LEADER 04185nam 22006495 450 001 9910887882503321 005 20250807143347.0 010 $a9789819764143 010 $a9819764149 024 7 $a10.1007/978-981-97-6414-3 035 $a(MiAaPQ)EBC31674245 035 $a(Au-PeEL)EBL31674245 035 $a(CKB)35309371300041 035 $a(DE-He213)978-981-97-6414-3 035 $a(EXLCZ)9935309371300041 100 $a20240913d2024 u| 0 101 0 $aeng 135 $aurcnu|||||||| 181 $ctxt$2rdacontent 182 $cc$2rdamedia 183 $acr$2rdacarrier 200 10$aFormation and Evolution of Star-Forming Filaments in Molecular Clouds /$fby Daisei Abe 205 $a1st ed. 2024. 210 1$aSingapore :$cSpringer Nature Singapore :$cImprint: Springer,$d2024. 215 $a1 online resource (109 pages) 225 1 $aSpringer Theses, Recognizing Outstanding Ph.D. Research,$x2190-5061 311 08$a9789819764136 311 08$a9819764130 320 $aIncludes bibliographical references. 327 $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. 330 $aThis book clears up some confusion in the field of star formation and proposes a solution to a problem that remains unsolved for more than a decade. Observations of molecular clouds show that dense filaments are the sites of present-day star formation, and it is thus necessary to understand the filament formation process because the filament is an initial condition in a star formation process. Theoretical studies suggest that shock waves in molecular clouds trigger filament formation. Several different mechanisms have been proposed, and the formation mechanism of the observed star-forming filaments is expected to be clarified. In this book, the author performs a series of isothermal magnetohydrodynamics (MHD) simulations of filament formation and identifies the formation mechanisms. It is found that the dominant filament formation mode changes with the velocity of the shock waves that trigger the filament formation. The filament width plays an important role in determining the fragmentation scale by self-gravity, and observations show that the width 0.1 pc is universal. On the other hand, in theory the width of the supercritical filaments was considered to be narrowed by self-gravity. Recent studies suggest that massive filaments are bound by the slow shocks that are caused by accretion flows onto the filaments. Since the wavefront of such a slow shock is known to be unstable as a slow shock instability (SSI), the accretion ram pressure is expected to be converted into thermal/turbulent pressure across the shock front, which potentially maintains the width. In the scale of dense filaments, ambipolar diffusion (AD) suppresses the SSI at small scales. The influence of AD on SSI is investigated using two-dimensional MHD simulations, and the nonlinear evolution of the SSI with AD is found to drive turbulences. The book demonstrate the effect of SSI including AD onto the filament evolution. 410 0$aSpringer Theses, Recognizing Outstanding Ph.D. Research,$x2190-5061 606 $aAstrophysics 606 $aPlasma astrophysics 606 $aPlasma waves 606 $aPlasma turbulence 606 $aAstrophysics 606 $aAstrophysical Plasma 606 $aWaves, instabilities and nonlinear plasma dynamics 606 $aTurbulence in plasmas 615 0$aAstrophysics. 615 0$aPlasma astrophysics. 615 0$aPlasma waves. 615 0$aPlasma turbulence. 615 14$aAstrophysics. 615 24$aAstrophysical Plasma. 615 24$aWaves, instabilities and nonlinear plasma dynamics. 615 24$aTurbulence in plasmas. 676 $a523.88 700 $aAbe$b Daisei$01846143 801 0$bMiAaPQ 801 1$bMiAaPQ 801 2$bMiAaPQ 906 $aBOOK 912 $a9910887882503321 996 $aFormation and Evolution of Star-Forming Filaments in Molecular Clouds$94430238 997 $aUNINA