TY - GEN
T1 - Expected observations of star formation process
T2 - Conference on Labyrinth of Star Formation dedicated to Prof. Anthony Whitworth, 2012
AU - Tomisaka, Kohji
AU - Kataoka, Akimasa
AU - Machida, Masahiro N.
AU - Tomida, Kengo
AU - Saigo, Kazuya
N1 - Funding Information:
This research was funded by the National Natural Science Foundation of China (Grant No. 51674004) and Education Department of Anhui Province of China (Grant Nos. KJ2016A104 and KJ2017A805).
Publisher Copyright:
© Springer International Publishing Switzerland 2014.
PY - 2014
Y1 - 2014
N2 - We performed MHD simulations of the contraction of rotating, magnetized molecular cloud cores. In the molecular cores, B-field and angular momentum (J) vector are not always aligned. When a first hydrostatic core forms, axisymmetric structure appears and average B and J are parallel in small scale. However, in large scale, the configuration is far from this. This means that contraction process is imprinted on the snapshot. We calculated two mock observations of MHD simulations (1) the polarization of dust thermal emission to reveal the magnetic evolution and (2) the line emissions from interstellar molecules to reveal the evolution of density and velocity. Comparing the mock observations with true ones, we can answer several questions: in which case the hourglass-shaped and S-shaped magnetic fields are seen; how the distribution of polarized intensity is understood; how the first hydrostatic core should be observationally identified.
AB - We performed MHD simulations of the contraction of rotating, magnetized molecular cloud cores. In the molecular cores, B-field and angular momentum (J) vector are not always aligned. When a first hydrostatic core forms, axisymmetric structure appears and average B and J are parallel in small scale. However, in large scale, the configuration is far from this. This means that contraction process is imprinted on the snapshot. We calculated two mock observations of MHD simulations (1) the polarization of dust thermal emission to reveal the magnetic evolution and (2) the line emissions from interstellar molecules to reveal the evolution of density and velocity. Comparing the mock observations with true ones, we can answer several questions: in which case the hourglass-shaped and S-shaped magnetic fields are seen; how the distribution of polarized intensity is understood; how the first hydrostatic core should be observationally identified.
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U2 - 10.1007/978-3-319-03041-8_24
DO - 10.1007/978-3-319-03041-8_24
M3 - Conference contribution
AN - SCOPUS:84959531559
SN - 9783319030401
T3 - Astrophysics and Space Science Proceedings
SP - 133
EP - 137
BT - The Labyrinth of Star Formation - Conference Dedicated to Prof. Anthony Whitworth
A2 - Goodwin, Simon
A2 - Stamatellos, Dimitris
A2 - Ward-Thompson, Derek
PB - Kluwer Academic Publishers
Y2 - 1 June 2012
ER -