasi-parallel regime mainly during 2004 and 2005, and we present a few detailed case studies from this time interval. For our analysis we used the measurements of the Cassini Plasma Spectrometer and the Magnetometer.<br />Locally the SLAMS act as fast mode shock waves, and we observed ion beam reflection, multiple beams, deceleration and plasma heating of the solar wind protons. These features are in agreement with the near Earth observations of SLAMS. We also detected whistler precursor waves multiple times, which was also documented in studies of the Earth's foreshock region. Since the frequency of the upstream ULF waves observed at Saturn is lower than it is at Earth, it also has an effect on the spatial extension of the SLAM structures, which arise from these waves. With only one spacecraft's measurements it is not possible to study the SLAMS with the same efficiency as with the four-point measurements of the CLUSTER probes, but the basic observational features and the description of their evolutional characteristics are summarized. </p>

[ITAL]Hubble Space Telescope[/ITAL] Images of the HH 34 Jet and Bow Shock: Structure and Proper Motions

2002 ◽  
Vol 123 (1) ◽  
pp. 362-381 ◽  
Author(s):  
Bo Reipurth ◽  
Steve Heathcote ◽  
Jon Morse ◽  
Pat Hartigan ◽  
John Bally
Keyword(s):  
Hubble Space Telescope ◽  
Shock Structure ◽  
Bow Shock ◽  
Proper Motions ◽  
Space Telescope

Analysis of short large amplitude magnetic structures at the Kronian bow shock

2020 ◽  
Author(s):  
Zsofia Bebesi ◽  
Geza Erdos ◽  
Melinda Dosa ◽  
Karoly Szego
Keyword(s):  
Large Amplitude ◽  
Ion Beam ◽  
Plasma Heating ◽  
Bow Shock ◽  
Ulf Waves ◽  
Fast Mode ◽  
Magnetic Structures ◽  
Earth Observations ◽  
Plasma Spectrometer ◽  
Beam Reflection

<p>            We present a comprehensive statistical analysis of Short Large Amplitude Magnetic Structures (SLAMS) upstream of the quasi-parallel bow shock of Saturn. During its mission Cassini extensive surveyed the quasi-parallel regime. For this study we used the measurements of the Cassini Plasma Spectrometer (CAPS) and the Magnetometer (MAG).</p><p>            The SLAM structures locally act as fast mode shock waves, and we observed possible ion beam reflection, multiple ion beams, deceleration and plasma heating of the solar wind protons. These features are in agreement with the near Earth observations. We also detected whistler precursor waves multiple times, which was also documented in studies of the Earth's foreshock region. Since the frequency of the upstream ULF waves detected at Saturn is lower than it is at Earth, it also has an effect on the spatial extension of the SLAM structures, which arise from these waves. With only one spacecraft's measurements it is not possible to study the SLAMS with the same efficiency as with the four-point measurements of the CLUSTER probes, but the basic observational features and the description of their evolutional characteristics are summarized.</p>

scholarly journals HH 34: The bow shock of a jet

1987 ◽  
Vol 122 ◽  
pp. 175-176
Author(s):  
Th. Bührke ◽  
R. Mundt
Keyword(s):  
Radial Velocity ◽  
Electron Density ◽  
High Velocity ◽  
Shock Structure ◽  
Bow Shock ◽  
Complex Velocity ◽  
Ccd Imaging ◽  
Working Surface ◽  
Lower Excitation ◽  
Hh Object

Deep CCD imaging of HH 34 in H∝ shows that the HH-object has a bow shock-like structure, of which the wings can be traced over about 1 arcmin ( pc). A knotty jet is pointing towards the apex of the bow shock structure. Long-slit spectroscopy reveals that 1) the jet has approximately a constant radial velocity and electron density. 2). The spectrum of the jet is of a much lower excitation than that of HH 34. 3) HH 34 has a complex velocity and line excitation structure. The extended bow shock is interpreted by a jet of which the working surface is propagating with high velocity (≈ 200 km/s) through a partially ionized medium.

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