scholarly journals Magnetic field spectrum at cosmological recombination revisited

2015 ◽  
Vol 91 (12) ◽  
Author(s):  
Shohei Saga ◽  
Kiyotomo Ichiki ◽  
Keitaro Takahashi ◽  
Naoshi Sugiyama
1976 ◽  
Vol 32 ◽  
pp. 233-254
Author(s):  
H. M. Maitzen

Ap stars are peculiar in many aspects. During this century astronomers have been trying to collect data about these and have found a confusing variety of peculiar behaviour even from star to star that Struve stated in 1942 that at least we know that these phenomena are not supernatural. A real push to start deeper theoretical work on Ap stars was given by an additional observational evidence, namely the discovery of magnetic fields on these stars by Babcock (1947). This originated the concept that magnetic fields are the cause for spectroscopic and photometric peculiarities. Great leaps for the astronomical mankind were the Oblique Rotator model by Stibbs (1950) and Deutsch (1954), which by the way provided mathematical tools for the later handling pulsar geometries, anti the discovery of phase coincidence of the extrema of magnetic field, spectrum and photometric variations (e.g. Jarzebowski, 1960).


2001 ◽  
Vol 8 (12) ◽  
pp. 5165-5170 ◽  
Author(s):  
J. N. Talmadge ◽  
V. Sakaguchi ◽  
F. S. B. Anderson ◽  
D. T. Anderson ◽  
A. F. Almagri

1964 ◽  
Vol 35 (10) ◽  
pp. 1307-1310 ◽  
Author(s):  
L. J. Greenstein ◽  
T. R. Shaifer ◽  
M. Epstein

1967 ◽  
Vol 31 ◽  
pp. 381-383
Author(s):  
J. M. Greenberg

Van de Hulst (Paper 64, Table 1) has marked optical polarization as a questionable or marginal source of information concerning magnetic field strengths. Rather than arguing about this–I should rate this method asq+-, or quarrelling about the term ‘model-sensitive results’, I wish to stress the historical point that as recently as two years ago there were still some who questioned that optical polarization was definitely due to magnetically-oriented interstellar particles.


1967 ◽  
Vol 31 ◽  
pp. 375-380
Author(s):  
H. C. van de Hulst

Various methods of observing the galactic magnetic field are reviewed, and their results summarized. There is fair agreement about the direction of the magnetic field in the solar neighbourhood:l= 50° to 80°; the strength of the field in the disk is of the order of 10-5gauss.


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