Shalchi Andreas (24 results)

Condition: As New. Unread book in perfect condition.

Condition: As New. Unread book in perfect condition.

Condition: New.

Condition: New.

Condition: New. In English.

Condition: New.

Hardback. Condition: New. If charged particles move through the interplanetary or interstellar medium, they interact with a large-scale magnetic ?eld such as the magnetic ?eld of the Sun or the Galactic magnetic ?eld. As these background ?elds are usually nearly constant in time and space, they can be approximated by a homogeneous ?eld. If there are no additional ?elds, the particle trajectory is a perfect helix along which the par- cle moves at a constant speed. In reality, however, there are turbulent electric and magnetic?elds dueto the interstellaror solar wind plasma. These ?elds lead to sc- tering of the cosmic rays parallel and perpendicular to the background ?eld. These scattering effects, which usually are of diffusive nature, can be described by s- tial diffusion coef?cients or, alternatively, by mean free paths. The knowledge of these parameters is essential for describing cosmic ray propagation as well as d- fusive shock acceleration. The latter process is responsible for the high cosmic ray energies that have been observed. The layout of this book is as follows. In Chap. 1, the general physical scenario is presented. We discuss fundamental processes such as cosmic ray propagation and acceleration in different systems such as the solar system or the interst- lar space. These processes are a consequence of the interaction between charged cosmic particles and an astrophysical plasma (turbulence). The properties of such plasmas are therefore the subject of Chap. 2.…

Condition: New. A science monograph presenting the forefront of cosmic ray diffusion theoryIf charged particles move through the interplanetary or interstellar medium, they interact with a large-scale magnetic ?eld such as the magnetic ?eld of the Sun or the Gal.

Condition: New. pp. 216.

Buch. Condition: Neu. Druck auf Anfrage Neuware - Printed after ordering - If charged particles move through the interplanetary or interstellar medium, they interact with a large-scale magnetic eld such as the magnetic eld of the Sun or the Galactic magnetic eld. As these background elds are usually nearly constant in time and space, they can be approximated by a homogeneous eld. If there are no additional elds, the particle trajectory is a perfect helix along which the par- cle moves at a constant speed. In reality, however, there are turbulent electric and magnetic elds dueto the interstellaror solar wind plasma. These elds lead to sc- tering of the cosmic rays parallel and perpendicular to the background eld. These scattering effects, which usually are of diffusive nature, can be described by s- tial diffusion coef cients or, alternatively, by mean free paths. The knowledge of these parameters is essential for describing cosmic ray propagation as well as d- fusive shock acceleration. The latter process is responsible for the high cosmic ray energies that have been observed. The layout of this book is as follows. In Chap. 1, the general physical scenario is presented. We discuss fundamental processes such as cosmic ray propagation and acceleration in different systems such as the solar system or the interst- lar space. These processes are a consequence of the interaction between charged cosmic particles and an astrophysical plasma (turbulence). The properties of such plasmas are therefore the subject of Chap. 2.…

Taschenbuch. Condition: Neu. Druck auf Anfrage Neuware - Printed after ordering - If charged particles move through the interplanetary or interstellar medium, they interact with a large-scale magnetic eld such as the magnetic eld of the Sun or the Galactic magnetic eld. As these background elds are usually nearly constant in time and space, they can be approximated by a homogeneous eld. If there are no additional elds, the particle trajectory is a perfect helix along which the par- cle moves at a constant speed. In reality, however, there are turbulent electric and magnetic elds dueto the interstellaror solar wind plasma. These elds lead to sc- tering of the cosmic rays parallel and perpendicular to the background eld. These scattering effects, which usually are of diffusive nature, can be described by s- tial diffusion coef cients or, alternatively, by mean free paths. The knowledge of these parameters is essential for describing cosmic ray propagation as well as d- fusive shock acceleration. The latter process is responsible for the high cosmic ray energies that have been observed. The layout of this book is as follows. In Chap. 1, the general physical scenario is presented. We discuss fundamental processes such as cosmic ray propagation and acceleration in different systems such as the solar system or the interst- lar space. These processes are a consequence of the interaction between charged cosmic particles and an astrophysical plasma (turbulence). The properties of such plasmas are therefore the subject of Chap. 2.…

Hardcover. Condition: Brand New. 1st edition. 199 pages. 9.25x6.25x0.50 inches. In Stock.

