122:
352:
Heitsch, Fabian; Zweibel, Ellen G.; Mac Low, Mordecai-Mark; Li, Pakshing; Norman, Michael L. (10 November 2001). "Magnetic Field
Diagnostics Based on Far-Infrared Polarimetry: Tests Using Numerical Simulations".
241:
195:
168:
145:
433:
Ostriker, Eve C.; Stone, James M.; Gammie, Charles F. (10 January 2001). "Density, Velocity, and
Magnetic Field Structure in Turbulent Molecular Cloud Models".
215:
60:
68:
513:
390:
Padoan, Paolo; Goodman, Alyssa; Draine, B. T.; Juvela, Mika; Nordlund, Ake; Rognvaldsson, Ornolfur Einar (October 2001).
30:
is a method that is used to calculate the mean strength of the interstellar magnetic field that is projected on the
35:
472:"SCUBA Polarization Measurements of the Magnetic Field Strengths in the L183, L1544, and L43 Prestellar Cores"
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Crutcher, Richard M.; Nutter, D. J.; Ward-Thompson, D.; Kirk, J. M. (January 2004).
39:
259:
Davis, Leverett (1 March 1951). "The
Strength of Interstellar Magnetic Fields".
272:
34:. The method was described by Leverett Davis Jr in 1951 and independently by
447:
408:
367:
392:"Theoretical Models of Polarized Dust Emission from Protostellar Cores"
117:{\displaystyle B=Q{\sqrt {4\pi \rho }}{\frac {\delta v}{\delta \phi }}}
488:
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456:
418:
391:
376:
337:
320:
304:
287:
243:. The method is also employed for prestellar molecular clouds.
286:
Davis, Leverett Jr.; Greenstein, Jesse L. (September 1951).
217:
is an order unity factor, which is typically taken it to be
288:"The Polarization of Starlight by Aligned Dust Grains"
42:
in 1953. According to this method, the magnetic field
223:
203:
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153:
133:
71:
48:
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54:
197:is the dispersion of polarization angles and
8:
319:Chandrasekhar, S.; Fermi, E. (July 1953).
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7:
62:in the plane of the sky is given by
14:
321:"Magnetic Fields in Spiral Arms"
28:Davis–Chandrasekhar–Fermi method
1:
236:{\displaystyle Q\approx 0.5}
190:{\displaystyle \delta \phi }
530:
36:Subrahmanyan Chandrasekhar
20:Chandrasekhar–Fermi method
476:The Astrophysical Journal
435:The Astrophysical Journal
396:The Astrophysical Journal
355:The Astrophysical Journal
325:The Astrophysical Journal
292:The Astrophysical Journal
273:10.1103/PhysRev.81.890.2
163:{\displaystyle \delta v}
514:Equations of astronomy
237:
211:
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118:
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170:is the line-of-sight
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147:is the mass density,
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140:{\displaystyle \rho }
119:
57:
16:Astrophysics equation
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69:
46:
172:velocity dispersion
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137:
114:
52:
210:{\displaystyle Q}
112:
92:
55:{\displaystyle B}
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448:astro-ph/0008454
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409:astro-ph/0104231
402:(2): 1005–1018.
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368:astro-ph/0103286
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32:plane of the sky
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469:
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441:(2): 980–1005.
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261:Physical Review
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12:
11:
5:
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489:10.1086/379705
482:(1): 279–285.
462:
457:10.1086/318290
425:
419:10.1086/322504
382:
377:10.1086/323489
361:(2): 800–814.
344:
338:10.1086/145731
311:
305:10.1086/145464
278:
267:(5): 890–891.
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509:Astrophysics
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40:Enrico Fermi
27:
23:
19:
18:
503:Categories
247:References
228:≈
185:ϕ
182:δ
155:δ
135:ρ
109:ϕ
106:δ
98:δ
90:ρ
87:π
24:CF method
331:: 113.
298:: 206.
127:where
443:arXiv
404:arXiv
363:arXiv
174:and
38:and
484:doi
480:600
453:doi
439:546
414:doi
400:559
373:doi
359:561
333:doi
329:118
300:doi
296:114
269:doi
231:0.5
26:or
22:or
505::
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365::
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335::
308:.
302::
275:.
271::
225:Q
205:Q
158:v
101:v
84:4
79:Q
76:=
73:B
50:B
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