The STEREO IMPACT Suprathermal Electron (STE) Instrument

Lin, R. P.; Curtis, D. W.; Larson, D. E.; Luhmann, J. G.; McBride, Steve; Maier, M.R.; Moreau, Thibault; Tindall, C.; Turin, P.; Wang, Linghua

doi:10.1007/s11214-008-9330-7

Cited by 39 publications

(19 citation statements)

References 25 publications

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“…Further information about the electron behavior across the ICME is provided by SWEA and the suprathermal electron instrument (STE; Lin et al 2008) on board STEREO, as shown in Figure 6. The electron energies range from $1 eV to 100 keV.…”

Section: Sep Eventsmentioning

confidence: 99%

A Comprehensive View of the 2006 December 13 CME: From the Sun to Interplanetary Space

Liu

Luhmann

Müller‐Mellin

et al. 2008

Astrophysical Journal

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141

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The biggest halo coronal mass ejection (CME) since the Halloween storm in 2003, which occurred on 2006 December 13, is studied in terms of its solar source and heliospheric consequences. The CME was accompanied by an X3.4 flare, EUV dimmings, and coronal waves. It generated significant space weather effects such as an interplanetary shock, radio bursts, major solar energetic particle (SEP) events, and a magnetic cloud (MC) that were detected by a fleet of spacecraft including STEREO, ACE, WIND, and Ulysses. Reconstruction of the MC with the Grad-Shafranov (GS) method yields an axis orientation oblique to the flare ribbons. Observations of the SEP intensities and anisotropies show that the particles can be trapped, deflected, and reaccelerated by the large-scale transient structures. The CME-driven shock was observed at both the Earth and Ulysses when they were separated by 74 in latitude and 117 in longitude, which is the largest shock extent ever detected. The ejecta seem to have been missed at Ulysses. The shock arrival time at Ulysses is well predicted by an MHD model that can propagate the 1 AU data outward. The CME /shock is tracked remarkably well from the Sun all the way to Ulysses by coronagraph images, type II frequency drift, in situ measurements, and the MHD model. These results reveal a technique that combines MHD propagation of the solar wind and type II emissions to predict the shock arrival time at the Earth, which is a significant advance for space weather forecasting, especially when in situ data become available from the Solar Orbiter and Solar Sentinels.

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Section: Sep Eventsmentioning

confidence: 99%

A Comprehensive View of the 2006 December 13 CME: From the Sun to Interplanetary Space

Liu

Luhmann

Müller‐Mellin

et al. 2008

Astrophysical Journal

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141

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“…Using high sensitivity measurements from the SupraThermal Electron instrument (Lin et al 2008) on the STEREO, Wang et al (2012) reported that the power-law spectral index δ of superhalo electrons observed during quiet-times near solar minimum ranges from ∼ 1.5 to ∼ 3.4, with an average of ∼ 2.35 ± 0.45. The observed density of superhalo electrons, about 10 −9 −10 −6 of the solar wind proton density, decreases with the decay of solar cycle, while δ has no solar-cycle variation.…”

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confidence: 99%

Numerical simulation of superhalo electrons generated by magnetic reconnection in the solar wind source region

Yang

Wang

et al. 2015

Res. Astron. Astrophys.

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Superhalo electrons appear to be continuously present in the interplanetary medium, even at very quiet times, with a power-law spectrum at energies above ∼2 keV.Here we numerically investigate the generation of superhalo electrons by magnetic reconnection in the solar wind source region, using the MHD and test particle simulations for both single X-line reconnection and multiple X-line reconnection. We find that the direct current electric field, produced in the magnetic reconnection region, can accelerate electrons from an initial thermal energy of T ∼ 10 5 K up to hundreds of keV. After acceleration, some of the accelerated electrons, together with the nascent solar wind flow driven by the reconnection, propagate upwards along the newly-opened magnetic field lines into the interplanetary space, while the rest move downwards into the lower atmosphere. Similar to the observed superhalo electrons at 1 AU, the flux of the upward-traveling accelerated electrons versus energy displays a power-law distribution at ∼ 2 − 100 keV, f (E) ∼ E −δ , with a δ of ∼ 1.5 − 2.4. For single (multiple) X-line reconnection, the spectrum becomes harder (softer) as the anomalous resistivity parameter α (uniform resistivity η) increases. These modeling results suggest that the acceleration in the solar wind source region may contribute to superhalo electrons.

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“…To measure the kinetic energy of the particles, each sensor head contains a solid state detector (SSD) with an ultra-thin window and several pixels, which is based on technology used for STE on STEREO (Lin et al 2008) (see Sect. 4.1).…”

Section: The Suprathermal Electron Proton (Step) Sensormentioning

confidence: 99%

The Energetic Particle Detector

Rodrı́guez-Pacheco

Wimmer‐Schweingruber

Mason

et al. 2020

A&A

136

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After decades of observations of solar energetic particles (SEP) from space-based observatories, relevant questions on particle injection, transport, and acceleration remain open. To address these scientific topics, accurate measurements of the particle properties in the inner heliosphere are needed. In this paper we describe the Energetic Particle Detector (EPD), an instrument suite that is part of the scientific payload aboard the Solar Orbiter mission. Solar Orbiter will approach the Sun as close as 0.28 au and will provide extra-ecliptic measurements beyond ∼ 30 • heliographic latitude during the later stages of the mission. The EPD will measure electrons, protons, and heavy ions with high temporal resolution over a wide energy range, from suprathermal energies up to several hundreds of megaelectronvolts/nucleons. For this purpose, EPD is composed of four units: the SupraThermal Electrons and Protons (STEP), the Electron Proton Telescope (EPT), the Suprathermal Ion Spectrograph (SIS), and the High-Energy Telescope (HET) plus the Instrument Control Unit (ICU) that serves as power and data interface with the spacecraft. The low-energy population of electrons and ions will be covered by STEP and EPT, while the high-energy range will be measured by HET. Elemental and isotopic ion composition measurements will be performed by SIS and HET, allowing full particle identification from a few kiloelectronvolts up to several hundreds of megaelectronvolts/nucleons. Angular information will be provided by the separate look directions from different sensor heads, on the ecliptic plane along the Parker spiral magnetic field both forward and backwards, and out of the ecliptic plane observing both northern and southern hemispheres. The unparalleled observations of EPD will provide key insights into long-open and crucial questions about the processes that govern energetic particles in the inner heliosphere.

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The STEREO IMPACT Suprathermal Electron (STE) Instrument

Cited by 39 publications

References 25 publications

A Comprehensive View of the 2006 December 13 CME: From the Sun to Interplanetary Space

A Comprehensive View of the 2006 December 13 CME: From the Sun to Interplanetary Space

Numerical simulation of superhalo electrons generated by magnetic reconnection in the solar wind source region

The Energetic Particle Detector

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