000 04251nam a22005655i 4500
001 978-981-97-6414-3
003 DE-He213
005 20251030113041.0
007 cr nn 008mamaa
008 240913s2024 si | s |||| 0|eng d
020 _a9789819764143
_9978-981-97-6414-3
024 7 _a10.1007/978-981-97-6414-3
_2doi
050 4 _aQB460-466
072 7 _aPHVB
_2bicssc
072 7 _aSCI005000
_2bisacsh
072 7 _aPHVB
_2thema
100 1 _aAbe, Daisei.
_eauthor.
_4aut
_4http://id.loc.gov/vocabulary/relators/aut
_984260
245 1 0 _aFormation and Evolution of Star-Forming Filaments in Molecular Clouds
_h[electronic resource] /
_cby Daisei Abe.
250 _a1st ed. 2024.
264 1 _aSingapore :
_bSpringer Nature Singapore :
_bImprint: Springer,
_c2024.
300 _aXII, 99 p. 47 illus., 43 illus. in color.
_bonline resource.
336 _atext
_btxt
_2rdacontent
337 _acomputer
_bc
_2rdamedia
338 _aonline resource
_bcr
_2rdacarrier
347 _atext file
_bPDF
_2rda
490 1 _aSpringer Theses, Recognizing Outstanding Ph.D. Research,
_x2190-5061
505 0 _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.
520 _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.
650 0 _aAstrophysics.
_968037
650 0 _aPlasma astrophysics.
_973287
650 0 _aPlasma waves.
_969749
650 0 _aPlasma turbulence.
_977282
650 1 4 _aAstrophysics.
_968037
650 2 4 _aAstrophysical Plasma.
_973288
650 2 4 _aWaves, instabilities and nonlinear plasma dynamics.
_969750
650 2 4 _aTurbulence in plasmas.
_977283
710 2 _aSpringerLink (Online service)
773 0 _tSpringer Nature eBook
776 0 8 _iPrinted edition:
_z9789819764136
776 0 8 _iPrinted edition:
_z9789819764150
776 0 8 _iPrinted edition:
_z9789819764167
830 0 _aSpringer Theses, Recognizing Outstanding Ph.D. Research,
_x2190-5061
_966370
856 4 0 _uhttps://doi.org/10.1007/978-981-97-6414-3
912 _aZDB-2-PHA
912 _aZDB-2-SXP
999 _c63363
_d63363