Survey of caveats in low-energy particle measurements: Ulysses/HI-SCALE and ACE/EPAM Instruments

Marhavilas, P. K.; Malandraki, O.; Anagnostopoulos, Georgios C.

doi:10.1016/j.pss.2015.06.010

Cited by 15 publications

(8 citation statements)

References 17 publications

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“…ftecs.com). Contamination by high-energy particles penetrating the instrument, occurring mainly at the onset of SEP events, might also contaminate the low-energy channels of both LEMS30 and LEMS120 (Marhavilas et al 2015). Besides, the LEMS30 P1 channel has no data since day 327 of 2001, and P2 has no data since day 302 of 2003 (Haggerty et al 2006).…”

Section: Observationsmentioning

confidence: 99%

Evolution of the Suprathermal Proton Population at Interplanetary Shocks

Lario

Berger

Decker

et al. 2019

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We investigate the evolution of the suprathermal (ST) proton population as interplanetary shocks cross 1 au. The variability of the ST proton intensities and energy spectra upstream of the shocks is analyzed in terms of the shock parameters, upstream magnetic field configurations, and preexisting upstream populations. Propitious conditions for the observation of ST particles at distances far upstream from the shock occur in parallel shock configurations when particles can easily escape from the shock vicinity. In this situation, ST intensity enhancements show onsets characterized by velocity dispersion effects and energy spectra that develop into a "hump" profile peaking around ∼10 keV just before the arrival of the shock. The observation of field-aligned proton beams at low energies (5-10 keV) is possible under conditions that facilitate the scatter-free propagation of the particles streaming out of the shock. Upstream of perpendicular shocks, ST intensity enhancements are only observed in close proximity to the shock. Power-law proton spectra develop downstream of the shocks. The functional form for the downstream phase-space density proportional to v −5 is observed only over a limited range of ST energies. The absence of ST populations observed far upstream of interplanetary shocks raises questions about whether ST protons contribute as a seed particle population in the processes of particle acceleration at shocks.

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Section: Observationsmentioning

confidence: 99%

Evolution of the Suprathermal Proton Population at Interplanetary Shocks

Lario

Berger

Decker

et al. 2019

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“…Since the spacecraft spin axis is within 20 • of the Sun-Earth line, LEMS30 points mostly Sunward while LEMS120 points anti-Sunward. One problem with LEMS30 is the failure of the P1 channel during 2001 [Haggerty et al, 2006] and X-ray contamination [Marhavilas et al, 2015]. This resulted in an elevated noise floor and eventually the instrument had to be turned off.…”

Section: Data and Analysis Proceduresmentioning

confidence: 99%

Effect of Coherent Structures on Energetic Particle Intensity in the Solar Wind at 1 Au

Tessein

Ruffolo

Matthaeus

et al. 2015

ApJ

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“…1a, the ESP onset was characterised by abrupt and simultaneous intensity rises in all ion energy channels of the Low-Energy Magnetic Spectrometer (LEMS120) of the Electron, Proton, and Alpha Monitor (EPAM; Gold et al 1998) on board the Advanced Composition Explorer (ACE). Most of the ions measured by ACE/EPAM are protons (Marhavilas et al 2015). Signatures of the ESP event were also detected by the Energetic and Relativistic Nuclei and Electron (ERNE) experiment (Torsti et al 1995) on board the Solar and Heliospheric Observatory (SoHO) for protons with energies up to ∼30 MeV.…”

Section: The Esp Event On 14 July 2012mentioning

confidence: 87%

Observation-based modelling of the energetic storm particle event of 14 July 2012

Wijsen

Aran

Scolini

et al. 2022

Preprint

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In this work, we model the energetic storm particle (ESP) event of 14 July 2012 using the energetic particle acceleration and transport model named PARADISE (PArticle Radiation Asset Directed at Interplanetary Space Exploration), together with the solar wind and coronal mass ejection (CME) model named EUHFORIA (EUropean Heliospheric FORcasting Information Asset). &#160;The CME generating the ESP event is simulated by using the spheromak model of EUHFORIA, which approximates the CME&#8217;s magnetic field as a linear force-free spheroidal magnetic field. The energetic particles are modelled by injecting a seed population of 50 KeV protons continiously at the CME-driven shock wave. The simulation results illustrate both the capabilities and limitations of the utilised models.&#160;&#160;We find that for energies below 1 MeV, the simulation results agree well with the upstream and downstream components of the ESP event observed by the Advanced Composition Explorer (ACE). &#160;This suggests that these low-energy protons are mainly the result of interplanetary particle acceleration. In the downstream region, the sharp drop in the energetic particle intensities is reproduced at the entry into the following magnetic cloud, illustrating the importance of a magnetised CME model.This research has received funding from the European Union&#8217;s Horizon 2020 research and innovation programme under grant agreement No 870405 (EUHFORIA 2.0).

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Survey of caveats in low-energy particle measurements: Ulysses/HI-SCALE and ACE/EPAM Instruments

Cited by 15 publications

References 17 publications

Evolution of the Suprathermal Proton Population at Interplanetary Shocks

Evolution of the Suprathermal Proton Population at Interplanetary Shocks

Effect of Coherent Structures on Energetic Particle Intensity in the Solar Wind at 1 Au

Observation-based modelling of the energetic storm particle event of 14 July 2012

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