COSTEP - Comprehensive Suprathermal and Energetic Particle Analyser

Müller‐Mellin, R.; Kunow, H.; Fleißner, V.; Pehlke, E.; Rode, E.; Röschmann, N.; Scharmberg, C.; Sierks, H.; Rusznyak, P.; McKenna‐Lawlor, S.; Elendt, I.; Sequeiros, J.; Meziat, D.; Sánchez, S. F.; Medina, J.; Peral, L. del; Witte, M.; Marsden, R. G.; Henrion, J.

doi:10.1007/bf00733437

Cited by 180 publications

(108 citation statements)

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“…We used the EPHIN instrument, part of the Comprehensive Suprathermal and Energetic Particle analyser (COSTEP) onboard SOHO (Müller-Mellin et al, 1995). For the proton events we used the 25 -41 MeV channel (column 2) whereas the electron onset time is estimated either from the 0.25 -0.7 MeV or 0.67 -3 MeV channel, as given with superscript "l" or "h" in column 4, respectively.…”

Section: Eastern Sep Eventsmentioning

confidence: 99%

Solar Energetic Particles and Associated EIT Disturbances in Solar Cycle 23

et al. 2014

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We explore the link between solar energetic particles (SEPs) observed at 1 AU and large-scale disturbances propagating in the solar corona, named after the Extreme ultraviolet Imaging Telescope (EIT) as EIT waves, which trace the lateral expansion of a coronal mass ejection (CME). A comprehensive search for SOHO/EIT waves was carried out for 179 SEP events during Solar Cycle 23 (1997 -2006). 87 % of the SEP events were found to be accompanied by EIT waves. In order to test if the EIT waves play a role in the SEP acceleration, we compared their extrapolated arrival time at the footpoint of the Parker spiral with the particle onset in the 26 eastern SEP events that had no direct magnetic connection to the Earth. We find that the onset of proton events was generally consistent with this scenario. However, in a number of cases the first near-relativistic electrons were detected too early. Furthermore, the electrons had in general only weakly anisotropic pitch-angle distributions. This poses a problem for the idea that the SEPs were accelerated by the EIT wave or in any other spatially confined region in the low corona. The presence of weak electron anisotropies in SEP events from the eastern hemisphere suggests that transport processes in interplanetary space, including cross-field diffusion, play a role in giving the SEPs access to a broad range of helio-longitudes.

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Section: Eastern Sep Eventsmentioning

confidence: 99%

Solar Energetic Particles and Associated EIT Disturbances in Solar Cycle 23

et al. 2014

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“…The solar energetic particle events were observed with the Comprehensive Suprathermal and Energetic Particle Analyser (COSTEP) (Müller-Mellin et al 1995) aboard the Solar and Heliospheric Observatory (SOHO) and with the 3-D plasma instrument on board the Wind spacecraft (Lin et al 1995). In this study we use the COSTEP and Wind 3-DP electron flux measurements in the ranges 0.25-0.7 MeV and below 0.39 MeV, respectively.…”

Section: Instrumentation and Data Selectionmentioning

confidence: 99%

Solar energetic electron events and coronal shocks

Klassen

Bothmer

Mann

et al. 2002

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Abstract. Mildly relativistic electrons appear during the solar energetic particle events. A detailed investigation on the origin of such electrons is presented for four particlular solar events. The mildly relativistic electrons have been detected at energies of 0.25-0.7 MeV by COSTEP/SOHO and below 0.392 MeV by Wind 3-DP experiments. Coronal shocks associated with these electron events are identified from the metric-to-decametric solar type II radio bursts. All selected events were associated with solar activity at western longitudes, so that the magnetic footpoints connecting the spacecraft with the Sun were close to the flare/shock/CME site. The associated type II bursts were accompanied by so-called shock accelerated (SA) type III bursts appearing to be emerging from the type II emission site. We found: (1) that all of the 0.25-0.7 MeV electron events were released during or after, but never simultaneously with the onset of type II bursts and CMEs. The time delay between the type II burst onset and the release of the mildly relativistic electrons is in the range of 11.5−45 min; (2) that the mildly relativistic electrons were released rather at the end of SA type III bursts or somewhat later; (3) that the mildly relativistic electrons were released when the associated type II burst and the CME reached a certain height (h ∼ 1-4 Rs) above the photosphere. For the four events studied, it is concluded that mildly relativistic electrons at 0.25-0.7 MeV energies measured in the interplanetary medium from solar energetic particle events are accelerated by coronal shock waves, commonly in association with white-light CMEs.

