Retuneable organic dye solution laser, excited by a nitrogen laser

Bychkov, Yu. I.; Losev, V. F.; Revenko, V. I.; Тарасенко, В. Ф.; Тимофеев, В. Б.

doi:10.1007/bf00894545

Cited by 2 publications

(2 citation statements)

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“…Several authors have suggested the jet is a post-SN feature resulting from an interaction between the ejecta and the pulsar wind nebula. Many variations of plasma instability models have been suggested including: (i) an aneurysm of ejecta pushed aside by the pulsar's plasma flow (Bychkov 1975;Véron-Cetty et al 1985;Marcelin et al 1990), (ii) Rayleigh-Taylor instabilities (Chevalier & Gull 1975;Kundt 1983) or differential acceleration (Chevalier & Gull 1975), (iii) pressure from swept-up magnetic field lines (Shull et al 1984), (iv) ejecta entrainment in magnetic fields formed by highly ordered outflows from the polar caps of the pulsar itself (Benford 1984) and (v) synchrotron driven shocks (Sankrit & Hester 1997).…”

Section: Plasma Instabilities Modelsmentioning

confidence: 99%

The Crab Nebula's dynamical age as measured from its northern filamentary jet

Rudie

Fesen

Yamada

2008

Monthly Notices of the Royal Astronomical Society

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We present a deep [O iii]λλ4959,5007 image of the northern filamentary jet in the Crab Nebula taken with the 8.2‐m Subaru telescope. Using this image and an image taken with the Kitt Peak National Observatory (KPNO) 4‐m in 1988, we have computed proper motions for 35 locations in the jet. The results suggest that when compared to the main body of the remnant, the jet experienced less outward acceleration from the central pulsar's rapidly expanding synchrotron nebula. The jet's apparent expansion rate yields an undecelerated explosion date for the Crab Nebula of 1055 ± 24 CE, a date much closer to the appearance of the historic 1054 CE guest star than the 1120–1140 CE dates estimated in previous studies using filaments located within the remnant's main nebula. Our proper motion measurements suggest the jet likely formed during the 1054 supernova explosion and represents the remnant's highest velocity knots possibly associated with a suspected N–S bipolar outflow from the supernova explosion.

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Section: Plasma Instabilities Modelsmentioning

confidence: 99%

The Crab Nebula's dynamical age as measured from its northern filamentary jet

Rudie

Fesen

Yamada

2008

Monthly Notices of the Royal Astronomical Society

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“…One early theory involved a two-component pulsar wind nebula (PWN) model where dense, line radiation emitting filaments were frozen in a "strong" 10 −3 Gauss magnetic field. Field lines forced between the filaments via plasma instabilities then expand outward forming the jet (Bychkov 1975;Marcelin et al 1990). Other models suggest a combination of magnetic fields and the Crab's PWN leading to a Rayleigh-Taylor instability 'bubble' bursting through the nebula's shell of ejecta (Chevalier & Gull 1975;Sankrit & Hester 1997).…”

Section: Introductionmentioning

confidence: 99%

A 3D kinematic study of the northern ejecta ‘jet’ of the Crab nebula

Black

Fesen

2015

Monthly Notices of the Royal Astronomical Society

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We present moderate resolution [O III] λλ4959,5007 line emission spectra of the Crab Nebula's northern ejecta jet. These data along with an [O III] image of the Crab Nebula were used to build 3-dimensional kinematic maps of the jet and adjacent remnant nebulosity to better understand the jet's properties and thus its likely origin. We find the jet's systemic velocity to be +170 ± 15 km s −1 with radial velocities ranging from −190 to +480 km s −1 . Our data indicate that the jet consists of thin filamentary walls (V exp 40 -75 km s −1 ), is virtually hollow in [O III] emission, and elliptical and funnel-like in shape rather than a straight cylindrical tube as previously thought. Examination of the Crab's 3D filamentary structure along the jet's base reveals a large and nearly emission-free opening in the remnant's thick outer ejecta shell. The jet's blueshifted and redshifted sides are surprisingly well defined and, like the jet's sharp western limb, appear radially aligned with the remnant's center of expansion. These alignments, along with the opening in the nebula at the jet's base and proper motions indicating an expansion age in line with the 1054 supernova event, suggest a direct connection between the jet's formation and the Crab's radial expansion. While our analysis supports the scenario that the jet may simply represent the highest velocity material of the remnant's N-S bipolar expansion, the nature of this expansion asymmetry remains unclear.

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Retuneable organic dye solution laser, excited by a nitrogen laser

Cited by 2 publications

References 0 publications

The Crab Nebula's dynamical age as measured from its northern filamentary jet

The Crab Nebula's dynamical age as measured from its northern filamentary jet

A 3D kinematic study of the northern ejecta ‘jet’ of the Crab nebula

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