Condition: New. In English.

Condition: Sehr gut. Zustand: Sehr gut | Sprache: Englisch | Produktart: Bücher | If charged particles move through the interplanetary or interstellar medium, they interact with a large-scale magnetic ?eld such as the magnetic ?eld of the Sun or the Galactic magnetic ?eld. As these background ?elds are usually nearly constant in time and space, they can be approximated by a homogeneous ?eld. If there are no additional ?elds, the particle trajectory is a perfect helix along which the par- cle moves at a constant speed. In reality, however, there are turbulent electric and magnetic?elds dueto the interstellaror solar wind plasma. These ?elds lead to sc- tering of the cosmic rays parallel and perpendicular to the background ?eld. These scattering effects, which usually are of diffusive nature, can be described by s- tial diffusion coef?cients or, alternatively, by mean free paths. The knowledge of these parameters is essential for describing cosmic ray propagation as well as d- fusive shock acceleration. The latter process is responsible for the high cosmic ray energies that have been observed. The layout of this book is as follows. In Chap. 1, the general physical scenario is presented. We discuss fundamental processes such as cosmic ray propagation and acceleration in different systems such as the solar system or the interst- lar space. These processes are a consequence of the interaction between charged cosmic particles and an astrophysical plasma (turbulence). The properties of such plasmas are therefore the subject of Chap. 2.…

Hardback. Condition: New. If charged particles move through the interplanetary or interstellar medium, they interact with a large-scale magnetic ?eld such as the magnetic ?eld of the Sun or the Galactic magnetic ?eld. As these background ?elds are usually nearly constant in time and space, they can be approximated by a homogeneous ?eld. If there are no additional ?elds, the particle trajectory is a perfect helix along which the par- cle moves at a constant speed. In reality, however, there are turbulent electric and magnetic?elds dueto the interstellaror solar wind plasma. These ?elds lead to sc- tering of the cosmic rays parallel and perpendicular to the background ?eld. These scattering effects, which usually are of diffusive nature, can be described by s- tial diffusion coef?cients or, alternatively, by mean free paths. The knowledge of these parameters is essential for describing cosmic ray propagation as well as d- fusive shock acceleration. The latter process is responsible for the high cosmic ray energies that have been observed. The layout of this book is as follows. In Chap. 1, the general physical scenario is presented. We discuss fundamental processes such as cosmic ray propagation and acceleration in different systems such as the solar system or the interst- lar space. These processes are a consequence of the interaction between charged cosmic particles and an astrophysical plasma (turbulence). The properties of such plasmas are therefore the subject of Chap. 2.…

Condition: new. Questo è un articolo print on demand.

Condition: new. Questo è un articolo print on demand.

Buch. Condition: Neu. This item is printed on demand - it takes 3-4 days longer - Neuware -If charged particles move through the interplanetary or interstellar medium, they interact with a large-scale magnetic eld such as the magnetic eld of the Sun or the Galactic magnetic eld. As these background elds are usually nearly constant in time and space, they can be approximated by a homogeneous eld. If there are no additional elds, the particle trajectory is a perfect helix along which the par- cle moves at a constant speed. In reality, however, there are turbulent electric and magnetic elds dueto the interstellaror solar wind plasma. These elds lead to sc- tering of the cosmic rays parallel and perpendicular to the background eld. These scattering effects, which usually are of diffusive nature, can be described by s- tial diffusion coef cients or, alternatively, by mean free paths. The knowledge of these parameters is essential for describing cosmic ray propagation as well as d- fusive shock acceleration. The latter process is responsible for the high cosmic ray energies that have been observed. The layout of this book is as follows. In Chap. 1, the general physical scenario is presented. We discuss fundamental processes such as cosmic ray propagation and acceleration in different systems such as the solar system or the interst- lar space. These processes are a consequence of the interaction between charged cosmic particles and an astrophysical plasma (turbulence). The properties of such plasmas are therefore the subject of Chap. 2. 216 pp. Englisch.…

Condition: New. Dieser Artikel ist ein Print on Demand Artikel und wird nach Ihrer Bestellung fuer Sie gedruckt. A science monograph presenting the forefront of cosmic ray diffusion theoryIf charged particles move through the interplanetary or interstellar medium, they interact with a large-scale magnetic ?eld such as the magnetic ?eld of the Sun or the Gal.…

