scholarly journals Thermal and dynamical balance in dense molecular cloud cores

1997 ◽  
Vol 288 (3) ◽  
pp. 674-678 ◽  
Author(s):  
C. J. Clarke ◽  
J. E. Pringle
Keyword(s):  
Molecular Cloud ◽  
Dense Molecular Cloud ◽  
Dynamical Balance ◽  
Cloud Cores

scholarly journals From Diffuse Gas to Dense Molecular Cloud Cores

2020 ◽  
Vol 216 (5) ◽  
Author(s):  
Javier Ballesteros-Paredes ◽  
Philippe André ◽  
Patrick Hennebelle ◽  
Ralf S. Klessen ◽  
J. M. Diederik Kruijssen ◽  
...  
Keyword(s):  
Molecular Cloud ◽  
Dense Molecular Cloud ◽  
Cloud Cores

scholarly journals An origin of arc structures deeply embedded in dense molecular cloud cores

2015 ◽  
Vol 449 (1) ◽  
pp. L123-L127 ◽  
Author(s):  
Tomoaki Matsumoto ◽  
Toshikazu Onishi ◽  
Kazuki Tokuda ◽  
Shu-ichiro Inutsuka
Keyword(s):  
Molecular Cloud ◽  
Dense Molecular Cloud ◽  
Cloud Cores

MASSES: An SMA Large Project Surveying Protostars to Reveal How Stars Gain their Mass

2018 ◽  
Vol 14 (S345) ◽  
pp. 66-69
Author(s):  
Ian W. Stephens ◽  
Michael M. Dunham ◽  
Philip C. Myers ◽  
Riwaj Pokhrel ◽  
Tyler L. Bourke ◽  
...  
Keyword(s):  
Angular Momentum ◽  
Molecular Cloud ◽  
Low Mass Stars ◽  
Dense Molecular Cloud ◽  
Large Project ◽  
Disk Evolution ◽  
Low Mass ◽  
Mass Assembly ◽  
Cloud Cores ◽  
Collapse Process

AbstractLow-mass stars form from the gravitational collapse of dense molecular cloud cores. While a general consensus picture of this collapse process has emerged, many details on how mass is transferred from cores to stars remain poorly understood. MASSES (Mass Assembly of Stellar Systems and their Evolution with the SMA), an SMA large project, has just finished surveying all 74 Class 0 and Class I protostars in the nearby Perseus molecular cloud to reveal the interplay between fragmentation, angular momentum, and outflows in regulating accretion and setting the final masses of stars. Scientific highlights are presented in this proceedings, covering the topics of episodic accretion, hierarchical thermal Jeans fragmentation, angular momentum transfer, envelope grain sizes, and disk evolution.

scholarly journals Models for Dense Molecular Cloud Cores

1997 ◽  
Vol 489 (1) ◽  
pp. 122-142 ◽  
Author(s):  
Steven D. Doty ◽  
David A. Neufeld
Keyword(s):  
Molecular Cloud ◽  
Dense Molecular Cloud ◽  
Cloud Cores

scholarly journals Dense molecular cloud cores as a source of micrometer-sized grains in galaxies

2014 ◽  
Vol 100 ◽  
pp. 40-45 ◽  
Author(s):  
Hiroyuki Hirashita ◽  
Ryosuke S. Asano ◽  
Takaya Nozawa ◽  
Zhi-Yun Li ◽  
Ming-Chang Liu
Keyword(s):  
Molecular Cloud ◽  
Dense Molecular Cloud ◽  
Cloud Cores

scholarly journals Aperture synthesis CS and 98 GHz continuum observations of protostellar IRAS sources in Taurus

1991 ◽  
Vol 147 ◽  
pp. 353-356
Author(s):  
N. Ohashi ◽  
R. Kawabe ◽  
M. Hayashi ◽  
M. Ishiguro
Keyword(s):  
Molecular Cloud ◽  
Total Mass ◽  
T Tauri Stars ◽  
Continuum Emission ◽  
Beam Size ◽  
Dust Grains ◽  
Dynamical Mass ◽  
T Tauri ◽  
Cloud Cores ◽  
The Continuum

The CS (J = 2 — 1) line and 98 GHz continuum emission have been observed for 11 protostellar IRAS sources in the Taurus molecular cloud with resolutions of 2.6″−8.8″ (360 AU—1200 AU) using the Nobeyama Millimeter Array (NMA). The CS emission is detected only toward embedded sources, while the continuum emission from dust grains is detected only toward visible T Tauri stars except for one embedded source, L1551-IRS5. This suggests that the dust grains around the embedded sources do not centrally concentrate enough to be detected with our sensitivity (∼4 m Jy r.m.s), while dust grains in disks around the T Tauri stars have enough total mass to be detected with the NMA. The molecular cloud cores around the embedded sources are moderately extended and dense enough to be detected in CS, while gas disks around the T Tauri are not detected because the radius of such gas disks may be smaller than 70 (50 K/Tex) AU. These results imply that the total amount of matter within the NMA beam size must increase when the central objects evolve into T Tauri stars from embedded sources, suggesting that the compact and highly dense disks around T Tauri stars are formed by the dynamical mass accretion during the embedded protostar phase.

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