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“…Near-relativistic electron event information derived from ACE/EPAM observations is complemented by event onset times determined from SOHO/EPHIN electron data (Müller-Mellin et al 1995). The energy channel of interest was 0.7-3.0 MeV.…”

Section: Onset Solar Release and Event End Time Determinationmentioning

confidence: 99%

“…We have extended the period of interest to cover the years 2011-2016 and also revisited the proton velocity dispersion analysis (VDA), electron event onset times, as well as electromagnetic (soft X-ray) and CME observations for the events listed in Vainio et al (2013). Based on data from the Energetic and Relativistic Nuclei and Electron (ERNE) experiment (Torsti et al 1995), the Large Angle and Spectrometric Coronagraph (LASCO; Brueckner et al 1995), and the Electron Proton Helium Instrument (EPHIN; Müller-Mellin et al 1995) aboard the Solar and Heliospheric Observatory (SOHO) spacecraft, as well as the Electron, Proton and Alpha Monitor (EPAM; Gold et al 1998) aboard the Advanced Composition Explorer (ACE) and the X-ray flux measuring instrumentation on the Geostationary Operational Environmental Satellites (GOES) in active operation during the period of interest, our catalogue comprises a total of 176 energetic solar particle events between 1996 and 2016. This time span covers solar cycle 23 in its entirety and more than the first half of solar cycle 24, which allows us to gain some insight into the differences of these two cycles.…”

Section: Introductionmentioning

confidence: 99%

Catalogue of 55–80 MeV solar proton events extending through solar cycles 23 and 24

Paassilta

Raukunen

Vainio

et al. 2017

J. Space Weather Space Clim.

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We present a new catalogue of solar energetic particle events near the Earth, covering solar cycle 23 and the majority of solar cycle 24 (1996-2016), based on the 55-80 MeV proton intensity data gathered by the Solar and Heliospheric Observatory/the Energetic and Relativistic Nuclei and Electron experiment (SOHO/ERNE). In addition to ERNE proton and heavy ion observations, data from the Advanced Composition Explorer/Electron, Proton and Alpha Monitor (ACE/EPAM) (near-relativistic electrons), SOHO/EPHIN (Electron Proton Helium Instrument) (relativistic electrons), SOHO/LASCO (Large Angle and Spectrometric Coronagraph) (coronal mass ejections, CMEs) and Geostationary Operational Environmental Satellite (GOES) soft X-ray experiments are also considered and the associations between the particle and CME/X-ray events deduced to obtain a better understanding of each event. A total of 176 solar energetic particle (SEP) events have been identified as having occurred during the time period of interest; their onset and solar release times have been estimated using both velocity dispersion analysis (VDA) and time-shifting analysis (TSA) for protons, as well as TSA for near-relativistic electrons. Additionally, a brief statistical analysis was performed on the VDA and TSA results, as well as the X-rays and CMEs associated with the proton/electron events, both to test the viability of the VDA and to investigate possible differences between the two solar cycles. We find, in confirmation of a number of previous studies, that VDA results for protons that yield an apparent path length of 1 AU < s [ 3 AU seem to be useful, but those outside this range are probably unreliable, as evidenced by the anticorrelation between apparent path length and release time estimated from the X-ray activity. It also appears that even the first-arriving energetic protons apparently undergo significant pitch angle scattering in the interplanetary medium, with the resulting apparent path length being on average about twice the length of the spiral magnetic field. The analysis indicates an increase in high-energy SEP events originating from the far-eastern solar hemisphere; for instance, such an event with a well-established associated GOES flare has so far occurred three times during cycle 24 but possibly not at all during cycle 23. The generally lower level of solar activity during cycle 24, as opposed to cycle 23, has probably caused a significant decrease in total ambient pressure in the interplanetary space, leading to a larger proportion of SEP-associated halo-type CMEs. Taken together, these observations point to a qualitative difference between the two solar cycles.

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COSTEP - Comprehensive Suprathermal and Energetic Particle Analyser

Cited by 180 publications

References 1 publication

Solar Energetic Particles and Associated EIT Disturbances in Solar Cycle 23

Solar Energetic Particles and Associated EIT Disturbances in Solar Cycle 23

Solar energetic electron events and coronal shocks

Catalogue of 55–80 MeV solar proton events extending through solar cycles 23 and 24

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