scholarly journals The influence of the magnetic field orientation on the angular momentum loss in the pre-main sequence phase: The case of very slowly rotating magnetic Ap stars

2002 ◽  
Vol 384 (2) ◽  
pp. 554-561 ◽  
Author(s):  
K. Stępień ◽  
J. D. Landstreet
Keyword(s):  
Magnetic Field ◽  
Angular Momentum ◽  
Main Sequence ◽  
Field Orientation ◽  
Magnetic Field Orientation ◽  
Momentum Loss ◽  
Angular Momentum Loss ◽  
Ap Stars ◽  
The Magnetic Field

scholarly journals Loss of magnetic flux and angular momentum from molecular clouds

1991 ◽  
Vol 147 ◽  
pp. 67-74
Author(s):  
Takenori Nakano
Keyword(s):  
Magnetic Field ◽  
Angular Momentum ◽  
Magnetic Flux ◽  
Molecular Clouds ◽  
Loss Rate ◽  
Momentum Loss ◽  
Angular Momentum Loss ◽  
The Magnetic Field ◽  
Flux Loss

The magnetic field and the angular momentum are major obstacles against cloud contraction. I will review recent results on magnetic flux loss rate and angular momentum loss rate and will investigate a gross feature of cloud contraction.

scholarly journals Loss of magnetic flux and angular momentum from molecular clouds

1991 ◽  
Vol 147 ◽  
pp. 67-74
Author(s):  
Takenori Nakano
Keyword(s):  
Magnetic Field ◽  
Angular Momentum ◽  
Magnetic Flux ◽  
Molecular Clouds ◽  
Loss Rate ◽  
Momentum Loss ◽  
Angular Momentum Loss ◽  
The Magnetic Field ◽  
Flux Loss

The magnetic field and the angular momentum are major obstacles against cloud contraction. I will review recent results on magnetic flux loss rate and angular momentum loss rate and will investigate a gross feature of cloud contraction.

scholarly journals An observational correlation between magnetic field, angular momentum and fragmentation in the envelopes of Class 0 protostars?

2020 ◽  
Vol 644 ◽  
pp. A47
Author(s):  
Maud Galametz ◽  
Anaëlle Maury ◽  
Josep M. Girart ◽  
Ramprasad Rao ◽  
Qizhou Zhang ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Angular Momentum ◽  
Large Scale ◽  
Magnetic Energy ◽  
Line Emission ◽  
Strong Relationship ◽  
Field Orientation ◽  
Multiple Systems ◽  
Magnetic Field Orientation ◽  
The Magnetic Field

Aims. The main goal of the following analysis is to assess the potential role of magnetic fields in regulating the envelope rotation, the formation of disks and the fragmentation of Class 0 protostars in multiple systems. Methods. We use the Submillimeter Array to carry out observations of the dust polarized emission at 0.87 mm, in the envelopes of a large sample of 20 Class 0 protostars. We estimate the mean magnetic field orientation over the central 1000 au envelope scales to characterize the orientation of the main component of the organized magnetic field at the envelope scales in these embedded protostars. This direction is compared to that of the protostellar outflow in order to study the relation between their misalignment and the kinematics of the circumstellar gas. The latter is traced via velocity gradient observed in the molecular line emission (mainly N2H+) of the gas at intermediate envelope scales. Results. We discover a strong relationship between the misalignment of the magnetic field orientation with the outflow and the amount of angular momentum observed at similar scales in the protostellar envelope, revealing a potential link between the kinetic and the magnetic energy at envelope scales. The relation could be driven by favored B-misalignments in more dynamical envelopes or a dependence of the envelope dynamics with the large-scale B initial configuration. Comparing the trend with the presence of fragmentation, we observe that single sources are mostly associated with conditions of low angular momentum in the inner envelope and good alignment of the magnetic field with protostellar outflows, at intermediate scales. Our results suggest that the properties of the magnetic field in protostellar envelopes bear a tight relationship with the rotating-infalling gas directly involved in the star and disk formation: we find that it may not only influence the fragmentation of protostellar cores into multiple stellar systems, but also set the conditions establishing the pristine properties of planet-forming disks.

