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Lu, F. J.; Aschenbach, B.; Song, Liming; Durouchoux, Ph.

doi:10.1023/a:1011670607532

Cited by 21 publications

(50 citation statements)

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“…While soft X-rays from this region are detected, they are primarily thermal in nature, and represent emission from the hot plasma that Ðlls the entire remnant Lu & Aschenbach 2000). Even the bright radio Ðlament detected by Bietenholz, Frail, & Hankins (1991) shows no corresponding enhancement in our X-ray image, although more constraining limits will be derivable from ACIS observations.…”

Section: An Image Of the Vela Pulsarmentioning

confidence: 69%

Vela Pulsar and Its Synchrotron Nebula

Helfand

Gotthelf

Halpern

2001

ApJ

283

305

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We present high-resolution Chandra X-ray observations of PSR B0833[45, the 89 ms pulsar associated with the Vela supernova remnant. We have acquired two observations separated by 1 month to search for changes in the pulsar and its environment following an extreme glitch in its rotation frequency. We Ðnd a well-resolved nebula with a toroidal morphology remarkably similar to that observed in the Crab Nebula, along with an axial Crab-like jet. Between the two observations, taken D3 ] 105 s and D3 ] 106 s after the glitch, the Ñux from the pulsar is found to be steady to within 0.75% ; the 3 p limit on the fractional increase in the pulsarÏs X-ray Ñux is of the inferred glitch energy. We use [10~5 this limit to constrain parameters of glitch models and neutron star structure. We do Ðnd a signiÐcant increase in the Ñux of the nebulaÏs outer arc ; if associated with the glitch, the inferred propagation velocity is similar to that seen in the brightening of the Crab Nebula wisps. We propose an explana-Z0.7c, tion for the X-ray structure of the Vela synchrotron nebula based on a model originally developed for the Crab Nebula. In this model, the bright X-ray arcs are the shocked termination of a relativistic equatorial pulsar wind that is contained within the surrounding kidney-bean shaped synchrotron nebula comprising the postshock, but still relativistic, Ñow. In a departure from the Crab model, the magnetization parameter p of the Vela pulsar wind is allowed to be of order unity ; this is consistent with the simplest MHD transport of magnetic Ðeld from the pulsar to the nebula, where B ¹ 4 ] 10~4 G. The inclination angle of the axis of the equatorial torus with respect to the line of sight is identical to that of the rotation axis of the pulsar as previously measured from the polarization of the radio pulse. The projection of the rotation axis on the sky may also be close to the direction of proper motion of the pulsar if previous radio measurements were confused by orthogonal-mode polarized components. We review e †ects that may enhance the probability of alignment between the spin axis and space velocity of a pulsar, and speculate that short-period, slowly moving pulsars are just the ones best-suited to producing synchrotron nebulae with such aligned structures. Previous interpretations of the compact Vela nebula as a bow-shock in a very weakly magnetized wind su †ered from data of inadequate spatial resolution and less plausible physical assumptions.

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Section: An Image Of the Vela Pulsarmentioning

confidence: 69%

Vela Pulsar and Its Synchrotron Nebula

Helfand

Gotthelf

Halpern

2001

ApJ

283

305

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“…1). The boundary between the bright and the dim part of shell is quite sharp (Lu & Aschenbach 2000). The change in the properties of the shell at different sides indicates that the characteristics of the ISM in the NE part differ from those in the SW part.…”

Section: Vela Snr Properties and Peculiarities Ne-sw Asymmetrymentioning

confidence: 93%

“…Apart from the difference of the radii, the spatially-resolved spectroscopic analysis by Lu & Aschenbach (2000) shows that the SW part of the shell appears to be hotter than the NE one. The shell is bright only on the NE side, while the SW side appears to be dim and is apparently more extended (see Fig.…”

Section: Vela Snr Properties and Peculiarities Ne-sw Asymmetrymentioning

confidence: 97%

“…The sharpness of the boundary shows that the change in the ISM properties is abrupt rather than gradual. Lu & Aschenbach (2000) estimate the contrast change of the two faint regions, each 1.5 • × 1.5 • , in the NE and SW parts, to be a factor of 11 in brightness and ∼6 in emission measure. Assuming the same estimate for the emission measure contrast change for the entire NE and SW parts of the SNR and taking into account the difference of the radii of the two parts of the SNR, one can find that the luminosity of the NE part L x,NE is a factor of ∼3.7 higher than the luminosity L x,SW of the SW part.…”

