solanki s k (21 Ergebnisse)

Zustand: New. In.

Zustand: Fair. This is an ex-library book and may have the usual library/used-book markings inside.This book has hardback covers. In fair condition, suitable as a study copy. No dust jacket. Please note the Image in this listing is a stock photo and may not match the covers of the actual item,950grams, ISBN:9780521420068.

Hardcover. Zustand: New. Zustand des Schutzumschlags: New. 1st Edition. Contents: Preface. 1. Rapid analysis of spatial a b and y diversities of birds in a landmosaic in Manipur/Rajkumari Ashalata Devi and Laishangbam Sanjit. 2. Diversity and status of lycaenids Lepidoptera: lycaenidae) in central Nepal/B. Khanal, M.K. Chalise and G.S. Solanki. 3. Wildlife and their behavior in Baghmara Buffer zone community forest, Nepal/B.K. Sharma, M.K. Chalise and G.S. Solanki. 4. Importance of biodiversity conservation and its role in management of diverse forest resource production with special reference to NEH region, India/Bandi Gopichand and Bandi Diddi Naidu. 5. Poetential benefits to biodiversity by using marine renewable energy/Guruswaamy. 6. Plants used in hair care by the ethnic communities in thoubal district of Manipur/Mohd. Habibullah Khan and P.S. Yadava. Conservation biology is concerned with phenomena that affect the maintenance, loss and restoration of biodiversity and the science of sustaining evolutionary processes that engender genetic population species and ecosystem diversity. The concern stems from estimates suggesting that up to 50% of all species on the planet will disappear within the next 50 years, which has contributed to poverty, starvation and will reset the course of evolution on this planet. The present book provides and introduction to the environment biodiversity and traditional system and is the compilation of various papers contributed by learned community from different part of the world.

Hardcover. Zustand: Very Good. No Jacket. Hardback copy, no dustjacket as issued. 428pp. Charts and graphs throughout. Not library copy, no inscriptions. (45/4).

Hardcover Jul 08, 2009. Zustand: gebraucht; wie neu.

Zustand: New. In.

Zustand: New. In.

Zustand: Sehr gut. Zustand: Sehr gut | Seiten: 436 | Sprache: Englisch | Produktart: Bücher | Starting in 1995 numerical modeling of the Earth¿s dynamo has ourished with remarkable success. Direct numerical simulation of convection-driven MHD- ow in a rotating spherical shell show magnetic elds that resemble the geomagnetic eld in many respects: they are dominated by the axial dipole of approximately the right strength, they show spatial power spectra similar to that of Earth, and the magnetic eld morphology and the temporal var- tion of the eld resembles that of the geomagnetic eld (Christensen and Wicht 2007). Some models show stochastic dipole reversals whose details agree with what has been inferred from paleomagnetic data (Glatzmaier and Roberts 1995; Kutzner and Christensen 2002; Wicht 2005). While these models represent direct numerical simulations of the fundamental MHD equations without parameterized induction effects, they do not match actual pla- tary conditions in a number of respects. Speci cally, they rotate too slowly, are much less turbulent, and use a viscosity and thermal diffusivity that is far too large in comparison to magnetic diffusivity. Because of these discrepancies, the success of geodynamo models may seem surprising. In order to better understand the extent to which the models are applicable to planetary dynamos, scaling laws that relate basic properties of the dynamo to the fundamental control parameters play an important role. In recent years rst attempts have been made to derive such scaling laws from a set of numerical simulations that span the accessible parameter space (Christensen and Tilgner 2004; Christensen and Aubert 2006).

Paperback. Zustand: Brand New. 436 pages. 9.25x6.10x1.03 inches. In Stock.

Hardcover. Zustand: Brand New. 1st edition. 430 pages. 9.29x0.87x0.31 inches. In Stock.

Taschenbuch. Zustand: Neu. Druck auf Anfrage Neuware - Printed after ordering - Starting in 1995 numerical modeling of the Earth's dynamo has ourished with remarkable success. Direct numerical simulation of convection-driven MHD- ow in a rotating spherical shell show magnetic elds that resemble the geomagnetic eld in many respects: they are dominated by the axial dipole of approximately the right strength, they show spatial power spectra similar to that of Earth, and the magnetic eld morphology and the temporal var- tion of the eld resembles that of the geomagnetic eld (Christensen and Wicht 2007). Some models show stochastic dipole reversals whose details agree with what has been inferred from paleomagnetic data (Glatzmaier and Roberts 1995; Kutzner and Christensen 2002; Wicht 2005). While these models represent direct numerical simulations of the fundamental MHD equations without parameterized induction effects, they do not match actual pla- tary conditions in a number of respects. Speci cally, they rotate too slowly, are much less turbulent, and use a viscosity and thermal diffusivity that is far too large in comparison to magnetic diffusivity. Because of these discrepancies, the success of geodynamo models may seem surprising. In order to better understand the extent to which the models are applicable to planetary dynamos, scaling laws that relate basic properties of the dynamo to the fundamental control parameters play an important role. In recent years rst attempts have been made to derive such scaling laws from a set of numerical simulations that span the accessible parameter space (Christensen and Tilgner 2004; Christensen and Aubert 2006).

