On the Presence of Polarization in the Continuous Radiation of Stars. II.

Hiltner, W. A.

doi:10.1086/145151

Cited by 159 publications

(75 citation statements)

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“…The first evidence for a Galactic magnetic field was found more than 50 years ago from the observation of linear polarization of starlight [12]. Meanwhile, quite detailed information about the GMF has been extracted mainly from Faraday rotation measurements of extragalactic sources or Galactic pulsars [13].…”

Section: Galactic Magnetic Field Modelsmentioning

confidence: 99%

The Galactic magnetic field as spectrograph for ultra-high energy cosmic rays

Kachelrieß

Serpico

Teshima

2007

Astroparticle Physics

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Section: Galactic Magnetic Field Modelsmentioning

confidence: 99%

The Galactic magnetic field as spectrograph for ultra-high energy cosmic rays

Kachelrieß

Serpico

Teshima

2007

Astroparticle Physics

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“…The first evidence for the existence of a Galactic magnetic field was derived from the observation of linear polarization of starlight by Hiltner (1949). Many new measurements have been done since using of Zeeman spectral-line splitting (gaseous clouds, central region of the Galaxy), optical polarization data (large-scale structures of the magnetic field in the local spiral arm) and the Faraday rotation measurements in the radio continuum emission of pulsars and of the extragalactic sources.…”

Section: Galactic Magnetic Field 21 Experimental Evidencementioning

confidence: 99%

The Galactic magnetic field and propagation of ultra-high energy cosmic rays

Prouza

Šmída

2003

A&A

108

139

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Abstract. The puzzle of ultra-high energy cosmic rays (UHECRs) still remains unresolved. With the progress in the preparation of the next generation of experiments (AUGER, EUSO, OWL), the importance of directional analysis of existing and future events is increasing. The Galactic Magnetic Field (GMF) plays the key role in source identification even in this energy range. We first analyze the current status of our experimental and theoretical knowledge about the GMF and introduce a complex up-to-date model of GMF. Then we present two examples of simple applications of the influence of the GMF on UHECR propagation. Both examples are based on the Lorentz equation solution. The first one is a basic directional analysis of the incident directions of UHECRs and the second one is a simulation of a change of chemical composition of CRs in the energy range 10 13 ÷ 10 19 eV. The results of these simple analyses are surprisingly rich -e.g. the rates of particle escape from the Galaxy or the amplifications of particle flux in specific directions.

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“…As discovered by Hiltner (1949), the interaction of light of distant stars with the interstellar medium (ISM) leads to a significant linear polarization. Because this additional "polarizer" (polarization degree P l,ISM , orientation angle γ ISM ) influences the observed light of both binary components, the observed position angle difference ∆γ may be reduced.…”

Section: Influence Of the Interstellar Polarizationmentioning

confidence: 99%

Pre-Main Sequence Binaries with Aligned Disks?

Wolf

Stecklum

Henning³

2001

Symp. - Int. Astron. Union

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Abstract. We present the results of a study performed with the goal to investigate whether low-mass pre-main sequence binary stars are formed by multiple fragmentation or via stellar capture. If binaries form preferentially by fragmentation, we expect their disks to be co-planar. On the other hand, the capture scenario will lead to a random distribution of disk orientations. We performed near-infrared polarization measurements of 49 young close binary stars in the K band with SOFI at the NTT. The near-infrared excess radiation of the targets mostly point to the presence of disks. For a major fraction of the sample, evidence for disks is also obvious from other features (outflows, jets, Herbig-Haro objects). We derived the disk orientation from the orientation of the polarization vector of both components of each binary. This statistical study allows to test which hypothesis (co-planarity, random orientation) is consistent with the observed distribution of polarimetric position angles. We find evidence that the disks are preferentially aligned.

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On the Presence of Polarization in the Continuous Radiation of Stars. II.

Cited by 159 publications

References 0 publications

The Galactic magnetic field as spectrograph for ultra-high energy cosmic rays

The Galactic magnetic field as spectrograph for ultra-high energy cosmic rays

The Galactic magnetic field and propagation of ultra-high energy cosmic rays

Pre-Main Sequence Binaries with Aligned Disks?

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