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1. |
Record Nr. |
UNINA9910806285703321 |
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Titolo |
Best care at lower cost : the path to continuously learning health care in America / / Committee on the Learning Health Care System in America, The Institute of Medicine ; Mark Smith [and three others], editors |
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Pubbl/distr/stampa |
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Washington, District of Columbia : , : National Academies Press, , [2013] |
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©2013 |
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ISBN |
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Descrizione fisica |
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1 online resource (437 p.) |
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Disciplina |
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Soggetti |
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Medical care - United States |
Medical policy - United States |
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Lingua di pubblicazione |
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Formato |
Materiale a stampa |
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Livello bibliografico |
Monografia |
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Note generali |
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Description based upon print version of record. |
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Nota di bibliografia |
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Includes bibliographical references. |
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Nota di contenuto |
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Introduction and overview -- Imperative : managing rapidly increasing complexity -- Imperative : achieving greater value in health care -- Imperative : capturing opportunities from technology, industry, and policy -- A continuously learning health care system -- Generating and applying knowledge in real time -- Engaging patients, families, and communities -- Achieving and rewarding high-value care -- Creating a new culture of care -- Actions for continuous learning, best care, and lower costs. |
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2. |
Record Nr. |
UNINA9910887882503321 |
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Autore |
Abe Daisei |
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Titolo |
Formation and Evolution of Star-Forming Filaments in Molecular Clouds / / by Daisei Abe |
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Pubbl/distr/stampa |
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Singapore : , : Springer Nature Singapore : , : Imprint : Springer, , 2024 |
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ISBN |
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Edizione |
[1st ed. 2024.] |
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Descrizione fisica |
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1 online resource (109 pages) |
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Collana |
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Springer Theses, Recognizing Outstanding Ph.D. Research, , 2190-5061 |
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Disciplina |
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Soggetti |
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Astrophysics |
Plasma astrophysics |
Plasma waves |
Plasma turbulence |
Astrophysical Plasma |
Waves, instabilities and nonlinear plasma dynamics |
Turbulence in plasmas |
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Lingua di pubblicazione |
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Formato |
Materiale a stampa |
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Livello bibliografico |
Monografia |
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Nota di bibliografia |
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Includes bibliographical references. |
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Nota di contenuto |
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Introduction -- Classification of Filament Formation Mechanisms -- The Effect of Shock Wave Duration on Star Formation and the Initial Condition of Massive Cluster Formation -- Filament Evolution Process -- Conclusion. |
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Sommario/riassunto |
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This book clears up some confusion in the field of star formation and proposes a solution to a problem that remains unsolved for more than a decade. Observations of molecular clouds show that dense filaments are the sites of present-day star formation, and it is thus necessary to understand the filament formation process because the filament is an initial condition in a star formation process. Theoretical studies suggest that shock waves in molecular clouds trigger filament formation. Several different mechanisms have been proposed, and the formation mechanism of the observed star-forming filaments is expected to be clarified. In this book, the author performs a series of isothermal magnetohydrodynamics (MHD) simulations of filament formation and |
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identifies the formation mechanisms. It is found that the dominant filament formation mode changes with the velocity of the shock waves that trigger the filament formation. The filament width plays an important role in determining the fragmentation scale by self-gravity, and observations show that the width 0.1 pc is universal. On the other hand, in theory the width of the supercritical filaments was considered to be narrowed by self-gravity. Recent studies suggest that massive filaments are bound by the slow shocks that are caused by accretion flows onto the filaments. Since the wavefront of such a slow shock is known to be unstable as a slow shock instability (SSI), the accretion ram pressure is expected to be converted into thermal/turbulent pressure across the shock front, which potentially maintains the width. In the scale of dense filaments, ambipolar diffusion (AD) suppresses the SSI at small scales. The influence of AD on SSI is investigated using two-dimensional MHD simulations, and the nonlinear evolution of the SSI with AD is found to drive turbulences. The book demonstrate the effect of SSI including AD onto the filament evolution. |
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