Motion of the Ultraviolet R Aquarii Jet

Hollis, J. M.; Lyon, Richard G.; Dorband, John E.; Feibelman, W. A.

doi:10.1086/303526

Cited by 20 publications

(30 citation statements)

References 19 publications

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“…2 and 3a), especially in 1992. This structure as well as the low intensity gas trailing right after C2 are similar to the structures observed with HST (Paresce & Hack 1994;Hollis et al 1997a). These features could be explained by a slowly moving shock front through which the gas in the jet flows.…”

Section: Magnetic Base In the Jet?supporting

confidence: 83%

“…According to the LJ1 model the components are on ballistic orbits, whereas in the LJ2 model the components should follow each other's tracks in a (twisted) magnetic field. The event separation time of the LJ2 model has been substantiated with HST observations (Hollis et al 1997a), but models in the UV-region yielded nonlinear B and D in 1991.63 and in 1999.78. acceleration. Characteristics of a helical structure were also seen.…”

Section: Introductionmentioning

confidence: 60%

“…The motion of C2 has also clearly slowed down since the observations of LJ. Actually, the component already had a lower speed in the UV-observations of Hollis et al (1997a), assuming that the positions of the components at these two frequencies can be compared.…”

Section: Magnetic Base In the Jet?mentioning

confidence: 99%

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Proper motion analysis of the jet of R Aquarii

Mäkinen

Lehto

Vainio

et al. 2004

A&A

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Abstract.We have observed the jet of R Aquarii at high resolution with the VLA in 1992. 83 and in 1999.78. Observations in the first epoch have resolved the base of the jet which shows a helical structure. We cannot detect the expected new jet component at either epoch. This does not disprove the idea of periodic ejection. Either the timing inferred from the acceleration models, or the assumed periastron passage is incorrect. Alternatively, a single new component cannot be resolved due to the dense core. Proper motion analysis of the jet components shows that previously derived acceleration models do not fit our new data. Indeed, the first ∼1 of the jet, both to north-east and south-west, appears fixed and has slowly moving shocks at the termination points, whereas the positions of the outer components fit best a ballistic orbit. We propose that the components are formed due to enhanced matter flow at periastron, accelerated during the first 1 and then ejected as bullets. Component A at a distance of ∼4 from the core has broken into two parts, similar to what was previously assumed to have happened to the outermost components B and D. The disruption is probably a consequence of a reverse shock or a collision with a cloud.

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Section: Magnetic Base In the Jet?supporting

confidence: 83%

Section: Introductionmentioning

confidence: 60%

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Proper motion analysis of the jet of R Aquarii

Mäkinen

Lehto

Vainio

et al. 2004

A&A

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“…The star has taken its revenge and now seems to be excreting, ejecting, or whatever the polite antonym is (Hollis et al 1997;Kuipers et al 1997). Perhaps it is alternating between accretion and excretion, like an X-ray binary subject to propeller episodes (Wynn et al 1997).…”

Section: Starry Starry Nightmentioning

confidence: 99%

Astrophysics in 1997

Trimble¹,

McFadden²

1998

PUBL ASTRON SOC PAC

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ABSTRACT. Martian marvels, a gamma-ray burster with a redshift, Galileo converses with Ganymede, a record galactic redshift of 4.92, and much else. Fiscal 1997 was definitely an exciting year for astronomers. We have tried hard to hit all the obvious highlights, but also to report more gradual progress on traditional problems of understanding planets, stars, galaxies, and the universe. Though the year was saddened by the loss of many valued colleagues, we nevertheless indulge in occasional soupçons of frivolity.

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“…Initially, the mass of the jet was calculated assuming a cylindrical system. This calculation did not take into account the true spatial extent [7], (c) All x-ray quantities are taken or derived from Kellogg et al [11,12], (d) Kafatos et al [10], (e) Meier & Kafatos [13], (f) Hollis et al [8] of the emission. In order to characterize the mass loss in the jet more quantitatively, the Chandra observation was re-analyzed on a pixel by pixel basis to give a tighter estimation of the jet volume hence a tighter mass estimate for the jet in the x-rays.…”

Section: Observationsmentioning

confidence: 99%

A study of the mass loss rates of symbiotic star systems

Korreck¹,

Kellogg²,

Sokoloski³

2007

AIP Conference Proceedings

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Abstract. The amount of mass loss in symbiotic systems is investigated, specifically mass loss via the formation of jets in R Aquarii (R Aqr). The jets in R Aqr have been observed in the Xray by Chandra over a four year time period. The jet changes on times scales of a year and new outflows have been observed. Understanding the amount of mass and the frequency of ejection further constrain the ability of the white dwarf in the system to accrete enough mass to become a Type 1a supernova progenitor. The details of multi-wavelength studies, such as speed, density and spatial extent of the jets will be discussed in order to understand the mass balance in the binary system. We examine other symbiotic systems to determine trends in mass loss in this class of objects.

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Motion of the Ultraviolet R Aquarii Jet

Cited by 20 publications

References 19 publications

Proper motion analysis of the jet of R Aquarii

Proper motion analysis of the jet of R Aquarii

Astrophysics in 1997

A study of the mass loss rates of symbiotic star systems

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