Neutral hydrogen in the direction of the Vela supernova remnant
We have carried out a study of the distribution and kinematics of the neutral hydrogen in the direction of the Vela supernova remnant (SNR). A field of 6°.8 × 5°.4 centered at l = 264°.1, b = -1°.6 was surveyed using the Parkes 64 m radio telescope (half-power beamwidth 14′.7 at 21 cm). Nearly 2300...
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1998
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| Acceso en línea: | https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046256_v116_n2_p813_Dubner http://hdl.handle.net/20.500.12110/paper_00046256_v116_n2_p813_Dubner |
| Aporte de: |
| Sumario: | We have carried out a study of the distribution and kinematics of the neutral hydrogen in the direction of the Vela supernova remnant (SNR). A field of 6°.8 × 5°.4 centered at l = 264°.1, b = -1°.6 was surveyed using the Parkes 64 m radio telescope (half-power beamwidth 14′.7 at 21 cm). Nearly 2300 H I profiles were obtained with a grid spacing of 7′.5. The presence of a thin, almost circular H I shell, centered at v = 1.6 ± 0.8 km s-1, is revealed. This shell delineates the outer border of the X-ray emission as shown in the ROSAT observations of Aschenbach, Egger, & Trümper and wraps around the receding part of the remnant. In addition, two higher velocity features possibly associated with Vela are observed at about -30 and 30 km s-1. These features are interpreted as gas accelerated by the expansion of the supernova shock. The low systemic velocity observed suggests a distance shorter than 500 pc for the Vela SNR. The H I shell is ∼7° in diameter and expands at v ∼ 30 km s-1. By assuming a distance of 350 pc, we calculate for this shell a linear radius of 22 pc, a swept-up mass of ∼ 1200-2300 M⊙, and an atomic preshock density of ∼ 1-2 cm-3. The kinetic energy transferred by the supernova shock into the interstellar medium is ∼(1-2) × 1049 ergs, while the initial energy of the explosion is estimated to be ∼ (1-2.5) × 1051 ergs. We present the distribution of the column density of the neutral material absorbing the X-radiation, an essential parameter in the analysis of X-ray data. A comparison between the H I and Hα emission suggests that the H I shell contains embedded dust that might be responsible for increased optical absorption in this region. On the other hand, the brightest arc-shaped optical filaments associated with the western side of Vela show good correspondence with the H I features. From a comparison between the H I and Molonglo Observatory Synthesis Telescope 843 MHz radio continuum emission, we find that the outermost arched radio filaments correlate well with the main ridge of the H I shell. No strong inhomogeneities were found in the ambient H I medium in the direction of Vela X (the central nebula, powered by the pulsar PSR B0833-45). |
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