Erratum: “Electromagnetic Waves near the Proton Cyclotron Frequency: STEREO Observations” (2014, ApJ, 786, 123)

Jian, L. K.; Wei, Hong; Russell, C. T.; Luhmann, J. G.; Klecker, B.; Omidi, N.; Isenberg, Philip A.; Goldstein, M. L.; Viñas, A. F.; Blanco‐Cano, X.

doi:10.3847/1538-4357/aa862f

Cited by 14 publications

(59 citation statements)

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“…Furthermore, the characteristics of LH‐ICWs in our study are somewhat similar to those reported by Jian et al [] for LFW storms observed in the pristine solar wind at 1 AU (average ω sc ≈0.178 Hz, average ω p ≈0.03 Hz, average ω p /Ω cp ≈0.6, average δ B / B 0 ≈0.025, and

θ_{B_{0} k} < 20 °

). Such LFW storms last over 10 min, and they were sporadically observed in the solar wind with an occurrence rate of around 0.9% of the analyzed time, strikingly similar to our observations (LH‐ICWs had a mean occurrence rate of around 1% inside MCs/MCL structures).…”

Section: Summary and Discussionsupporting

confidence: 90%

Low‐frequency waves within isolated magnetic clouds and complex structures: STEREO observations

et al. 2015

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[2007][2008][2009][2010][2011]. It is important to study in detail the properties of waves in space plasmas since particle distribution functions can be modified by wave-particle interactions. We compare wave characteristics within IMCs with those waves observed inside CSs. Both left-handed (LH) and right-handed (RH), near-circularly polarized, transverse and almost parallel-propagating LFWs (around the proton cyclotron frequency) were sporadically observed inside both IMCs and CSs. In contrast, compressive mirror-mode waves (MMs) were observed only within CSs. We studied local plasma conditions inside the IMCs and CSs to gain insight about wave origin: most of the MMs within CSs were observed in regions with enhanced plasma beta ( > 1); the majority of the LH waves were found in low beta plasmas ( < 1), and the RH waves were predominantly observed at moderate betas (0.4 < ≤ 2). These observations are in agreement with linear kinetic theory predictions for the growth of the mirror, the LH ion cyclotron, and the RH ion firehose instability, respectively. It is possible that the waves were generated locally inside the IMCs and CSs via temperature anisotropies. The plasma beta enhancements that were frequently observed inside the CSs may be the result of compressions and heating taking place inside the interacting structures.

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θ_{B_{0} k} < 20 °

Section: Summary and Discussionsupporting

confidence: 90%

Low‐frequency waves within isolated magnetic clouds and complex structures: STEREO observations

et al. 2015

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“…These waves could play an important role in energizing the corona/solar wind ions and in modifying their temperature anisotropy [e.g., Ofman et al ., 2001, ; Gary et al ., ; Podesta and Gary , ; Omidi et al ., , ]. Studies of these waves have been made at around 0.3 AU [ Jian et al ., ] and at 1 AU [ Tsurutani et al ., ; Jian et al ., , ; He et al ., ]. These waves have been observed over the high‐latitude Southern and Northern Hemispheres of the Sun between 1.5 and 3.0 AU by the Ulysses spacecraft [ Podesta and Gary , ].…”

Section: Introductionmentioning

confidence: 99%

“…At 1 AU, Jian et al . [] investigated various wave modes that might explain the observations and concluded that they are likely ion cyclotron waves (ICWs) generated in solar wind frame of reference by temperature anisotropy of the ions. They concluded that other sources are unlikely: like interstellar pickup ions He + or Ne + , cometary pickup ions, and solar energetic particles associated with solar flares or interplanetary coronal mass ejections.…”

Section: Introductionmentioning

confidence: 99%

“…These waves are observed when the IMF is preferentially in the radial direction [e.g., Murphy et al ., ; Jian et al ., , , ]. The observed angle between the wave vector ( k ) and the IMF is typically less than 20° [e.g., Jian et al ., , , ], being either nearly field aligned or antifield aligned with the IMF direction. For ICWs generated in the solar wind frame, in which they are left‐handed circularly polarized, the Doppler shift relative to the spacecraft frame will be large, because V SW / V A > 4 (where V SW is the solar wind speed and V A is the Alfvén speed and is a proxy for the ICW phase speed).…”

Section: Introductionmentioning

confidence: 99%

“…Jian et al . [] covered 1 year of STEREO A measurements and were focused on LFW storms which lasted at least 10 min. In that study they found that the intrinsic properties of the wave events were independent of the temporal duration of the events.…”

Section: Introductionmentioning

confidence: 99%

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MESSENGER survey of in situ low frequency wave storms between 0.3 and 0.7 AU

et al. 2015

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MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) magnetometer data was surveyed between 0.3 and 0.7 AU from 6 June 2007 to 23 March 2011 for low‐frequency wave (LFW) storms, when the magnetometer was sampling at a rate of at least 2 s−1. A total of 12,197 LFW events were identified, of which 5506 lasted 10 min or longer. The events have a high degree of polarization, are circularly polarized, with wave vectors nearly aligned or antialigned with the interplanetary magnetic field (IMF) at frequencies in the vicinity of the proton cyclotron frequency. These events are observed about 6% of the time, preferentially associated with radially directed inward or outward IMF. Their occurrence rate and median duration do not change much with R, where R is the heliocentric radial distance. For a narrow‐frequency window in the solar wind frame, left‐handed storms in the spacecraft frame have a power drop off that is roughly proportional to R−3 which is consistent with a source close the Sun, while right‐handed storms have a power drop off roughly proportional R−1 which is not consistent with a source close to the Sun. The power in the left‐handed LFW storms is on average greater than the right‐handed ones by a factor of 3. In the solar wind frame, the wave frequency decreases from 0.13 to 0.04 Hz moving from 0.3 to 0.7 AU, but the frequency normalized by the local proton cyclotron frequency does not change much with the running median varying from 0.35 to 0.5. The normalized frequency band widths of the wave power spectra increase slightly with R, possibly associated with energy dissipation.

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ACE observations of magnetic waves arising from newborn interstellar pickup helium ions

Argall

Fisher

Joyce

et al. 2015

Geophysical Research Letters

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We report low‐frequency magnetic waves that were observed by the Advanced Composition Explorer (ACE) spacecraft on day of year 180 of 1999 with characteristics consistent with the predictions of waves excited by newborn interstellar pickup He+ ions. This event was found by examining daily spectrograms of MAG data, a new data product that is now available to the community via the ACE Science Center. The event shown here is one of approximately 20 similar events that will be analyzed in future studies. This event is fairly typical of those we have found so far. The waves exist at spacecraft‐frame frequencies between the He+ cyclotron frequency and approximately twice the H+ cyclotron frequency. Fluctuations are transverse to the mean magnetic field, are noncompressive, circularly polarized, have field‐aligned minimum variance directions, and are left‐hand polarized in the spacecraft frame as predicted by theory. The event lasts for just under 1 h.

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Erratum: “Electromagnetic Waves near the Proton Cyclotron Frequency: STEREO Observations” (2014, ApJ, 786, 123)

Cited by 14 publications

References 0 publications

Low‐frequency waves within isolated magnetic clouds and complex structures: STEREO observations

Low‐frequency waves within isolated magnetic clouds and complex structures: STEREO observations

MESSENGER survey of in situ low frequency wave storms between 0.3 and 0.7 AU

ACE observations of magnetic waves arising from newborn interstellar pickup helium ions

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