Date & Time: 2024/Feb./22 (Thu.) 17:00-18:00, Venue: Zoom TV Conference System. This is an informal seminar on the formation of stars and planets. We welcome anyone interested in the subject.

Title:  Formation and Evolution of Star-forming Filaments in Molecular Clouds

Speaker:  安部 大晟 (名古屋大学)

Abstract: 

Observations of molecular clouds indicate that dense filaments are the sites for present-day star formation. Therefore, it is crucial to understand filament formation and evolution, as these filaments provide the initial conditions for star formation. The width of filaments is a significant factor as it determines the fragmentation scale through self-gravity and affects the stellar masses to be formed. Observations suggest that the width has a universal value of 0.1 pc, regardless of the filament's line mass. However, theoretical predictions suggest that the width of supercritical filaments (> 17 solar masses per pc) should contract due to self-gravity. Most simulations show a much narrower width due to strong gravity for massive filaments, and why massive filaments maintain their width of 0.1 pc has remained unexplained for more than ten years. Recent studies suggest that massive filaments (~100 solar masses per pc) are bound by slow mode shocks resulting from accretion flows onto the filaments. The wavefront of the slow mode shock is known to be unstable, and the corrugation of the shock front grows. This corrugation converts the accretion flow's ram pressure into thermal/turbulent pressure across the shock front, possibly maintaining the filament's width. In this study, we perform non-ideal MHD simulations to investigate filament evolution via slow-shock instability, considering ambipolar diffusion, which is effective in dense filaments. We discovered slow-shock instability including ambipolar diffusion drives anisotropic turbulence in the massive filament, named this new mechanism the "bullet mechanism". We also conducted a simulation considering self-gravity and found that the bullet mechanism can sustain a realistic filament width, even for a filament as massive as ~100 solar masses per pc.

他、会議報告、速報など、飛び入りも歓迎します。今回もしくは次回以降、話題提供できる方は世話人までメールしていただけましたら幸いです。 

Participants: 29,  Affiliations: 12 

Participants list:

Ibaraki U.  B4 Takumi Matsunaga 

JAMSTEC PD Sota Arakawa

Kagoshima U. D1 Yudai Kobayashi

Kobe U. DA Kenji Kurosaki 

Kogakuin U. AP Takayuki Muto

Kyushu U. D3 Asako Sato, M2 AyumuShosi, M2 Yuki Akaike, M2 Shingo Nozaki, M2 Takashi Shimokawa, M1 Mitsuki Omura

Nagoya U. P Shu-ichiro Inutsuka, A Valeska Valdivia, PD Daisei Abe, D2 Kanta Kitajima, D1 Ryushi Miyayama, M2 Izumi SENO, M1 Wataru Takahashi, M1 Onogawa Kenshin

NAOJ PD Yoshiaki Misugi, RS Gabriel Guimarães 

RIKEN PD Ryosuke Tominaga

Shiga-U medical AP Kazutaka Motoyama

Tokyo Tech B4 Issei Kojima, B4 Kazuki Ehara

U. Tokyo P Takeru SUZUKI, M2 Kanako Narita, M2 Yuto Komichi

Unknown: Anri MIZUNO

次回：2024/Apr./11  

連絡世話人：冨永遼佑（理化学研究所） ryosuke.tominaga[at]riken.jp