Dust Grain Orientation in the Interstellar Magnetic Field
نویسندگان
چکیده
منابع مشابه
Interstellar Dust and Magnetic Field at the Heliosphere
The very weak polarization of light from nearby stars reaches a maximum near the ecliptic plane in a position offset by λ ∼ 35 from the heliosphere nose direction. The position angle for the polarization in this ecliptic-plane peak is the same for near and distant stars, to within uncertainties, indicating the interstellar magnetic field direction is relatively constant over several hundred par...
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The orientation of the local interstellar magnetic field introduces asymmetries in the heliosphere that affect the location of heliospheric radio emissions and the streaming direction of ions from the termination shock of the solar wind. We combined observations of radio emissions and energetic particle streaming with extensive three-dimensional magnetohydrodynamic computer simulations of magne...
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Tiny interstellar dust grains causing the polarization of light from the nearest stars are deflected sideways in the outer heliosheath regions, along with the interstellar magnetic field. Observations of optical polarization of stars beyond the heliosphere nose, and at distances 5– 200 pc, suggest the direction of the upwind interstellar magnetic field is relatively constant. The polarization v...
متن کاملInterstellar Dust at the Magnetic Wall of the Heliosphere
February 5, 2008 Two sets of data show that small interstellar grains captured in interstellar magnetic fields, → BIS, draped over the heliosphere appear to polarize the light of nearby stars. The polarizing grains couple to → BIS, while larger grains couple to the cloud velocity. The maximum polarization direction, Pmax, is offset in ecliptic longitude by ∆λ ∼ +35 from the upwind direction, an...
متن کاملInterstellar Dust at the Magnetic Wall of the Heliosphere . II
February 11, 2008 Two sets of data show that small interstellar grains captured in interstellar magnetic fields, → BIS, draped over the heliosphere appear to polarize the light of nearby stars. The polarizing grains couple to → BIS, while larger grains couple to the cloud velocity. The maximum polarization direction, Pmax, is offset in ecliptic longitude by ∆λ ∼ +35 from the upwind direction, a...
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ژورنال
عنوان ژورنال: Symposium - International Astronomical Union
سال: 1990
ISSN: 0074-1809
DOI: 10.1017/s0074180900190126