Buch. Zustand: Neu. Druck auf Anfrage Neuware - Printed after ordering - Starting in 1995 numerical modeling of the Earth's dynamo has ourished with remarkable success. Direct numerical simulation of convection-driven MHD- ow in a rotating spherical shell show magnetic elds that resemble the geomagnetic eld in many respects: they are dominated by the axial dipole of approximately the right strength, they show spatial power spectra similar to that of Earth, and the magnetic eld morphology and the temporal var- tion of the eld resembles that of the geomagnetic eld (Christensen and Wicht 2007). Some models show stochastic dipole reversals whose details agree with what has been inferred from paleomagnetic data (Glatzmaier and Roberts 1995; Kutzner and Christensen 2002; Wicht 2005). While these models represent direct numerical simulations of the fundamental MHD equations without parameterized induction effects, they do not match actual pla- tary conditions in a number of respects. Speci cally, they rotate too slowly, are much less turbulent, and use a viscosity and thermal diffusivity that is far too large in comparison to magnetic diffusivity. Because of these discrepancies, the success of geodynamo models may seem surprising. In order to better understand the extent to which the models are applicable to planetary dynamos, scaling laws that relate basic properties of the dynamo to the fundamental control parameters play an important role. In recent years rst attempts have been made to derive such scaling laws from a set of numerical simulations that span the accessible parameter space (Christensen and Tilgner 2004; Christensen and Aubert 2006).

Zustand: New. In.

Zustand: New. In.

Taschenbuch. Zustand: Neu. Druck auf Anfrage Neuware - Printed after ordering - The discovery of chemical elements in celestial bodies and the first estimates of the chemical composition of the solar atmosphere were early results of Astrophysics - the subdiscipline of Astronomy that was originally concerned with the general laws of radiation and with spectroscopy. Following the initial quantitative abundance studies by Henry Norris Russell and by Cecilia Payne-Gaposchkin, a tremendous amount of theoretical, observa tional, laboratory and computational work led to a steadily improving body of knowledge of photospheric abundances - a body of knowledge that served to guide the theory of stellar evolution. Solar abundances determined from photospheric spectra, together with the very similar abundances determined from carbonaceous chondrites (where extensive information on isotopic composition is available as well), are nowadays the reference for all cosmic composition measures. Early astrophysical studies of the solar photospheric composition made use of atmosphere models and atomic data. Consistent abundances derived from different atmospheric layers and from lines of different strength helped to confirm and estab lish both models and atomic data, and eventually led to the now accepted, so-called 'absolute' abundance values - which, for practical reasons, however, are usually given relative to the number of hydrogen nuclei.

Buch. Zustand: Neu. Druck auf Anfrage Neuware - Printed after ordering - The discovery of chemical elements in celestial bodies and the first estimates of the chemical composition of the solar atmosphere were early results of Astrophysics - the subdiscipline of Astronomy that was originally concerned with the general laws of radiation and with spectroscopy. Following the initial quantitative abundance studies by Henry Norris Russell and by Cecilia Payne-Gaposchkin, a tremendous amount of theoretical, observa tional, laboratory and computational work led to a steadily improving body of knowledge of photospheric abundances - a body of knowledge that served to guide the theory of stellar evolution. Solar abundances determined from photospheric spectra, together with the very similar abundances determined from carbonaceous chondrites (where extensive information on isotopic composition is available as well), are nowadays the reference for all cosmic composition measures. Early astrophysical studies of the solar photospheric composition made use of atmosphere models and atomic data. Consistent abundances derived from different atmospheric layers and from lines of different strength helped to confirm and estab lish both models and atomic data, and eventually led to the now accepted, so-called 'absolute' abundance values - which, for practical reasons, however, are usually given relative to the number of hydrogen nuclei.

Paperback. Zustand: Brand New. reprint edition. 428 pages. 9.50x6.25x1.25 inches. In Stock.

Hardcover. Zustand: Brand New. 444 pages. 9.50x6.50x1.00 inches. In Stock.

Zustand: New. Proceedings of an ISSI Workshop, 26-30 January 1998, Bern, Switzerland Editor(s): Frohlich, Claus; Huber, Martin C. E.; Solanki, S. K. (Institute of Astronomy, ETH, Zurich, Switzerland); von Steiger, Rudolf. Series: Space Sciences Series of ISSI. Num Pages: 431 pages, biography. BIC Classification: PGM. Category: (P) Professional & Vocational; (UP) Postgraduate, Research & Scholarly. Dimension: 235 x 155 x 25. Weight in Grams: 926. . 1998. Reprinted from SPACE SCIENCE REVIEWS, 85:1-2, 199. Hardback. . . . . Books ship from the US and Ireland.

Hardcover. Zustand: gut. 1998. Solar Composition and its Evolution from Core to Corona : Proceedings of an ISSI Workshop 2630 January 1998, Bern, Switzerland In deutscher Sprache. pages.

Hardcover. Zustand: Sehr gut. sehr gut, near FINE - lager nur a-916 Language: DEU.