Buch. Condition: Neu. This item is printed on demand - Print on Demand Titel. Neuware -If charged particles move through the interplanetary or interstellar medium, they interact with a large-scale magnetic eld such as the magnetic eld of the Sun or the Galactic magnetic eld. As these background elds are usually nearly constant in time and space, they can be approximated by a homogeneous eld. If there are no additional elds, the particle trajectory is a perfect helix along which the par- cle moves at a constant speed. In reality, however, there are turbulent electric and magnetic elds dueto the interstellaror solar wind plasma. These elds lead to sc- tering of the cosmic rays parallel and perpendicular to the background eld. These scattering effects, which usually are of diffusive nature, can be described by s- tial diffusion coef cients or, alternatively, by mean free paths. The knowledge of these parameters is essential for describing cosmic ray propagation as well as d- fusive shock acceleration. The latter process is responsible for the high cosmic ray energies that have been observed. The layout of this book is as follows. In Chap. 1, the general physical scenario is presented. We discuss fundamental processes such as cosmic ray propagation and acceleration in different systems such as the solar system or the interst- lar space. These processes are a consequence of the interaction between charged cosmic particles and an astrophysical plasma (turbulence). The properties of such plasmas are therefore the subject of Chap. 2.Springer-Verlag KG, Sachsenplatz 4-6, 1201 Wien 216 pp. Englisch.…

Taschenbuch. Condition: Neu. This item is printed on demand - Print on Demand Titel. Neuware -If charged particles move through the interplanetary or interstellar medium, they interact with a large-scale magnetic eld such as the magnetic eld of the Sun or the Galactic magnetic eld. As these background elds are usually nearly constant in time and space, they can be approximated by a homogeneous eld. If there are no additional elds, the particle trajectory is a perfect helix along which the par- cle moves at a constant speed. In reality, however, there are turbulent electric and magnetic elds dueto the interstellaror solar wind plasma. These elds lead to sc- tering of the cosmic rays parallel and perpendicular to the background eld. These scattering effects, which usually are of diffusive nature, can be described by s- tial diffusion coef cients or, alternatively, by mean free paths. The knowledge of these parameters is essential for describing cosmic ray propagation as well as d- fusive shock acceleration. The latter process is responsible for the high cosmic ray energies that have been observed. The layout of this book is as follows. In Chap. 1, the general physical scenario is presented. We discuss fundamental processes such as cosmic ray propagation and acceleration in different systems such as the solar system or the interst- lar space. These processes are a consequence of the interaction between charged cosmic particles and an astrophysical plasma (turbulence). The properties of such plasmas are therefore the subject of Chap. 2.Springer-Verlag KG, Sachsenplatz 4-6, 1201 Wien 216 pp. Englisch.…

Condition: New. Print on Demand pp. 216 49 Illus.

Condition: New. PRINT ON DEMAND pp. 216.

Taschenbuch. Condition: Neu. This item is printed on demand - it takes 3-4 days longer - Neuware -If charged particles move through the interplanetary or interstellar medium, they interact with a large-scale magnetic eld such as the magnetic eld of the Sun or the Galactic magnetic eld. As these background elds are usually nearly constant in time and space, they can be approximated by a homogeneous eld. If there are no additional elds, the particle trajectory is a perfect helix along which the par- cle moves at a constant speed. In reality, however, there are turbulent electric and magnetic elds dueto the interstellaror solar wind plasma. These elds lead to sc- tering of the cosmic rays parallel and perpendicular to the background eld. These scattering effects, which usually are of diffusive nature, can be described by s- tial diffusion coef cients or, alternatively, by mean free paths. The knowledge of these parameters is essential for describing cosmic ray propagation as well as d- fusive shock acceleration. The latter process is responsible for the high cosmic ray energies that have been observed. The layout of this book is as follows. In Chap. 1, the general physical scenario is presented. We discuss fundamental processes such as cosmic ray propagation and acceleration in different systems such as the solar system or the interst- lar space. These processes are a consequence of the interaction between charged cosmic particles and an astrophysical plasma (turbulence). The properties of such plasmas are therefore the subject of Chap. 2. 216 pp. Englisch.…