Basics of the Solar Wind

Basics of the Solar Wind

The topics are treated at various levels of difficulty both qualitatively and quantitatively. This book will appeal to graduate students and researchers in earth and atmospheric sciences, and astrophysics.

Author: Nicole Meyer-Vernet

Publisher: Cambridge University Press

ISBN: 9781139461559

Category: Science

Page:

View: 566

The Sun continually ejects matter into space, blowing a huge bubble of supersonic plasma. This solar wind bathes the whole solar system and shapes all planetary environments. The growth of space technology has considerably increased our knowledge of this medium. This 2007 book presents an introduction to the subject, starting with basic principles and including all the latest advances from space exploration and theory. It contains a short introduction to plasma physics and discusses the structure of the solar interior and atmosphere, the production of solar wind and its perturbations. It explains the objects of the Solar System, from dust to comets and planets, and their interaction with the solar wind. The final sections explore the astrophysical point of view. The topics are treated at various levels of difficulty both qualitatively and quantitatively. This book will appeal to graduate students and researchers in earth and atmospheric sciences, and astrophysics.
Categories: Science

Solar Wind Ten

Solar Wind Ten

The Tenth Solar Wind conference describes the latest results in the physics of the outer solar atmosphere, the solar wind, and the interplanetary medium which together comprise the heliosphere.

Author: Marco Velli

Publisher: American Institute of Physics

ISBN: 0735401489

Category: Science

Page: 860

View: 348

The Tenth Solar Wind conference describes the latest results in the physics of the outer solar atmosphere, the solar wind, and the interplanetary medium which together comprise the heliosphere. The conference brought together researchers studying the sun and its influence on the earth’s space environment both from an experimental and theoretical point of view. The effect of the solar magnetic field in shaping and accelerating the solar wind throughout the solar cycle, via coronal heating and coronal mass ejections was described in unprecedented clarity and breadth, thanks to both satellite experiments and numerical modelling. The conference proceedings is of interest to researchers in space science and the geomagnetic effects of solar activity, plasma physicists and astrophysicists as well as other scientists interested in the life of our mother star.
Categories: Science

The Solar Wind

The Solar Wind

The solar wind is found to have a considerable effect on the lunar atmosphere. First, the calculated density of the lunar atmosphere is greatly reduced by collisions with protons in the solar wind.

Author: J. R. Herring

Publisher:

ISBN: NASA:31769000456866

Category: Solar wind

Page: 14

View: 806

"Parker's model of a spherically expanding corona, the "solar wind," is compared with D.E. Blackwell's observations of the 1954 minimum equatorial corona. A significant discrepancy is found between the predicted and the observed electron densities at distances from the sun greater than 20 solar radii. Blackwell's data are found to be consistent with a model in which the corona expands mostly within a disk less than 25 solar radii thick, lying within the sun's equatorial plane. The thickness of the disk as a function of distance from the sun is qualitatively explained in terms of magnetic pressure. The solar wind is found to have a considerable effect on the lunar atmosphere. First, the calculated density of the lunar atmosphere is greatly reduced by collisions with protons in the solar wind. If the flux of particles in this wind has the conventional values ranging between 10(exp 10) to 10(exp 11) per sq cm-sec, the calculations yield a lunar pressure of 10(exp -13) atmosphere of argon, in agreement with the value predicted by Elsmore and Whitfield on the basis of observations on the occultation of radio stars. Second, following a suggestion by Gold, it was found that the collisions of solar-wind protons with the lunar surface produce an atmosphere of cold neutral hydrogen with a density of 10(exp 5) per cu cm at the lunar surface. The density falls off at greater distances in accordance with the inverse-square law. Estimates indicate that the interaction of solar particles with the neutral hydrogen will produce an extended lunar ionosphere with a density of the order of 400 protons/cu cm in the vicinity of the moon."
Categories: Solar wind

The Solar Wind and the Earth

The Solar Wind and the Earth

As a star, the sun is continuously emitting an enormous amount of energy 33 into space, up to as much as 3. 9 X 10 erg/ s. This energy emission consists of three modes.

