東華大學圖書館 |

Language: English

Help

回圖書館首頁

手機版館藏查詢

Back

Switch To: Labeled | MARC Mode | ISBD

Formation and evolution of star-form...

Abe, Daisei.

Linked to FindBook

Google Book

Amazon

博客來

Formation and evolution of star-forming filaments in molecular clouds

Record Type:	Electronic resources : Monograph/item
Title/Author:	Formation and evolution of star-forming filaments in molecular clouds/ by Daisei Abe.
Author:	Abe, Daisei.
Published:	Singapore :Springer Nature Singapore : : 2024.,
Description:	xii, 99 p. :ill. (chiefly color), digital ;24 cm.
Notes:	"Doctoral thesis accepted by Nagoya University, Nagoya, Japan."
[NT 15003449]:	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.
Contained By:	Springer Nature eBook
Subject:	Stars - Formation. -
Online resource:	https://doi.org/10.1007/978-981-97-6414-3
ISBN:	9789819764143

Formation and evolution of star-forming filaments in molecular clouds
Abe, Daisei.

Formation and evolution of star-forming filaments in molecular clouds[electronic resource] /by Daisei Abe. - Singapore :Springer Nature Singapore :2024. - xii, 99 p. :ill. (chiefly color), digital ;24 cm. - Springer theses,2190-5061. - Springer theses..

"Doctoral thesis accepted by Nagoya University, Nagoya, Japan."

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.

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 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.

ISBN: 9789819764143

Standard No.: 10.1007/978-981-97-6414-3doiSubjects--Topical Terms:

777194
Stars
--Formation.

LC Class. No.: QB806

Dewey Class. No.: 523.8

Formation and evolution of star-forming filaments in molecular clouds
LDR:03255nmm a2200349 a 4500 001 2375379
003 DE-He213
005 20240913130234.0
006 m d
007 cr nn 008maaau
008 241231s2024 si s 0 eng d
020 $a 9789819764143 $q (electronic bk.)
020 $a 9789819764136 $q (paper)
024 7 $a 10.1007/978-981-97-6414-3 $2 doi
035 $a 978-981-97-6414-3
040 $a GP $c GP
041 0 $a eng
050 4 $a QB806
072 7 $a PHVB $2 bicssc
072 7 $a SCI005000 $2 bisacsh
072 7 $a PHVB $2 thema
082 0 4 $a 523.8 $2 23
090 $a QB806 $b .A138 2024
100 1 $a Abe, Daisei. $3 3724868
245 1 0 $a Formation and evolution of star-forming filaments in molecular clouds $h [electronic resource] / $c by Daisei Abe.
260 $a Singapore : $b Springer Nature Singapore : $b Imprint: Springer, $c 2024.
300 $a xii, 99 p. : $b ill. (chiefly color), digital ; $c 24 cm.
490 1 $a Springer theses, $x 2190-5061
500 $a "Doctoral thesis accepted by Nagoya University, Nagoya, Japan."
505 0 $a 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.
520 $a 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 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 $a Stars $x Formation. $3 777194
650 0 $a Astrophysics. $3 535904
650 2 4 $a Astrophysical Plasma. $3 3606556
650 2 4 $a Waves, instabilities and nonlinear plasma dynamics. $3 3592701
650 2 4 $a Turbulence in plasmas. $3 3595790
710 2 $a SpringerLink (Online service) $3 836513
773 0 $t Springer Nature eBook
830 0 $a Springer theses. $3 1314442
856 4 0 $u https://doi.org/10.1007/978-981-97-6414-3
950 $a Physics and Astronomy (SpringerNature-11651)