First observations of energetic particles near comet Halley

Somogyi, A.; Gringauz, K. I.; Szegö, K.; Szabó, László; Kozma, Gergely Tibor; Remizov, A. P.; Erö, J.; Klimenko, I. N.; Szűcs, I.; Веригин, М. И.; Windberg, J.; Cravens, T. E.; Dyachkov, A.; Erdö́s, G.; Farago, M.; Gombosi, T. I.; Kecskeméty, K.; Keppler, E.; Kovács, T.; Kondor, A.; Logachev, Y. I.; Lohonyai, L.; Marsden, R. G.; Redl, Robert; Richter, A. K.; Stolpovskii, V. G.; Szabó, József; Szentpétery, I.; Szepesváry, A.; Tátrallyay, M.; Varga, A.; Vladimirova, G. A.; Wenzel, K. P.; Zarándy, Ákos

doi:10.1038/321285a0

Cited by 75 publications

(16 citation statements)

References 11 publications

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“…VOYAGER ENERGETIC PARTICLE OBSERVATIONS 169 ed with these bow shocks although the origin of these ions is most likely the planetary magnetosphere itself (Sarris et al, 1976;Zwickl et al, 1980) Finally, we now have observation of cometary ions at relatively high energies, suggesting some acceleration via solar wind pickup and, potentially, through interaction with the cometary shock (Somogyi et al, 1986).…”

Section: Introductionmentioning

confidence: 82%

Voyager energetic particle observations at interplanetary shocks and upstream of planetary bow shocks: 1977?1990

Krimigis

1992

Space Sci Rev

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ABSTRACT. The Voyager 1 and 2 spacecraft include instrumentation that makes comprehensive ion (E ~> 28 keV) and electron (E _> 22 keV) measurements in several energy channels with good temporal, energy, and compositional resolution. Data collected over the past decade (1977)(1978)(1979)(1980)(1981)(1982)(1983)(1984)(1985)(1986)(1987)(1988), including observations upstream and downstream of four planetary bow shocks (Earth, Jupiter, Saturn, Uranus) and numerous interplanetary shocks to -30 AU, are reviewed and analyzed in the context of the Fermi and shock drift acceleration (SDA) models. Principal findings upstream of planetary bow shocks include the simultaneous presence of ions and electrons, detection of "tracer" ions characteristic of the parent magnetosphere (O, S, O +), power-law energy spectra extending to _> 5 MeV, and large (up to 100:1) anisotropies. Results from interplanetary shocks include observation of acceleration to the highest energies ever seen in a shock (~> 22 MeV for protons, >~ 220 MeV for oxygen), the "saturation" in energy gain to ~< 300 keV at quasi-parallel shocks, the observation of shock-accelerated relativistic electrons, and separation of high-energy (upstream) from low-energy (downstream) populations to within -1 particle gyroradius in a near-perpendicular shock. The overall results suggest that ions and electrons observed upstream of planetary bow shocks have their source inside the parent magnetosphere, with first order Fermi acceleration playing a secondary role at best. Further, that quasi-perpendicular interplanetary shocks accelerate ions and electrons most efficiently to high energies through the shock-drift process. These findings suggest that great care must be exercised in the application of concepts developed for heliosphere shocks to cosmic ray acceleration through shocks at supernova remnants.

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Section: Introductionmentioning

confidence: 82%

Voyager energetic particle observations at interplanetary shocks and upstream of planetary bow shocks: 1977?1990

Krimigis

1992

Space Sci Rev

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“…21: http://nssdc.gsfc.nasa.gov/nmc/experimentDisplay.do?id=1984-128A-11. 22: Somogyi et al (1986). 23: Kivelson et al (1992).…”

Section: A Brief Overview Of Space Physics Exploration At Venusmentioning

confidence: 99%

Solar Wind Interaction and Impact on the Venus Atmosphere

et al. 2017

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Venus has intrigued planetary scientists for decades because of its huge contrasts to Earth, in spite of its nickname of "Earth's Twin". Its invisible upper atmosphere and space environment are also part of the larger story of Venus and its evolution. In 60s to 70s, several missions (Venera and Mariner series) explored Venus-solar wind interaction regions. They identified the basic structure of the near-Venus space environment, for example, existence of the bow shock, magnetotail, ionosphere, as well as the lack of the intrinsic magnetic field. A huge leap in knowledge about the solar wind interaction with Venus was made possible by the 14-year long mission, Pioneer Venus Orbiter (PVO), launched in 1978. More recently, ESA's probe, Venus Express (VEX), was inserted into orbit in 2006, operated for 8 years.Owing to its different orbit from that of PVO, VEX made unique measurements in the polar and terminator regions, and probed the near-Venus tail for the first time. The near-tail hosts dynamic processes that lead to plasma energization. These processes in turn lead to the loss of ionospheric ions to space, slowly eroding the Venusian atmosphere. VEX carried an ion spectrometer with a moderate mass-separation capability and the observed ratio of the escaping hydrogen and oxygen ions in the wake indicates the stoichiometric loss of water from Venus. The structure and dynamics of the induced magnetosphere depends on the prevailing solar wind conditions. VEX studied the response of the magnetospheric system on different time scales. A plethora of waves was identified by the magnetometer on VEX; some of them were not previously observed by PVO. Proton cyclotron waves were seen far upstream of the bow shock, mirror mode waves were observed in magnetosheath and whistler mode waves, possibly generated by lightning discharges were frequently seen. VEX also encouraged renewed numerical modeling efforts, including fluid-type of models and particle-fluid hybrid type of models, describing the plasma interaction on scales ranging from ion gyro radius to the entire induced magnetosphere. In this review article, we review what has been found from space physics measurements around Venus (from the solar wind down to the ionopause), with a particular emphasis on updated results since the Venus Express mission. We conclude the article by a short discussion on the remaining open scientific questions and the future of this field.

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“…On the other hand the very extensive atmospheres around comets imply important effects, as has been indicated by recent measurements near comets Giacobini-Zinner and Halley (Mendis et al, 1986;Gringauz et al, 1986;Somogyi et al, 1986). The presence of a hot oxygen corona makes this mass loading effect an important one at Venus.…”

Section: Discussionmentioning

confidence: 86%

The effect of the hot oxygen corona on the interaction of the solar wind with Venus

Belot︠s︡erkovskiĭ¹,

Бреус²,

Крымский³

et al. 1987

Geophysical Research Letters

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A numerical gas dynamic model, which includes the effects of mass loading of the shocked solar wind, was used to calculate the density and magnetic field variations in the magnetosheath of Venus. These calculations were carried out for conditions corresponding to a specific orbit of the Pioneer Venus Orbiter (PVO orbit 582). A comparison of the model predictions and the measured shock position, density and magnetic field values showed a reasonable agreement, indicating that a gas dynamic model that includes the effects of mass loading can be used to predict these parameters.

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First observations of energetic particles near comet Halley

Cited by 75 publications

References 11 publications

Voyager energetic particle observations at interplanetary shocks and upstream of planetary bow shocks: 1977?1990

Voyager energetic particle observations at interplanetary shocks and upstream of planetary bow shocks: 1977?1990

Solar Wind Interaction and Impact on the Venus Atmosphere

The effect of the hot oxygen corona on the interaction of the solar wind with Venus

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