Author: Syun-Ichi Akasofu

Publisher: Springer

ISBN: 9027724725

Category: Science

Page: 316

View: 204

As a star, the sun is continuously emitting an enormous amount of energy 33 into space, up to as much as 3. 9 X 10 erg/ s. This energy emission consists of three modes. Almost all the energy is emitted in the form of the familiar black-body radiation, commonly called sunlight. Although the amount of energy emitted is small, the sun also emits x rays, extreme ultraviolet (EUV), and UV radiations, which are absorbed above the earth's stratosphere. These constitute the second mode of solar energy, separate from the black-body radiation that penetrates the lower layers of the atmosphere. The sun has another important mode of energy emission in which the energy is carried out by charged particles. These particles have a very wide range of energies, from less than I keY to more than I GeV. Because of this wide range, it is convenient to group them into two components: particles with energies greater than 10 keY and the lower-energy particles. The former are generally referred to as solar protons or solar cosmic rays; their emission is associated with active features on the sun. Their interaction with the atmosphere is similar to that of the x ray and EUV radiation. Low-energy particles constitute plasma, a gas of equal numbers of positive and negative particles. Actually, this plasma is the outermost part of the solar atmosphere, namely the corona, which blows out continuously . For this reason, the plasma flow is called the solar wind.
Categories: Science

The Sun the Solar Wind and the Heliosphere

The Sun  the Solar Wind  and the Heliosphere

This volume represents the state of the art of the science covered by the International Association of Geomagnetism and Aeronomy (IAGA) Division IV: Solar Wind and Interplanetary Field.

Author: Mari Paz Miralles

Publisher: Springer Science & Business Media

ISBN: 9048197872

Category: Science

Page: 384

View: 747

This volume represents the state of the art of the science covered by the International Association of Geomagnetism and Aeronomy (IAGA) Division IV: Solar Wind and Interplanetary Field. It contains a collection of contributions by top experts addressing and reviewing a variety of topics included under the umbrella of the division. It covers subjects that extend from the interior of the Sun to the heliopause, and from the study of physical processes in the Sun and the solar wind plasma to space weather forecasts. The book is organized in 6 parts: the solar interior, the solar atmosphere, the heliosphere, heliophysical processes, radio emissions, and coordinated science in the Sun-Earth system. In addition, we highlight some of the results presented during the IAGA Division IV symposia in the 11th Scientific Assembly of IAGA in Sopron, Hungary, on 23-30 August 2009, which was planned simultaneously with this book.
Categories: Science

The Solar Wind

The Solar Wind

Author: Robert J. Mackin

Publisher:

ISBN: UOM:39015008418264

Category: Cosmic physics

Page: 400

View: 253

Categories: Cosmic physics

Coronal Expansion and Solar Wind

Coronal Expansion and Solar Wind

The present volume is an attempt to synthesize the solar wind observations and coronal expansion models from this decade of rapid development.

Author: A. J. Hundhausen

Publisher: Springer Science & Business Media

ISBN: 9783642654145

Category: Science

Page: 238

View: 530

Little more than ten years have passed since spaceprobe-borne instruments con clusively demonstrated the existence of the solar wind. These observations con firmed the basic validity of a theoretical model, first proposed by E. N. Parker, predicting a continuous, rapid expansion of the solar corona. The subsequent decade has seen a tremendous growth in both the breadth and sophistication of solar wind observations; the properties of the interplanetary plasma near the orbit of the earth are now known in great detail. The theory of the coronal ex pansion has also been highly refilled both in the sense of including additional physical processes, and of treating more realistic (time-dependent and non spheri cally-symmetric) coronal boundary conditions. The present volume is an attempt to synthesize the solar wind observations and coronal expansion models from this decade of rapid development. The ultimate goal is, of course, the interpretation of observed solar wind phenomena as the effects of basic physical processes occurring in the coronal and interplanetary plasma and as the natural manifestations of solar properties and structures. This approach implies an emphasis upon the "large-scale" features revealed by the observations. It requires extensive use of the concepts and methods of fluid mechanics.
Categories: Science

Solar Wind Nine Proceedings of the Ninth International Solar Wind Conference

Solar Wind Nine  Proceedings of the Ninth International Solar Wind Conference

The Solar Wind Nine Conference was the ninth in the series of solar wind conferences established in 1964 by Dr. Marcia Neugebauer to provide a forum for the interaction between solar physicists and space physicists interested in the origin ...

