Titlebook: Interstellar Magnetic Fields; Observation and Theo Rainer Beck,Roland Gr?ve Conference proceedings 1987 Springer-Verlag Berlin Heidelberg 1

Harding

書目名稱Interstellar Magnetic Fields影響因子(影響力)




書目名稱Interstellar Magnetic Fields影響因子(影響力)學(xué)科排名




書目名稱Interstellar Magnetic Fields網(wǎng)絡(luò)公開度




書目名稱Interstellar Magnetic Fields網(wǎng)絡(luò)公開度學(xué)科排名




書目名稱Interstellar Magnetic Fields被引頻次




書目名稱Interstellar Magnetic Fields被引頻次學(xué)科排名




書目名稱Interstellar Magnetic Fields年度引用




書目名稱Interstellar Magnetic Fields年度引用學(xué)科排名




書目名稱Interstellar Magnetic Fields讀者反饋




書目名稱Interstellar Magnetic Fields讀者反饋學(xué)科排名

突襲

不透明性

The Magnetic Field in IC 342he line of sight [1]. This allows a detailed study of the magnetic field in the spiral arms of IC 342 even with the medium resolution achievable with the 100-m radio telescope at centimetre wavelengths. The largescale structure of the magnetic field in IC 342 was earlier suggested to be ring-like [2] similar to M31.

敵手

RAGE

Semblance

High Resolution Observations of Linearly Polarized Emissions of IC 342rt two long ridges of polarized intensity are prominent. The outer one can be traced along about 20 kpc. Both ridges coincide with two optical spiral arms and two HI spiral arms[2]. The region of maximal polarized intensity is near the bifurcation of the optical and HI spiral arms.

原來

expansive

Mere僅僅

Nonthermal Radio Emission from Dwarf Galaxies: Do They Host Large-Scale Magnetic Fields?ary over a wide range, from a few percent up to almost unity. And, most characteristically, their star formation rates cannot have been constant over the past ～ 10. yr: many of them must have been subject to bursts of star formation.

冥界三河