Section: Vela Snr Properties and Peculiarities Ne-sw Asymmetrymentioning

confidence: 99%

“…The most commonly cited estimate is t SNR = t pulsar 1.14 × 10 4 yr, where t pulsar is the age of the Vela pulsar (Reichley et al 1970). The total 0.1−2.4 keV X-ray luminosity from Vela SNR in erg/s is (Lu & Aschenbach 2000) L x, tot = 3.0 × 10 35 D vela 290 pc 2 erg/s.…”

Section: Vela Snr Properties and Peculiarities Ne-sw Asymmetrymentioning

confidence: 99%

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Modeling of the Vela complex including the Vela supernova remnant, the binary systemγ² Velorum, and the Gum nebula

Sushch

Hnatyk

Neronov

2010

A&A

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We study the geometry and dynamics of the Vela complex including the Vela supernova remnant (SNR), the binary system γ 2 Velorum and the Gum nebula. We show that the Vela SNR belongs to a subclass of non-Sedov adiabatic remnants in a cloudy interstellar medium (ISM), the dynamics of which is determined by the heating and evaporation of ISM clouds. We explain observable characteristics of the Vela SNR with a SN explosion with energy 1.4 × 10 50 erg near the step-like boundary of the ISM with low intercloud densities (∼10 −3 cm −3 ) and with a volume-averaged density of clouds evaporated by shock in the north-east (NE) part about four times higher than the one in the south-west (SW) part. The observed asymmetry between the NE and SW parts of the Vela SNR could be explained by the presence of a stellar wind bubble (SWB) blown by the nearest-to-the Earth Wolf-Rayet (WR) star in the γ 2 Velorum system. We show that the size and kinematics of γ 2 Velorum SWB agree with predictions of numerical calculations for the evolution of the SWB of M ini = 35 M star. The low initial mass of the WR star in γ 2 Velorum implies that the luminosity of the nuclear line of 26 Al, produced by γ 2 Velorum, is below the sensitivity of existing gamma-ray telescopes.

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Theory of cosmic ray and γ-ray production in the supernova remnant RX J0852.0-4622

Berezhko¹,

Puhlhoefer²,

Völk³

2009

A&A

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Aims. The properties of the Galactic supernova remnant (SNR) RX J0852.0-4622 are theoretically analysed.Methods. An explicitly time-dependent, nonlinear kinetic model of cosmic ray (CR) acceleration in SNRs is used to describe the properties of SNR RX J0852.0-4622, the accelerated CRs, and the nonthermal emission. The source is assumed to be at a distance of ≈1 kpc in the wind bubble of a massive progenitor star. An estimate of the thermal X-ray flux in this configuration is given. Results. We find that the overall synchrotron spectrum of RX J0852.0-4622 as well as the filamentary structures in hard X-rays lead to an amplified magnetic field B > 100 μG in the SNR interior. This implies that the leptonic very high energy (VHE) γ-ray emission is suppressed, and that the VHE γ-rays are hadronically dominated. The energy spectrum of protons produced over the lifetime of the remnant until now may well reach "knee" energies. The derived γ-ray morphology is consistent with the HESS measurements. The amount of energy in energetic particles corresponds to about 35% of the hydrodynamic explosion energy. A remaining uncertainty concerns the thermal X-ray flux at 1 keV. A rough estimate, which is possibly not quite appropriate for the assumed wind bubble configuration, is found to be higher than the nonthermal flux at this energy. Conclusions. It is concluded that this SNR expanding into the wind bubble of a massive star in a dense gas environment can be a hadronic γ-ray source that is consistent with all existing multiwavelength constraints, except possibly the thermal X-ray emission.

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Cited by 21 publications

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Vela Pulsar and Its Synchrotron Nebula

Vela Pulsar and Its Synchrotron Nebula

Modeling of the Vela complex including the Vela supernova remnant, the binary systemγ² Velorum, and the Gum nebula

Theory of cosmic ray and γ-ray production in the supernova remnant RX J0852.0-4622

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Untitled

Cited by 21 publications

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Vela Pulsar and Its Synchrotron Nebula

Vela Pulsar and Its Synchrotron Nebula

Modeling of the Vela complex including the Vela supernova remnant, the binary systemγ2 Velorum, and the Gum nebula

Theory of cosmic ray and γ-ray production in the supernova remnant RX J0852.0-4622

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Modeling of the Vela complex including the Vela supernova remnant, the binary systemγ² Velorum, and the Gum nebula