Star Forming Dense Cloud Cores in the TeV -ray SNR RX J1713.7-3946

2010 ◽  
Author(s):  
Sano Hidetoshi
Keyword(s):  
Star Forming ◽  
Dense Cloud ◽  
Cloud Cores

scholarly journals STAR-FORMING DENSE CLOUD CORES IN THE TeV GAMMA-RAY SNR RX J1713.7–3946

2010 ◽  
Vol 724 (1) ◽  
pp. 59-68 ◽  
Author(s):  
H. Sano ◽  
J. Sato ◽  
H. Horachi ◽  
N. Moribe ◽  
H. Yamamoto ◽  
...  
Keyword(s):  
Gamma Ray ◽  
Star Forming ◽  
Dense Cloud ◽  
Cloud Cores

C18O Observations of the Dense Cloud Cores and Star Formation in Ophiuchus

2000 ◽  
Vol 528 (2) ◽  
pp. 817-840 ◽  
Author(s):  
Kengo Tachihara ◽  
Akira Mizuno ◽  
Yasuo Fukui
Keyword(s):  
Star Formation ◽  
Dense Cloud ◽  
Cloud Cores

scholarly journals Multiplicity Among the Young Stars

1992 ◽  
Vol 135 ◽  
pp. 41-49
Author(s):  
M. Simon
Keyword(s):  
Angular Momentum ◽  
Molecular Cloud ◽  
Young Stars ◽  
Circumstellar Disk ◽  
Multiple Systems ◽  
Star Forming ◽  
Lunar Occultation ◽  
Angular Momenta ◽  
Cloud Cores ◽  
Active Disks

AbstractOur survey for companions of the young stars now includes 45 systems in the Taurus star-forming region (SFR) and 21 in the Ophiuchus SFR. It is carried out by lunar occultation and imaging in the IR and can identify binaries in the separation range 0″.005 to 10″ in systems brighter than K=10 mag. The observed multiplicity in Taurus is ~1.6 stars/system which is comparable to that of the nearby solarlike stars but corrections for incompleteness increase the multiplicity to at least 1.8.Inner active disks are equally represented among the single and multiple systems. The multiple systems have less massive outer disks than the single systems, but there are significant exceptions. The binary UZ Tau W contains a circumstellar disk or disks of mass ~0.024 M⊙ and size ~13 AU. The quadruple GG Tau system has a remarkably extensive circumbinary disk of mass ~ 0.07M⊙. These mass estimates are comparable to the minimum values required for the proto-planetary disk of the Solar System.The specific angular momenta of the most widely spaced binaries in our sample adjoin the lowest values that can be measured for molecular cloud cores. The actual distributions probably overlap which suggests that the origin of the angular momentum of binaries is in their molecular cloud birthplaces.

scholarly journals A (Sub)Millimeter survey of massive star-forming regions identified by the ISOPHOT Serendipity Survey (ISOSS)

2006 ◽  
Vol 2 (S237) ◽  
pp. 424-424
Author(s):  
Martin Hennemann ◽  
Stephan M. Birkmann ◽  
Oliver Krause ◽  
Dietrich Lemke
Keyword(s):  
Molecular Cloud ◽  
Massive Star ◽  
Infrared Emission ◽  
Evolutionary Stage ◽  
Star Forming ◽  
Star Forming Regions ◽  
Low Mass ◽  
Low Levels ◽  
Cloud Cores ◽  
Mass Case

AbstractA sample of potential massive starforming regions identified at 170 m by ISO was observed in the submillimeter and millimeter regime. These observations allow us to infer physical properties of the molecular cloud cores. Two sources are presented in detail: ISOSS J23053+5953 and J183640221 show viable candidates for massive protocluster cores. Our analysis shows very low temperatures and low levels of turbulence of the major mass fraction in the molecular cloud cores besides active star formation at an early evolutionary stage. These conditions seem similar to the low mass case and may precede phases of luminous infrared emission observed towards young massive protostars.

scholarly journals THE DEUTERIUM FRACTIONATION TIMESCALE IN DENSE CLOUD CORES: A PARAMETER SPACE EXPLORATION

2015 ◽  
Vol 804 (2) ◽  
pp. 98 ◽  
Author(s):  
Shuo Kong ◽  
Paola Caselli ◽  
Jonathan C. Tan ◽  
Valentine Wakelam ◽  
Olli Sipilä
Keyword(s):  
Parameter Space ◽  
Space Exploration ◽  
Dense Cloud ◽  
Cloud Cores

scholarly journals Dense cloud cores revealed by CO in the low metallicity dwarf galaxy WLM

Nature ◽  
2015 ◽  
Vol 525 (7568) ◽  
pp. 218-221 ◽  
Author(s):  
Monica Rubio ◽  
Bruce G. Elmegreen ◽  
Deidre A. Hunter ◽  
Elias Brinks ◽  
Juan R. Cortés ◽  
...  
Keyword(s):  
Dwarf Galaxy ◽  
Dense Cloud ◽  
Low Metallicity ◽  
Cloud Cores

A C18O Survey of Dense Cloud Cores in Taurus: Star Formation

1998 ◽  
Vol 502 (1) ◽  
pp. 296-314 ◽  
Author(s):  
Toshikazu Onishi ◽  
Akira Mizuno ◽  
Akiko Kawamura ◽  
Hideo Ogawa ◽  
Yasuo Fukui
Keyword(s):  
Star Formation ◽  
Dense Cloud ◽  
Cloud Cores

scholarly journals Investigating the complex velocity structures within dense molecular cloud cores with GBT-Argus

2019 ◽  
Vol 490 (1) ◽  
pp. 527-539 ◽  
Author(s):  
Che-Yu Chen ◽  
Shaye Storm ◽  
Zhi-Yun Li ◽  
Lee G Mundy ◽  
David Frayer ◽  
...  
Keyword(s):  
Angular Momentum ◽  
Large Scale ◽  
High Spectral Resolution ◽  
Star Forming ◽  
Velocity Gradients ◽  
Dense Molecular Cloud ◽  
First Results ◽  
Scale Turbulence ◽  
Cloud Cores ◽  
Flow Compression

ABSTRACT We present the first results of high-spectral resolution (0.023 km s−1) N2H+ observations of dense gas dynamics at core scales (∼0.01 pc) using the recently commissioned Argus instrument on the Green Bank Telescope (GBT). While the fitted linear velocity gradients across the cores measured in our targets nicely agree with the well-known power-law correlation between the specific angular momentum and core size, it is unclear if the observed gradients represent core-scale rotation. In addition, our Argus data reveal detailed and intriguing gas structures in position–velocity (PV) space for all five targets studied in this project, which could suggest that the velocity gradients previously observed in many dense cores actually originate from large-scale turbulence or convergent flow compression instead of rigid-body rotation. We also note that there are targets in this study with their star-forming discs nearly perpendicular to the local velocity gradients, which, assuming the velocity gradient represents the direction of rotation, is opposite to what is described by the classical theory of star formation. This provides important insight on the transport of angular momentum within star-forming cores, which is a critical topic on studying protostellar disc formation.

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