Plasma processes at comet Churyumov–Gerasimenko: Expectations for Rosetta

2013 ◽  
Vol 79 (6) ◽  
pp. 1067-1070 ◽  
Author(s):  
D. A. MENDIS ◽  
M. HORÁNYI
Keyword(s):  
Solar Wind ◽  
Solar Radiation ◽  
Bow Shock ◽  
Short Paper ◽  
Wind Flow ◽  
The Sun ◽  
Cometary Plasma ◽  
Variable Nature ◽  
Solar Wind Flow ◽  
Comet 67P

AbstractThe Rosetta–Philae mission to comet 67P/Churyumov–Gerasimenko in 2014 will provide a unique opportunity to observe the variable nature of the interaction of a comet with the solar radiation and the solar wind, as the comet approaches the Sun. In this short paper we will focus on the varying global structure of the cometary plasma environment. Specifically we make predictions on the varying locations of the two basic transitions in the global, contaminated solar wind flow toward the comet: the outer bow shock and the ionopause.

Solar wind flow through the comet P/Halley bow shock

1988 ◽  
pp. 55-60
Author(s):  
A. J. Coates ◽  
A. D. Johnstone ◽  
M. F. Thomsen ◽  
V. Formisano ◽  
E. Amata ◽  
...  
Keyword(s):  
Solar Wind ◽  
Bow Shock ◽  
Wind Flow ◽  
Solar Wind Flow ◽  
Flow Through

(Non)-radial propagation of the solar wind flow

2020 ◽  
Author(s):  
Zdeněk Němeček ◽  
Tereza Ďurovcová ◽  
Jana Šafránková ◽  
Jiří Šimůnek ◽  
John D. Richardson ◽  
...  
Keyword(s):  
Solar Wind ◽  
Radial Velocity ◽  
Orbital Motion ◽  
Wind Flow ◽  
The Sun ◽  
Mars Express ◽  
The Earth ◽  
Solar Wind Flow ◽  
Magnetospheric Tail ◽  
Radial Propagation

<p>The solar wind aberration due to non-radial velocity components and the Earth orbital motion is important for the overall magnetosphere geometry because the magnetospheric tail is aligned with the solar wind flow. This paper investigates an evolution of non-radial components of the solar wind flow along the path from the Sun to 6 AU. A comparison of observations at 1 AU and closer to or further from the Sun based on measurements of many spacecraft at different locations in the heliosphere (Wind, ACE, Spektr-R, THEMIS B and C, Helios 1 and 2, Mars-Express, Voyager 1 and 2) shows that (i) the average values of non-radial components vary with the distance from the Sun and (ii) they differ according to solar wind streams.</p>

scholarly journals The infant bow shock: a new frontier at a weak activity comet

2018 ◽  
Vol 619 ◽  
pp. L2 ◽  
Author(s):  
Herbert Gunell ◽  
Charlotte Goetz ◽  
Cyril Simon Wedlund ◽  
Jesper Lindkvist ◽  
Maria Hamrin ◽  
...  
Keyword(s):  
Solar Wind ◽  
Oscillation Amplitude ◽  
Bow Shock ◽  
The Sun ◽  
New Frontier ◽  
Before And After ◽  
Magnetic Field Magnitude ◽  
Weak Activity ◽  
Comet 67P

The bow shock is the first boundary the solar wind encounters as it approaches planets or comets. The Rosetta spacecraft was able to observe the formation of a bow shock by following comet 67P/Churyumov–Gerasimenko toward the Sun, through perihelion, and back outward again. The spacecraft crossed the newly formed bow shock several times during two periods a few months before and after perihelion; it observed an increase in magnetic field magnitude and oscillation amplitude, electron and proton heating at the shock, and the diminution of the solar wind further downstream. Rosetta observed a cometary bow shock in its infancy, a stage in its development not previously accessible to in situ measurements at comets and planets.

Waves in the magnetic field and solar wind flow outside the bow shock at comet P/Halley

1988 ◽  
pp. 47-54 ◽  
Author(s):  
A. Johnstone ◽  
K. Glassmeier ◽  
M. Acuna ◽  
H. Borg ◽  
D. Bryant ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Bow Shock ◽  
Wind Flow ◽  
Solar Wind Flow ◽  
The Magnetic Field

scholarly journals Occurrence rate of magnetic holes between 0.72 and 1 AU: comparative study of Cluster and VEX data

2011 ◽  
Vol 29 (5) ◽  
pp. 717-722 ◽  
Author(s):  
O. A. Amariutei ◽  
S. N. Walker ◽  
T. L. Zhang
Keyword(s):  
Solar Wind ◽  
Occurrence Rate ◽  
Wind Flow ◽  
The Sun ◽  
Common Features ◽  
The Earth ◽  
Magnetic Field Magnitude ◽  
Solar Wind Flow ◽  
Stable Plasma ◽  
The Magnetic Field

