Fine Structure of Interplanetary Shock Front—Results from BMSW Experiment with High Time Resolution

The structure of subcritical interplanetary shocks was studied using high time resolution from the BMSW plasma instrument onboard the Spektr‐R satellite and MFI magnetometer measurements from WIND. Ion scales of the ramp and wavelength of precursor waves were obtained and compared with results of th...

Full description

Saved in:
Bibliographic Details
Published in:Journal of geophysical research. Space physics 2019-11, Vol.124 (11), p.8191-8207
Main Authors: Borodkova, N.L., Eselevich, V.G., Zastenker, G.N., Sapunova, O.V., Yermolaev, Yu.I., Šafránková, J., Nĕmeček, Z., Přech, L.
Format: Article
Language:English
Subjects:
Balances (scales)
dispersion of oblique magnetosonic waves
Energy dissipation
Fine structure
interplanetary shock
Ions
Oscillations
Precursors
ramp
Solar wind
Solar wind ions
Upstream
upstream wave train
Wave packets
Wavelengths
Whistlers
Citations: Items that this one cites
Items that cite this one
Online Access:Get full text
Tags: Add Tag
No Tags, Be the first to tag this record!
Description
Summary:The structure of subcritical interplanetary shocks was studied using high time resolution from the BMSW plasma instrument onboard the Spektr‐R satellite and MFI magnetometer measurements from WIND. Ion scales of the ramp and wavelength of precursor waves were obtained and compared with results of the bow shock structure study. The comparison of precursor wavelengths, determined experimentally with those determined from dispersion relation for low‐Mach, low‐beta shocks has showed similar results. This confirms the assumption that the dispersion of oblique magnetosonic waves is the determining factor in the formation of upstream wave trains. On the base of the case study it was shown that damped downstream oscillations of density, velocity, temperature may be generated by the interaction of the inflowing solar wind ions with the reflected gyrating ions inside the ramp. A sequence of six wave trains of magnetosonic whistlers has been observed upstream the ramp of subcritical oblique IP shock. The amplitude of oscillations inside the trains decreased with increasing distance from the ramp. The possible energy dissipation mechanism within the shock front is discussed. Key Points The structure of subcritical interplanetary shocks including ramp and precursor wave train was studied on the base of the BMSW plasma data It was confirmed that dispersion of the oblique magnetosonic waves is the determining factor in the formation of the upstream wave trains It was shown that reflected protons play an important role in the formation of fine structure of interplanetary shock front
ISSN:2169-9380
2169-9402
DOI:10.1029/2018JA026255