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- W2021004885 abstract "<i>Context. <i/>HH 444 is one of the first Herbig-Haro (HH) jets discovered within a photoionized region.<i>Aims. <i/>We re-analyze the H<i>α<i/> and red [S II] HST images of HH 444, and calculate the width of the jet as a function of distance from the source. We compare the H<i>α<i/> image with predictions from variable ejection velocity jet models.<i>Methods. <i/>The determination of the jet's width is done with a non-parametric, wavelet analysis technique. The axisymmetric, photoionized jet simulations are used to predict H<i>α<i/> maps that can be directly compared with the observations.<i>Results. <i/>Starting with a thin jet (unresolved at the resolution of the observations), we are able to produce knots with widths and morphologies that generally agree with the H<i>α<i/> knots of HH 444. This agreement is only obtained if the jet axis is at a relatively large, ~45° angle with respect to the sky. This agrees with previous spectroscopic observations of the HH 444 bow shock, which imply a relatively large jet axis/plane of the sky angle.<i>Conclusions. <i/>We conclude that the general morphology of the chain of knots close to V510 Ori (the HH 444 source) can be explained with a variable ejection velocity jet model. For explaining the present positions of the HH 444 knots, however, it is necessary to invoke a more complex ejection velocity history than a single-mode, periodic variability." @default.
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- W2021004885 date "2010-07-01" @default.
- W2021004885 modified "2023-09-27" @default.
- W2021004885 title "A variable jet model for the Hαemission of HH 444" @default.
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- W2021004885 doi "https://doi.org/10.1051/0004-6361/200913908" @default.
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