Abstract. Localised depressions in the magnetic field magnitude, or magnetic holes, are common features in many regions of solar system plasma. Two distinct mechanisms for their generation have been proposed. The first proposed that the structures are generated locally, close to the point of observation. The alternative has been proposed by Russell et al. (2008), who suggest that the observed magnetic holes represent nonlinear mirror structures that can be carried by the solar wind over vast distances of mirror stable plasma. According to Russell et al. (2008), magnetic holes are created in the vicinity of the sun and are convected by the solar wind outward. Periods of Cluster 1 and VEX data when both spacecraft were connected by the solar wind flow have been considered in this study, in order to determine the evolution of the magnetic holes occurrence rate. The comparison of the magnetic holes occurrence near the Venus and the Earth supports the Russell et al. (2008) premise that they are generated closer to the Sun most likely somewhere within the orbit of Mercury.

Modelling the evolution of CMEs and their shocks through different solar wind structures

2020 ◽  
Author(s):  
Erika Palmerio ◽  
Christina Lee ◽  
Leila Mays ◽  
Dusan Odstrcil
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Vantage Point ◽  
Angular Width ◽  
Wind Flow ◽  
The Sun ◽  
Ambient Wind ◽  
Fast Wind ◽  
Solar Wind Flow ◽  
Ambient Solar Wind

<p>The evolution of coronal mass ejections (CMEs) as they travel away from the Sun is one of the major issues in heliophysics and space weather. After erupting, CMEs propagate outwards through the background solar wind flow, which in turn may significantly affect CME evolution by means of e.g. acceleration, deflection, and/or rotation. In order to determine to which extent the ambient wind can alter the speed, trajectory, and orientation of a CME, we run a series of 3D magnetohydrodynamics simulations (using the coupled solar–heliospheric WSA–Enlil model) to conduct a multi-vantage point study of the radial and longitudinal evolution of CME structures as they propagate up to Earth’s (1 AU) and Mars’ (1.5 AU) orbits. We explore a broad range of input CME parameters (initial radial speed, angular width) and ambient solar wind conditions (slow versus fast wind) to investigate the different evolutionary behaviours of CMEs and their driven shocks and sheath regions. To study the radial and longitudinal evolution for the modelled CME ejecta and shock events, we examine the resulting magnetic field and plasma time series at different heliocentric distances (0.5 AU, 1 AU, and 1.5 AU) and heliolongitudes (in 30° increments). This work will help establish a set of expected CME behaviours at Earth’s and Mars’ radial distances, which can be used for analysing real CME events.</p>

ULF waves in the foreshock formed by the radial IMF: their effect on solar wind sheath-like deflection

2020 ◽  
Author(s):  
Olga Gutynska ◽  
Jaroslav Urbář ◽  
Jana Šafránková ◽  
Zdeněk Němeček
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Statistical Study ◽  
Low Frequency ◽  
Bow Shock ◽  
Ulf Waves ◽  
Wind Flow ◽  
Solar Wind Flow ◽  
The Mean

<p>Particle reflection at the bow shock provides a source of free energy to drive local instabilities and turbulence within the foreshock. A variety of low-frequency fluctuations (up to 16 mHz) results from the interactions of back-streaming ions with the incoming solar wind flow. We report observations of low-frequency magnetosonic waves observed during intervals of a radial interplanetary magnetic field in the foreshock. A case study of simultaneous dual THEMIS spacecraft observations of asymmetrical fluctuations in V<sub>y</sub> is complemented by a statistical study of similar solar wind deflections in the foreshock.  Our moment calculations do not include the reflected particles as well as heavier ions, revealed the modulation of a solar wind core and deflection of the solar wind in the foreshock. This effect decreases with the distance from the bow shock. We conclude that large asymmetrical Vy velocity component fluctuations are typical for the foreshock formed by the radial IMF. The asymmetry of fluctuations changes the mean direction of the incoming solar wind flow within the foreshock leading to preconditioning prior to its encounter with the bow shock.</p>

Solar wind flow past Venus and its implications for the occurrence of the Kelvin–Helmholtz instability

2007 ◽  
Vol 55 (12) ◽  
pp. 1793-1803 ◽  
Author(s):  
H.K. Biernat ◽  
N.V. Erkaev ◽  
U.V. Amerstorfer ◽  
T. Penz ◽  
H.I.M. Lichtenegger
Keyword(s):  
Solar Wind ◽  
Wind Flow ◽  
Helmholtz Instability ◽  
Flow Past ◽  
Solar Wind Flow
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