Stereoscopic observations of solar flares made onboard the 2001 Mars Odyssey spacecraft and CORONAS-F satellite

Livshits, M. A.; Chernetskii, V. A.; Богомолов, А. В.; Kuznetsov, S. N.; Logachev, Yu. I.; Myagkova, I. N.; Свертилов, С. И.; Yushkov, B. Yu.

doi:10.1134/s0038094606020092

Cited by 5 publications

(6 citation statements)

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“…Indeed, a large white light flare was observed (Metcalf et al 2003), which also produced a significant flux of neutrons at Earth (Watanabe et al 2003), along with strong sub-THz emission (Raulin et al 2004). Various aspects of this flare have been discussed in numerous papers (e.g., Livshits et al 2006;Kuznetsov et al 2006;Grechnev et al 2013).…”

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confidence: 99%

A Large-scale Plume in an X-class Solar Flare

Fleishman

Nita

Gary

2017

ApJ

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Ever-increasing multi-frequency imaging of solar observations suggests that solar flares often involve more than one magnetic fluxtube. Some of the fluxtubes are closed, while others can contain open field. The relative proportion of nonthermal electrons among those distinct loops is highly important for understanding the energy release, particle acceleration, and transport. The access of nonthermal electrons to the open field is further important as the open field facilitates the solar energetic particle (SEP) escape from the flaring site, and thus controls the SEP fluxes in the solar system, both directly and as seed particles for further acceleration. The large-scale fluxtubes are often filled with a tenuous plasma, which is difficult to detect in either EUV or X-ray wavelengths; however, they can dominate at low radio frequencies, where a modest component of nonthermal electrons can render the source optically thick and, thus, bright enough to be observed. Here we report detection of a large-scale 'plume' at the impulsive phase of an X-class solar flare, SOL2001-08-25T16:23, using multi-frequency radio data from Owens Valley Solar Array. To quantify the flare spatial structure, we employ 3D modeling utilizing force-free-field extrapolations from the line-of-sight SOHO/MDI magnetograms with our modeling tool GX Simulator. We found that a significant fraction of the nonthermal electrons accelerated at the flare site low in the corona escapes to the plume, which contains both closed and open field. We propose that the proportion between the closed and open field at the plume is what determines the SEP population escaping into interplanetary space.

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confidence: 99%

A Large-scale Plume in an X-class Solar Flare

Fleishman

Nita

Gary

2017

ApJ

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“…HEND records are somewhat more complex to evaluate than SEP because both scintillators are sensitive to neutrons, charged particles, and energetic photons (Livshits et al, ). As Livshits et al (, ) and Hurley et al () describe, the energy intervals that both scintillators can record are 60 keV–2 MeV for the inner detector and 30 keV–1 MeV for the outer detector. The inner scintillator energy range includes radiation caused by the large number of electrons with energies ~100 keV, which produce gamma rays at the detector.…”

Section: Observationsmentioning

confidence: 95%

“…Previous studies of flare detections by HEND showed that the typical duration of a flare as recorded by this instrument is ~10–12 min, normally associated with photons with energy between 80 and 300 keV, having a sharp increase in counts, and are then followed by a slower decay. Moreover, a typical flare, if detected by HEND, does so independently of its position around the planet (see, e.g., Livshits et al, ; Livshits et al, ). We note that HEND's view of the Sun during this period was never obstructed by Mars, as the Sun was always in the FOV of Mars Odyssey throughout the Siding Spring encounter.…”

Section: Observationsmentioning

confidence: 99%

Energetic Particle Showers Over Mars from Comet C/2013 A1 Siding Spring

et al. 2018

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This paper is a phenomenological description of multispacecraft observations of energetic particles caused by the close flyby of comet C/2013 A1 Siding Spring with Mars on 19 October 2014. This is the first time that cometary energetic particles have been observed at Mars. The Mars Atmosphere and Volatile EvolutioN (MAVEN)-solar energetic particle (SEP) and the Mars Odyssey-High Energy Neutron Detector (HEND) instruments recorded evidence of precipitating particles, which are likely O + pickup ions, during the~10 hr that Mars was within the region of the comet's coma. O + pickup ions were also detected several hours after, although whether their origin is the comet or space weather is not conclusive. We discuss the possible origin of those particles and also the cause of an additional shower of energetic particles that HEND observed between 22 and 35 hr after the comet's closest approach, which may be related to dust impacts from the comet's dust tail. An O + pickup ion energy flux simulation is performed with representative solar wind and cometary conditions, together with a simulation of their energy deposition profile in the atmosphere of Mars. Results indicate that the O + pickup ion fluxes observed by SEP were deposited in the ionosphere around 105 to 120 km altitude, and they are compared with precomet flyby estimations of cometary pickup ions. The comet's flyby deposited a significant fluence of energetic particles into Mars' upper atmosphere, at a similar level to a large space weather event.

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“…[6,72,61]). We use the data on particles with energies between ∼195 keV -1000 keV ( [37]) provided by the outer scintillator.…”

Section: Instrumentationmentioning

confidence: 99%

Interaction of Space Weather Phenomena with Mars Plasma Environment During Solar Minimum 23/24

et al. 2021

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We study the interaction of three solar wind (SW) structures, two stream interaction regions, and one interplanetary coronal mass ejection, with Mars’ plasma environment during November 20–27, 2007. This period corresponds to the solar minimum between the solar cycles 23 and 24 which was characterized by very low values of the SW density and dynamic pressure and low interplanetary magnetic field magnitude. During that time the Mars Express orbit was in the terminator plane, while the Earth, Sun, and Mars were almost aligned, so we use the Advance Composition Explorer and Solar Terrestrial Relations Observatory probes as SW monitors in order to identify and characterize the structures that later hit Mars. We find that the passage of these structures caused strong variations in the bow shock location (between 2.2 and 3.0 RM), compression of the magnetospheric cavity (up to 45%), and an increased transterminator flow below 2 RM (by a factor of ≤ 8). This study shows that during times of low solar activity, modest space weather phenomena may cause large variations of plasma flow at Mars.

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Stereoscopic observations of solar flares made onboard the 2001 Mars Odyssey spacecraft and CORONAS-F satellite

Cited by 5 publications

References 1 publication

A Large-scale Plume in an X-class Solar Flare

A Large-scale Plume in an X-class Solar Flare

Energetic Particle Showers Over Mars from Comet C/2013 A1 Siding Spring

Interaction of Space Weather Phenomena with Mars Plasma Environment During Solar Minimum 23/24

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