Author: Ruth Esser

Publisher: Amer Inst of Physics

ISBN: STANFORD:36105023642569

Category: Medical

Page: 859

View: 165

The Solar Wind Nine Conference was the ninth in the series of solar wind conferences established in 1964 by Dr. Marcia Neugebauer to provide a forum for the interaction between solar physicists and space physicists interested in the origin and evolution of the solar wind. One of the scientific goals of the conference was to reflect the importance of the synergistic interaction between theory, numerical modeling and simulations, in situ measurements and remote sensing observations, in the exploration of the solar wind. Indeed, the opportunity provided by the many concurrent missions Ulysses, Yohkoh, SOHO, TRACE, SPARTAN, WIND, and ACE, which probe the Sun and interplanetary space from different vantage points, provided very rich material for the contributions. The presentations included invited reviews and contributed talks as well as poster presentations. This conference took place almost 40 years after Parkers prediction of the existence of the solar wind.
Categories: Medical

Solar Wind Seven

Solar Wind Seven

PREFACE The International Conference Solar Wind Seven was held in Goslar (
Germany) from September 15 to 21, 1991. The large number of 214 participating
scientists from 22 countries exceeded all our expectations. What attracted them ...

Author: E. Marsch

Publisher: Elsevier

ISBN: 9781483287805

Category: Science

Page: 740

View: 640

The third COSPAR Colloquium entitled Solar Wind Seven was held in Goslar, Germany in September 1991. Twenty-two countries were represented by scientists, many of whom are leading experts in the area of heliospheric physics. The Proceedings reflect current research on solar wind and particularly emphasizes the source regions. The main topics covered encompass Coronal Heating and Solar Wind Acceleration; Large-Scale Structure of the Interplanetary Medium; Minor Ions, Neutrals and Cosmic Rays in the Heliosphere; Kinetic Physics, Waves and Turbulence and finally Heliospheric Dynamic Phenomena.
Categories: Science

In the Solar Wind

In the Solar Wind

The 1984 winner of the National Poetry Series Competition focuses on the theme of boundaries--between land and sea, the physical and the spiritual, and the waking world and dreams, as well as those of time, the universe, and the mind

Author: Wendy Battin

Publisher: Doubleday Books

ISBN: STANFORD:36105037830226

Category: Poetry

Page: 69

View: 574

The 1984 winner of the National Poetry Series Competition focuses on the theme of boundaries--between land and sea, the physical and the spiritual, and the waking world and dreams, as well as those of time, the universe, and the mind
Categories: Poetry

Solar Wind Five

Solar Wind Five

Author: Marcia Neugebauer

Publisher:

ISBN: NASA:31769000466311

Category:

Page: 742

View: 778

Categories:

Solar Corona and Solar Wind

Solar Corona and Solar Wind

Author: COSPAR. Plenary Meeting

Publisher:

ISBN: UOM:39015024420120

Category: Solar wind

Page: 410

View: 969

Categories: Solar wind

Turbulent Heating and Anisotropy in the Solar Wind

Turbulent Heating and Anisotropy in the Solar Wind

Miyake W, Mukai T, Terasawa T, Hirao K (1988) Stream interaction as a heat
source in the solar wind. Sol Phys 117(1):171–178. https://doi.org/10.1007/
BF00148580 Narita Y, Glassmeier KH, Sahraoui F, Goldstein ML (2010) Wave-
vector ...

Author: Victor Montagud-Camps

Publisher: Springer Nature

ISBN: 9783030303839

Category: Science

Page: 123

View: 916

This book presents two important new findings. First, it demonstrates from first principles that turbulent heating offers an explanation for the non-adiabatic decay of proton temperature in solar wind. Until now, this was only proved with reduced or phenomenological models. Second, the book demonstrates that the two types of anisotropy of turbulent fluctuations that are observed in solar wind at 1AU originate not only from two distinct classes of conditions near the Sun but also from the imbalance in Alfvén wave populations. These anisotropies do not affect the overall turbulent heating if we take into account the relation observed in solar wind between anisotropy and Alfvén wave imbalance. In terms of the methods used to obtain these achievements, the author shows the need to find a very delicate balance between turbulent decay and expansion losses, so as to directly solve the magnetohydrodynamic equations, including the wind expansion effects.
Categories: Science