On the absence of plasma wave emissions and the magnetic field orientation in the distant magnetosheath

1994 ◽  
Vol 21 (24) ◽  
pp. 2761-2764 ◽  
Author(s):  
F. V. Coroniti ◽  
E. W. Greenstadt ◽  
S. L. Moses ◽  
B. T. Tsurutani ◽  
E. J. Smith
Keyword(s):  
Magnetic Field ◽  
Plasma Wave ◽  
Field Orientation ◽  
Magnetic Field Orientation ◽  
The Magnetic Field

scholarly journals The Magnetic Field of the Crab as Revealed by New, High Resolution, Multi-Band Radio Images

1990 ◽  
Vol 140 ◽  
pp. 79-80
Author(s):  
M. F. Bietenholz ◽  
P. P. Kronberg
Keyword(s):  
Magnetic Field ◽  
High Resolution ◽  
Crab Nebula ◽  
Radio Observations ◽  
Field Orientation ◽  
Magnetic Field Orientation ◽  
The Crab Nebula ◽  
The Magnetic Field ◽  
Made In ◽  
Multi Band

We present and describe recent radio observations of the Crab Nebula, which allow us to determine the magnetic field orientation and depolarization at unprecedented resolution. The observations were made in 1987-1988 using all four configurations of the VLA, at 1410,1515,4625, and 4885 MHz. The resulting maps were all convolved with a clean beam of 1.8″ × 2.0″, elongated in P.A. 80°, and the residuals added back in.

scholarly journals Hollow Cylindrical Lobes with a Helical Velocity Field of the L1551 Bipolar Flow

1987 ◽  
Vol 115 ◽  
pp. 287-300
Author(s):  
Yutaka Uchida ◽  
Norio Kaifu ◽  
Kazunari Shibata ◽  
Saeko S. Hayashi ◽  
Tetsuo Hasegawa
Keyword(s):  
Magnetic Field ◽  
Angular Momentum ◽  
Star Formation ◽  
Velocity Field ◽  
Formation Process ◽  
High Spatial Resolution ◽  
Cylindrical Structure ◽  
Angular Momentum Loss ◽  
Show Evidence ◽  
The Magnetic Field

Observations of the structure and the velocity field in the L1551 bipolar flow were made with the 45m telescope at Nobeyama in the 115GHz 12CO J = 1 – 0 line with high spatial resolution. It was found that the bipolar flow lobes have a clear hollow cylindrical structure and show evidence of a helical velocity field. They appear to rotate in the same direction as the CS disk found by Kaifu et al. (1984). The velocity of the flow in the bipolar directions increases with distance up to ∼ 3′ from the central object, IRS 5. These characteristics coincide with those predicted by the magnetodynamic theory proposed by Uchida and Shibata and indicate the essential importance of the magnetic field in producing such flows and also in the star-formation process itself through the enhancement of angular-momentum loss.

Effect of Processing Variables on The Magnetic Field Orientation of Liquid Crystalline Thermosets

1999 ◽  
Vol 559 ◽  
Author(s):  
Derek M. Lincoln ◽  
Elliot P. Douglas
Keyword(s):  
Magnetic Field ◽  
Liquid Crystalline ◽  
Fractional Factorial Design ◽  
Fractional Factorial ◽  
Field Orientation ◽  
Magnetic Field Orientation ◽  
Liquid Crystalline Epoxy ◽  
Processing Variables ◽  
Degree Of Orientation ◽  
The Magnetic Field

ABSTRACTWe have investigated the effect of various processing variables on the magnetic field orientation of a liquid crystalline epoxy. By using a modified fractional factorial design, we created an empirical model which can be used to predict the degree of orientation as a function of these variables. The model predicts the correct qualitative trends, namely that orientation increases with increasing magnetic field strength, increases with increasing time in the field, and decreases with increasing B-staging. The model also reveals some surprising effects of B-staging on the degree of orientation.

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