Comet Halley remote plasma tail observations and in situ solar wind properties: VEGA- IMF/plasma observations and ground-based optical observations from 1 December 1985 to 1 May 1986

1991 ◽  
Vol 39 (5) ◽  
pp. 697-708 ◽  
Author(s):  
Magda Delva ◽  
Konrad Schwingenschuh ◽  
Malcolm B. Niedner ◽  
Konstantin I. Gringauz
Keyword(s):  
Solar Wind ◽  
Optical Observations ◽  
Remote Plasma ◽  
Plasma Tail ◽  
Comet Halley

Comets: pre- and post-Halley

1991 ◽  
Vol 9 (2) ◽  
pp. 219-224
Author(s):  
K. S. Krishna Swamy
Keyword(s):  
Solar Wind ◽  
Intensive Study ◽  
Cometary Plasma ◽  
Comet Halley ◽  
Insight Into

AbstractThe recent intensive study of Comet Halley based on in situ measurements, observations carried out with rockets and satellites and supplemented with co-ordinated Earth based observations has not only confirmed pre-Halley results, but also has given new insight into the nature of the nucleus, dust, gas and the interaction of cometary plasma with the solar wind. These observations also have raised many new questions and problems. Several of these aspects will be discussed. For a better understanding of these problems, the planned future missions to comets will also be discussed.

scholarly journals The Global Interaction of Comets with the Solar Wind

1991 ◽  
Vol 116 (2) ◽  
pp. 1125-1144 ◽  
Author(s):  
K. R. Flammer
Keyword(s):  
Solar Wind ◽  
Heliocentric Distance ◽  
Theoretical Models ◽  
Bow Shock ◽  
Flow Transition ◽  
The Sun ◽  
In Situ Observations ◽  
Comet Halley

AbstractThe global interaction of the solar wind with a comet as it orbits the Sun is reviewed. After a brief survey of the flow transition regions observed at comet Halley is presented, theoretical models are given for the cometocentric distance of the bow shock, the cometopause, and the ionopause. In addition, predictions are made as to what heliocentric distance these boundaries should form at. The results of these models are compared with the in situ observations at comet Halley.

scholarly journals Plasma Dynamics in Mercury’s Magnetosphere

2005 ◽  
Vol 13 ◽  
pp. 67-69
Author(s):  
Wing-Huen Ip
Keyword(s):  
Solar Wind ◽  
Space Weather ◽  
Optical Observations ◽  
Surface Plasma ◽  
Plasma Dynamics ◽  
Weather Effects ◽  
Interaction Processes ◽  
Atomic Sodium ◽  
Sodium And Potassium

AbstractMercury is in all sense of the words still Terra Incognito, its magnetosphere is hence little known. The only source of knowledge came from the in-situ measurements by the Mariner 10 close encounters in 1974. This has been complemented since by ground-based observations of the atomic sodium and potassium emissions in the vicinity of the planetary disk. This series of optical observations has produced intriguing evidence of magnetospheric and/or solar wind effects on the surface-plasma interaction processes. In this review we will describe the current theories of the corresponding space weather effects.

scholarly journals The International Cometary Explorer (ICE) Mission to comet Giacobini-Zinner (G/Z)

1985 ◽  
Vol 83 ◽  
pp. 405-414
Author(s):  
J.C. Brandt ◽  
R.W. Farquhar ◽  
S.P. Maran ◽  
M.B. Niedner ◽  
T. von Rosenvinge
Keyword(s):  
Solar Wind ◽  
September 11 ◽  
Solar Wind Interaction ◽  
Downstream Side ◽  
Pass Through ◽  
Comet Halley

AbstractThe ICE spacecraft will pass through the tail of P/Giacobini-Zinner on September 11, 1985, to make in situ measurements of particles, fields, and waves that will contribute significantly to the knowledge of plasma tails and other aspects of the cometary/solar wind interaction. By obtaining data on the downstream side of G/Z, the ICE will complement the later upstream measurements obtained by the Comet Halley probes.

scholarly journals Power Spectral Analysis of Enhanced Scintillation of Quasar 3C459 Due to Comet Halley

1992 ◽  
Vol 45 (1) ◽  
pp. 115 ◽  
Author(s):  
P Janardhan ◽  
SK Alurkar ◽  
AD Bobra ◽  
OB Slee ◽  
D Waldron
Keyword(s):  
Solar Wind ◽  
Spectral Analysis ◽  
Power Spectral Analysis ◽  
Density Variation ◽  
Scale Size ◽  
Power Spectral ◽  
Plasma Tail ◽  
Halley's Comet ◽  
Electron Density Variation ◽  
Comet Halley

