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P. Boumis C. Dickinson J. Meaburn C. D. Goudis P. E. Christopoulou J. A. López M. Bryce M. P. Redman 《Monthly notices of the Royal Astronomical Society》2001,320(1):61-65
A deep Hα image of interlocking filamentary arcs of nebulosity has been obtained with a wide-field (≈30° diameter) narrow-band filter camera combined with a charge-coupled device as a detector. The resultant mosaic of images, extending to a galactic latitude of −65°, has been corrected for field distortions and had galactic coordinates superimposed on it to permit accurate correlations with the most recent H i (21 cm), X-ray (0.75 keV) and FIR ( IRAS 100 μm) maps.
Furthermore, an upper limit of 0.13 arcsec yr−1 to the expansion proper motion of the primary 25° long nebulous arc has been obtained by comparing a recent Hα image obtained with the San Pedro Martir telescope of its filamentary edge with that on a Palomar Observatory Sky Survey E plate obtained in 1951.
It is concluded that these filamentary arcs are the superimposed images of separate shells (driven by supernova explosions and/or stellar winds) rather than the edges of a single 'superbubble' stretching from Barnard's Arc (and the Orion Nebula) to these high galactic latitudes. The proper motion measurement argues against the primary Hα-emitting arc being associated with the giant radio loop (Loop 2) except in extraordinary circumstances. 相似文献
Furthermore, an upper limit of 0.13 arcsec yr
It is concluded that these filamentary arcs are the superimposed images of separate shells (driven by supernova explosions and/or stellar winds) rather than the edges of a single 'superbubble' stretching from Barnard's Arc (and the Orion Nebula) to these high galactic latitudes. The proper motion measurement argues against the primary Hα-emitting arc being associated with the giant radio loop (Loop 2) except in extraordinary circumstances. 相似文献
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Spatially resolved, broad Hα line profiles from both the luminous blue variable star ε Carinae (ε Car) and the surrounding filamentary Car II ('Keyhole') nebula, where they have been scattered and reflected by dust, have been observed periodically from 1985 to 1997. The Hα line profiles from ε Car in this 12-yr period show some, albeit not dramatic, changes. The sharp and deep P Cygni-type absorption feature that was observed first in 1985 in the broad, scattered/reflected profiles from the surrounding Keyhole nebula is not present in any of the direct ε Car profiles. This distinctive feature is now shown to be spatially variable over the Keyhole nebula and most prominent along the direction of the axis of the bipolar Homunculus nebula at PA 132°. No evidence of any temporal variability of this sharp feature has been found in 12 yr of monitoring, even from the most well-defined scattering/reflecting cloud along PA 132°.
It is concluded that a 46°-wide cone of light from ε Car is relatively unobscured along the axis of the Homunculus nebula and that this must be the consequence of a dense torus close to the star. 相似文献
It is concluded that a 46°-wide cone of light from ε Car is relatively unobscured along the axis of the Homunculus nebula and that this must be the consequence of a dense torus close to the star. 相似文献
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P. Boumis J. Meaburn M. Lloyd S. Akras 《Monthly notices of the Royal Astronomical Society》2009,396(2):1186-1188
A deep wide-field image in the light of the Hα and [N ii ] 6548 & 6584 Å emission lines, of the planetary nebula HFG1 which surrounds the pre-cataclysmic binary system V664 Cas, has revealed a tail of emission at least 20 arcmin long, at a position angle of 316°. Evidence is presented which suggests that this is an ≈105 yr old trail of shocked material, left behind V664 Cas as it ejects matter whilst ploughing through its local interstellar media at anywhere between 29 and 59 km s−1 depending on its distance from the Sun. 相似文献
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