Journal
ASTROPHYSICAL JOURNAL
Volume 819, Issue 1, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.3847/0004-637X/819/1/6
Keywords
instabilities; plasmas; solar wind; waves
Categories
Funding
- NASA Postdoctoral Program at the Goddard Space Flight Center
- Conicyt-Becas Chile Postdoctoral Fellowship
- Heliophysics Guest Investigator grant
- NASA [NNX13AI65G]
- STFC [ST/K000977/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/K000977/1] Funding Source: researchfish
- NASA [473262, NNX13AI65G] Funding Source: Federal RePORTER
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We use audification of 0.092 s cadence magnetometer data from the Wind spacecraft to identify waves with amplitudes >0.1 nT near. the ion gyrofrequency (similar to 0.1 Hz) with duration longer than 1 hr during 2008. We present one of the most common types of event for a case study and find it to be a proton-cyclotron wave storm, coinciding with highly radial magnetic field and a suprathermal proton beam close in density to the core distribution itself. Using linear Vlasov analysis, we conclude that the long-duration, large-amplitude waves are generated by the instability of the proton distribution function. The origin of the beam is unknown, but the radial field period is found in the trailing edge of a fast solar wind stream and resembles other events thought to be caused by magnetic field footpoint motion or interchange reconnection between coronal holes and closed field lines in the corona.
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