04045nam a22005175i 4500001001800000003000900018005001700027007001500044008004100059020003700100024003500137050001400172072001700186072002300203072001600226100008100242245011500323250001800438264007200456300006400528336002600592337002600618338003600644347002400680490007200704505022300776520192300999650002502922650003202947650002502979650003003004650002503034650003303059650006303092650003403155710003403189773002603223776003603249776003603285776003603321830007903357856004603436912001403482912001403496999001703510978-981-97-6414-3DE-He21320251030113041.0cr nn 008mamaa240913s2024    si |    s    |||| 0|eng d  a97898197641439978-981-97-6414-37 a10.1007/978-981-97-6414-32doi 4aQB460-466 7aPHVB2bicssc 7aSCI0050002bisacsh 7aPHVB2thema1 aAbe, Daisei.eauthor.4aut4http://id.loc.gov/vocabulary/relators/aut98426010aFormation and Evolution of Star-Forming Filaments in Molecular Cloudsh[electronic resource] /cby Daisei Abe.  a1st ed. 2024. 1aSingapore :bSpringer Nature Singapore :bImprint: Springer,c2024.  aXII, 99 p. 47 illus., 43 illus. in color.bonline resource.  atextbtxt2rdacontent  acomputerbc2rdamedia  aonline resourcebcr2rdacarrier  atext filebPDF2rda1 aSpringer Theses, Recognizing Outstanding Ph.D. Research,x2190-50610 aIntroduction -- 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.  aThis 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 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. 0aAstrophysics.968037 0aPlasma astrophysics.973287 0aPlasma waves.969749 0aPlasma turbulence.97728214aAstrophysics.96803724aAstrophysical Plasma.97328824aWaves, instabilities and nonlinear plasma dynamics.96975024aTurbulence in plasmas.9772832 aSpringerLink (Online service)0 tSpringer Nature eBook08iPrinted edition:z978981976413608iPrinted edition:z978981976415008iPrinted edition:z9789819764167 0aSpringer Theses, Recognizing Outstanding Ph.D. Research,x2190-506196637040uhttps://doi.org/10.1007/978-981-97-6414-3  aZDB-2-PHA  aZDB-2-SXP  c63363d63363