The radio source 2314+038 (3C459) showed enhanced scintillations on three days at a solar elongation of about 90� as the plasma tail of Halley's Comet swept across it on six days during 16-21 December 1985. If we assume that the plasma velocities in the tail were not constant everywhere, but increased linearly from about 50 kms-1 at the tail axis to the normal average solar wind velocity of 400 kms-1 at the edges where the tail merged with the solar wind, a power spectral analysis of the scintillations shows two ranges of the rms electron density variation t:..N and scale size a. In particular, these are a fine scale zone near the axis where a is in the range 9 to 27 km and t:..N in the range 2 to 5 cm -3 and a zone near the edges with a and t:..N in the ranges 100 to 265 km and 0�4 to 0�8 cm-3 respectively. The assumption of a single velocity of 100 kms-1 throughout the tail shows similar fine scales near the tail axis and large scales near the edges. The scale sizes in that case range from about 18 km at the axis to about 70 km at the edges, corresponding to t:..N of 3�3 and 0�85 cm-3 respectively. A comparison with the results obtained by Slee et al. (1987) shows that there is no radial variation of t:..N. The tail-lag is seen to playa crucial role in determining the correct occulting geometry and the path of the source through the tail.

Comparison of Heliospheric In Situ Data with the Quasi‐steady Solar Wind Models

2008 ◽  
Vol 674 (2) ◽  
pp. 1158-1166 ◽  
Author(s):  
S. T. Lepri ◽  
S. K. Antiochos ◽  
P. Riley ◽  
L. Zhao ◽  
T. H. Zurbuchen
Keyword(s):  
Solar Wind ◽  
In Situ Data

scholarly journals Dust in the Solar System

1989 ◽  
Vol 44 (10) ◽  
pp. 877-882 ◽  
Author(s):  
H. Fechtig
Keyword(s):  
Solar Irradiation ◽  
Dust Particles ◽  
Normal Density ◽  
Dust Grains ◽  
Cometary Dust ◽  
In Situ Experiments ◽  
Asteroidal Belt ◽  
Comet Halley ◽  
Cometary Origin

Abstract Properties of cometary dust particles are better known since the space missions to Comet Halley. Their properties (densities, atomic composition) are compared with relevant observations from lunar microcraters and in-situ experiments. At 1 AU in the eliptic, 2/3 of the dust grains are normal density particles, presumably of asteroidal origin and irregularly shaped, while the remaining 1/3 are low density particles, presumably of cometary origin, but due to solar irradiation in a processed state (corresponding to “Brownlee”-particles). Beyond the asteroidal belt only black cometary dust grains are observed which have recently been released from comet nuclei orbiting on highly eccentric trajectories.

Prospective White-light Imaging and In Situ Measurements of Quiescent Large-scale Solar-wind Streams from the Parker Solar Probe and Solar Orbiter

2018 ◽  
Vol 868 (2) ◽  
pp. 137 ◽  
Author(s):  
Ming Xiong ◽  
Jackie A. Davies ◽  
Xueshang Feng ◽  
Bo Li ◽  
Liping Yang ◽  
...  
Keyword(s):  
Solar Wind ◽  
White Light ◽  
Large Scale ◽  
In Situ Measurements ◽  
White Light Imaging

scholarly journals Asymmetric multifractal model for solar wind intermittent turbulence

2008 ◽  
Vol 15 (4) ◽  
pp. 615-620 ◽  
Author(s):  
A. Szczepaniak ◽  
W. M. Macek
Keyword(s):  
Solar Wind ◽  
Solar Maximum ◽  
Solar Wind Plasma ◽  
Intermittent Turbulence ◽  
Proposed Model ◽  
Scaling Parameters ◽  
Generalized Dimensions ◽  
Multifractal Nature ◽  
Turbulent Cascade

Abstract. We consider nonuniform energy transfer rate for solar wind turbulence depending on the solar cycle activity. To achieve this purpose we determine the generalized dimensions and singularity spectra for the experimental data of the solar wind measured in situ by Advanced Composition Explorer spacecraft during solar maximum (2001) and minimum (2006) at 1 AU. By determining the asymmetric singularity spectra we confirm the multifractal nature of different states of the solar wind. Moreover, for explanation of this asymmetry we propose a generalization of the usual so-called p-model, which involves eddies of different sizes for the turbulent cascade. Naturally, this generalization takes into account two different scaling parameters for sizes of eddies and one probability measure parameter, describing how the energy is transferred to smaller eddies. We show that the proposed model properly describes multifractality of the solar wind plasma.

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